Schedule Abstracts Author Index Schedule Sunday Sunday, January 9, 2011, 12:30 PM - 3:40 PM HAD I Special: The Astronomical Contributions of the Herschel Family Sunday, January 9, 2011, 4:00 PM - 6:00 PM HAD II Special: Neptune after One Orbit: Reflections on the Discovery of a Planet Monday Monday, January 10, 2011, 8:30 AM - 9:20 AM Kavli Lecture: Cassini Eyes the Rings of Saturn Monday, January 10, 2011, 9:00 AM - 6:30 PM NANOGrav Posters Kepler Posters Gamma Ray Bursts AGN, QSO, Blazars Black Holes Binary Stellar Systems, X-ray Binaries Career Paths, Professional Development, and STEM Diversity HAD III History Poster Papers Dwarf Galaxies Elliptical Galaxies Galaxy Clusters Large Scale Structure, Cosmic Distance Scale Dark Matter & Dark Energy Star Associations, Star Clusters - Galactic & Extra-galactic Stellar Evolution, Stellar Populations Stellar Atmospheres, Winds The Sun The Solar System Instrumentation: Ground Based or Airborne Education, Public Outreach, Citizen Science and Science Impact Monday, January 10, 2011, 10:00 AM - 11:30 AM Results from the First Year of Observations with the Cosmic Origins Spectrograph Kepler I HEAD: High Energy Processes in Star Formation Binary Stellar Systems, X-ray Binaries AGN, QSO, Blazars I Hydrogen Epoch of Reionization Arrays (HERA): Progress and Planning Gamma Ray Bursts Galaxy Clusters: Intracluster Medium and Cluster Masses Strategies for Addressing Harassment and Prejudice HAD IV History of Astronomy Interstellar Medium: Dust Particles and Emission YSOs, Etc. I Starburst Galaxies Evolution of Galaxies I Computation: Learning, Simulating, Data Reduction Monday, January 10, 2011, 11:40 AM - 12:30 PM Chandra's First Decade (Plus) of Discovery Monday, January 10, 2011, 2:00 PM - 3:30 PM Super-Earths and Terrestrial Planets: Latest Results from the Kepler Mission Community Science with LSST Science Highlights from NASA's Astrophysics Data Analysis Program I The Low-Frequency Gravitational Wave Universe: Detection Prospects, Sources, and Astrophysics AGN, QSO, Blazars II White Dwarfs in Binaries and Interacting Systems Galaxy Clusters: Intracluster Medium and Cosmology Evolution of Galaxies II HAD V History of Astronomy Planetary Nebulae and Supernova Remnants YSO's Etc. II Interstellar Medium: HII Regions Star formation in Extragalactic Systems Monday, January 10, 2011, 3:40 PM - 4:30 PM Pierce Prize: Dark Matter and Black Holes Over Cosmic Time Monday, January 10, 2011, 4:30 PM - 5:20 PM Exoplanets: Misaligned, Migratory, Metallic, and Mini Tuesday Tuesday, January 11, 2011, 8:30 AM - 9:20 AM The Virgo Cluster: New Results from New Surveys Tuesday, January 11, 2011, 9:00 AM - 6:30 PM Dark Energy Survey Radio Sky Surveys Project with the Allen Telescope Array The Milky Way, The Galactic Center Stars, Cool Dwarfs, Brown Dwarfs Cosmic Microwave Background Starburst Galaxies Spiral Galaxies The Center for Astronomy Education (CAE) Collaboration of Astronomy Teaching Scholars (CATS) Program: A Year-Three Update Astronomy Education and Research in Grades K-12 Cosmology Interstellar Medium, Dust Interstellar Medium, Molecular Clouds, HII Regions LSST Posters Exoplanet Detection: Techniques & Observations Instrumentation: Space Missions Exploring the Far-IR/Sub-mm with the Herschel Space Observatory Planetary Nebulae and Supernova Remnants Emerging Results on an Extreme Binary, Epsilon Aur Star Formation Planck Poster Session Tuesday, January 11, 2011, 10:00 AM - 11:30 AM Kepler II Exploring the Far-IR/Sub-mm with the Herschel Space Observatory Radio Sky Surveys Project with the Allen Telescope Array Large Scale Structure, Cosmic Distance Scale The Dark Energy Survey Science Highlights from NASA's Astrophysics Data Analysis Program II M31, M32 & S4G Spirals Practical Tools & Techniques for Educators HAD VI History of Astronomy Evolution of Galaxies III AGN, QSO, Blazars III Galaxy Clusters: Surveys and AGN Cosmology I Pulsars, Neutron Stars I Interstellar Medium: Molecular Gas Interstellar Medium, Cosmic Rays and Magnetic Fields Tuesday, January 11, 2011, 11:40 AM - 12:30 PM Early Astrophysics Results from Planck Tuesday, January 11, 2011, 2:00 PM - 3:30 PM Exoplanet Detection: Transits Habitability of a Terrestrial Planet Surveys and Large Programs HEAD: New Radio Insights in High Energy Phenomena Emerging Results on the Extreme Binary, epsilon Aurigae Gravitational Lenses and Gravitational Waves Multiple Cool and Brown Dwarfs Galaxy Clusters: Lensing and S-Z Effect The Center for Astronomy Education (CAE) Collaboration of Astronomy Teaching Scholars (CATS) Program: A Year-Three Research Update Evolution of Galaxies IV AGN, QSO, Blazars IV Cosmology II Stellar Winds, Jets, and Ejecta Evolution of Galaxies V Pulsars, Neutron Stars II Tuesday, January 11, 2011, 3:40 PM - 4:30 PM Warner Prize: Millisecond Pulsars: The Gifts that Keep on Giving Tuesday, January 11, 2011, 4:30 PM - 5:20 PM A New View of the High Energy Gamma-Ray Sky with the Fermi Gamma-Ray Space Telescope Wednesday Wednesday, January 12, 2011, 8:30 AM - 9:20 AM The First Supermassive Black Holes Wednesday, January 12, 2011, 9:00 AM - 6:30 PM Observing with ALMA Early Science with EVLA Early Results from WISE Surveys and Large Programs Evolution of Galaxies Pulsars, Neutron Stars Supernovae Evolved Stars, Cataclysmic Variables, Novae, Wolf-Rayet Phenomena Circumstellar Disks YSOs, Very Young Stars and Friends White Dwarfs Variable Stars Extrasolar Planets: Characterization and Theory Computation, Data Handling, Image Analysis Intergalactic Medium, QSO Absorption Line Systems Undergraduate Astronomy Education and Research Gravitational Lenses and Gravitational Waves Catalogs Astrobiology & Laboratory Astrophysics Wednesday, January 12, 2011, 10:00 AM - 11:30 AM Early Results from the Wide-field Infrared Survey Explorer Exoplanet Detection: Imaging, Interferometry Supermassive Black Holes Early Science with the Expanded Very Large Array Ultraviolet Astronomy in the New Detector Era The Solar System Stars, Cool Dwarfs, Brown Dwarfs Supernovae I - Type Ia Evolution of Galaxies VI AGN, QSO, Blazars V Stellar Evolution, Stellar Populations and Variable Stars Nearby Galaxy Clusters, Groups, and Ellipticals Cosmic Microwave Background Wednesday, January 12, 2011, 11:40 AM - 12:30 PM Heinemann Prize: The Inner Space/Outer Space Connections: Dark Matter, Dark Energy, Inflation and All That Wednesday, January 12, 2011, 2:00 PM - 3:30 PM Observing with ALMA Exoplanet Detection: Many Techniques The Sun, the Earth & Astrobiology Joint Astrophysics and Planetary Science Studies From the Outer Solar System Cluster Cosmology with Optical and SZ data Circumstellar Disks I and Sedna The Milky Way, The Galactic Center Supernovae II - Type Ia Evolution of Galaxies VII AGN, QSO, Blazars VI Star Associations, Star Clusters - Galactic & Extra-galactic I Stellar Populations and Kinematics of Dwarf and Irregular Galaxies Wednesday, January 12, 2011, 3:40 PM - 4:30 PM Cannon Prize: Stellar Archaeology: New Science with Old Stars Wednesday, January 12, 2011, 4:30 PM - 5:20 PM Rossi Prize: Exploring the Very High Energy Sky with H.E.S.S. Thursday Thursday, January 13, 2011, 8:30 AM - 9:20 AM Exoplanets: New Approaches to their Discovery and Characterization Thursday, January 13, 2011, 9:00 AM - 2:00 PM Extrasolar Planets Galaxies, Galaxy Clusters and Friends Education and Outreach High Energy, Cosmology and Other Topics Instrumentation, Surveys and Data Stars, Star Formation and Associated Topics The Solar System II The Sun II Thursday, January 13, 2011, 10:00 AM - 11:30 AM Exoplanet Detection: Radial Velocities Exoplanet Atmospheres - Modeling and Observations Dark Matter & Dark Energy Black Holes Astronomy Education Research Circumstellar Disks II Evolution of Galaxies VIII AGN, QSO, Blazars VII Star Associations, Star Clusters II Supernovae III The Role of Environment in Galactic Star Formation Intergalactic Medium, QSO Absorption Line Systems Instrumentation: Ground Based Thursday, January 13, 2011, 11:40 AM - 12:30 PM Addressing Unconscious Bias: Steps toward an Inclusive Scientific Culture Thursday, January 13, 2011, 2:00 PM - 3:30 PM Exoplanet Systems - Characterization and Dynamics The Formation of Very Massive Stars Spiral Galaxies Exoplanet Atmospheres - Observations and Modeling II Circumstellar Disks III Education and Outreach Beyond IYA Evolution of Galaxies IX Elliptical Galaxies: S4G, LIERs, Black Holes Supernovae IV Origin and Evolution of the Milky Way Satellites Instrumentation: Space Missions The Intergalactic Medium as seen by FIREBALL & CW1 Star Associations, Star Clusters III Thursday, January 13, 2011, 3:40 PM - 4:30 PM Berkeley Prize: Kepler: Opening New Doors in Astronomy Abstracts Sunday, January 9, 2011, 12:30 PM - 3:40 PM HAD I Special: The Astronomical Contributions of the Herschel Family Special Session Room 613/614 The Herschels: A very fashionable scientific family Emily Winterburn1 1University College London, United Kingdom. 12:30 PM - 1:15 PM Room 613/614 What is special about the Herschel family? It is a family that has attracted the attention of historians of science for many years and has done so for a number of reasons. Some simply marvel at the family’s ability to have produced generations upon generation of great men and women of science. Others have highlighted the work of individuals within the family and how their work changed the way astronomy was done, what it was about, and then later did the same for science as a whole. The unusually high status enjoyed by Herschel women, Caroline Herschel in particular, has not escaped notice, though I will here question some of the conclusions drawn about her motivations. Most of all, however I will argue in this paper, they should be interesting to a modern audience for the way in which they managed time and again, generation on generation, to make science fashionable and popular. In this paper I will look at three generations of this family - from William and Caroline discovering comets and planets in the late eighteenth century, through John and his claim that society needs science to be properly civilised, to John and Margaret’s children and their varied takes on the relationship between astronomy, science and the public. I will look at the role astronomy played in each of their lives, how they were taught and taught each other and how in each generation they managed to make their work the talk of the town. The Herschels and the Nebulae Robert W. Smith1 1University of Alberta. 1:15 PM - 1:40 PM Room 613/614 An innovative observer, theorist and telescope builder, William Herschel is now generally recognised as one of the greatest astronomers of all time. In this paper I will argue that to set Herschel’s career correctly into context it is essential to see him in addition as a natural philosopher (as the term `natural philosopher’ was understood around 1800). In examining Herschel as a natural philosopher, I will focus on his shifting views on the nature of the nebulae, views I will also contrast and compare with those of his son John Herschel. Herschel's 20ft Telescope at the Smithsonian David H. DeVorkin1 1Smithsonian Inst.. 1:40 PM - 1:55 PM Room 613/614 The tube and one of the mirrors from the original Herschel 20-foot telescope have been on display at the National Air and Space Museum since September 12, 2001. Approximately 3,000 visitors walk past it each day, inspecting how William and Caroline jointly operated the telescope in their garden. This presentation will recount how the telescope was brought to NASM, and prepared for exhibition. We will also discuss a bit of what we've learned about the telescope's history from developing this display. William Herschel's Explorations of the Conditions for Extraterrestrial Life Marvin Bolt1 1Adler Planetarium. 2:10 PM - 2:35 PM Room 613/614 William Herschel’s notion of life on the sun has been described as one of his stranger ideas. A more careful look, though, supports his declaration to have founded his view “upon astronomical principles” (broadly construed) as opposed to resembling the musings of “fanciful poets.” In particular, we’ll explore how contemporary concepts of geology and heat informed William’s defense of solarians, and see how a few of John Herschel’s methodological comments provide insight into William’s reasoning. Planetary Observations by William Herschel Woodruff T. Sullivan, III1 1Univ. of Washington. 2:35 PM - 3:00 PM Room 613/614 William Herschel was a constant observer of the planets and ~40% of his publications are concerned with every known object in the solar system; yet historians have paid little attention to this aspect of his career. In this paper I will summarize his major solar system findings (including the moon and sun) and, for a few key cases, discuss his observational techniques and interpretations. I will also argue for significant connections between Herschel’s planetary and solar work and his more familiar work on the sidereal universe. Who Invented the Word Asteroid: William Herschel or Stephen Weston? Clifford J. Cunningham1 1James Cook University. 3:00 PM - 3:15 PM Room 613/614 William Herschel made the first serious study of 1 Ceres and 2 Pallas in the year 1802. He was moved by their dissimilarities to the other planets to coin a new term to distinguish them. For this purpose he enlisted the aid of his good friends William Watson and Sir Joseph Banks. Watson gave him a long list of possible names, most of which sound quite ludicrous. With a lifetime of experience classifying and naming newly found objects in nature, Banks became the man both Erasmus Darwin (in 1781) and William Herschel (in 1802) turned to for sage advice in developing a new descriptive language. In the case of Ceres and Pallas, Banks turned the task over to his friend, the noted philologist Stephen Weston FRS. It has recently been stated by a noted British historian that it was Weston- not Herschel- who coined the term “asteroid” to collectively describe Ceres and Pallas. This claim is investigated, and parallels are drawn in the use of neologism in astronomy and botany. John Herschel's Graphical Method Thomas L. Hankins1 1University of Washington. 3:15 PM - 3:40 PM Room 613/614 John Herschel’s Graphical Method In 1833 John Herschel published an account of his graphical method for determining the orbits of double stars. He had hoped to be the first to determine such orbits, but Felix Savary in France and Johann Franz Encke in Germany beat him to the punch using analytical methods. Herschel was convinced, however, that his graphical method was much superior to analytical methods, because it used the judgment of the hand and eye to correct the inevitable errors of observation. Line graphs of the kind used by Herschel became common only in the 1830s, so Herschel was introducing a new method. He also found computation fatiguing and devised a “wheeled machine” to help him out. Encke was skeptical of Herschel’s methods. He said that he lived for calculation and that the English would be better astronomers if they calculated more. It is difficult to believe that the entire Scientific Revolution of the 17th century took place without graphs and that only a few examples appeared in the 18th century. Herschel promoted the use of graphs, not only in astronomy, but also in the study of meteorology and terrestrial magnetism. Because he was the most prominent scientist in England, Herschel’s advocacy greatly advanced graphical methods. Sunday, January 9, 2011, 4:00 PM - 6:00 PM HAD II Special: Neptune after One Orbit: Reflections on the Discovery of a Planet Special Session Room 613/614 The Discovery of Neptune: Why It Mattered in 1846 and Why It Still Matters Robert W. Smith1 1University of Alberta. 4:00 PM - 4:20 PM Room 613/614 The discovery of Neptune is one of the most well-known events in the history of nineteenth century astronomy as well as one of the most analyzed. Given the ferocious battle for priority that the optical discovery provoked, it is not surprising that much of the literature on the discovery has focused narrowly on issues around the appropriate amount of credit to be handed out to the main protagonists for the theoretical and optical discoveries of the planet. In this paper I will instead seek to put the discovery of Neptune and the events surrounding it into the broad context of mid-nineteenth century science to explain why it was seen to matter so much at the time and why it still matters today. The Life and Times of John Couch Adams, from 1819 to 1847 Brian M. Sheen1 1Roseland Observatory, United Kingdom. 4:20 PM - 4:40 PM Room 613/614 John Couch Adams was born in 1819 in the middle of Cornwall, the most remote and isolated county in England. How he progressed from there to Cambridge University to become one of the finest mathematicians of the nineteenth century fills everyone who studies him with awe. Tragically what should have been his greatest triumph - the discovery of a new planet - was marred by mishap, controversy and unanswered questions. This presentation examines one of the first of these questions and provides new answers based on recently revealed evidence. The Astronomer Royal of the day was attempting to support Adams and as part of that support asked if his analysis took into account changes in radius vector of Uranus. Adams did not reply and the rest as they say is history. However there is far more to the question than a non-existent letter - this in itself turns out to be not exactly true. Further analysis of the orbits and a letter in French - not been translated before reveals Adams had a more profound understanding of the situation than some later authors have given him credit. Neptune's Discovery: Le Verrier, Adams, and the Assignment of Credit William Sheehan1 1Child and Adolescent Behavioral Health Services. 4:40 PM - 5:00 PM Room 613/614 As one of the most significant achievements of 19th century astronomy, the discovery of Neptune has been the subject of a vast literature. A large part of this literature--beginning with the period immediately after the optical discovery in Berlin--has been the obsession with assigning credit to the two men who attempted to calculate the planet's position (and initially this played out against the international rivalry between France and England). Le Verrier and Adams occupied much different positions in the Scientific Establishments of their respective countries; had markedly different personalities; and approached the investigation using different methods. A psychiatrist and historian of astronomy tries to provide some new contexts to the familiar story of the discovery of Neptune, and argues that the personalities of these two men played crucial roles in their approaches to the problem they set themselves and the way others reacted to their stimuli. Adams had features of high-functioning autism, while Le Verrier's domineering, obsessive, orderly personality--though it allowed him to be immensely productive--eventually led to serious difficulties with his peers (and an outright revolt). Though it took extraordinary smarts to calculate the position of Neptune, the discovery required social skills that these men lacked--and thus the process to discovery was more bumbling and adventitious than it might have been. The discovery of Neptune occurred at a moment when astronomy was changing from that of heroic individuals to team collaborations involving multiple experts, and remains an object lesson in the sociological aspects of scientific endeavor. "These Frenchmen fly at one like wild cats": The French Press Attacks on British Claims for a Role in the Discovery of Neptune Craig B. Waff1 1Air Force Research Laboratory. 5:00 PM - 5:20 PM Room 613/614 In a letter to the editor of the Athenaeum (a weekly British intellectual periodical) that appeared in its 3 October 1846 issue, John Herschel revealed that a young Cambridge fellow, John Couch Adams, had performed calculations, as yet not published or otherwise publicly announced, that were similar to those made by Urbain Jean Joseph Le Verrier in predicting a position for a hypothetical planet disturbing the motion of Uranus. As is well known, a plea from Le Verrier led Johann Gottfried Galle to search for and optically discover, on 23 September 1846, a transuranian object near Le Verrier’s predicted position. Shortly after the appearance of Herschel’s letter, he and Adams, as well as Cambridge Observatory director James Challis and Astronomer Royal George Airy, became the targets of an intense month-long public attack by various Parisian newspapers and magazines, which perceived a British attempt to “steal” the discovery of the new planet, soon to be named Neptune. It was this attack that led to the despairing comment in Herschel’s diary that appears in the title of my talk. Although this attack has been frequently mentioned by commentators on the controversies surrounding the discovery of Neptune, the actual French publications have virtually never been examined in detail. An analysis of some of these articles, as well as British responses to them, is presented here. The Neptune Affair: American Mathematicians Find the World Stage Deborah Kent1 1Hillsdale College. 5:20 PM - 5:40 PM Room 613/614 The sensational news of Neptune’s observation reached the United States about a month after the initial sighting at the Berlin observatory on 23 September 1846. The ensuing dispute over the priority of discovery captured both popular interest and scientific attention in America. A handful of ambitious scientists viewed the Neptune affair as an opportunity to establish the legitimacy of American science, especially in response to the perceived superiority of European science. This talk will focus on the role of Harvard mathematician Benjamin Peirce in questioning the mathematical particulars of the discovery and shaping related rhetoric to advance the professionalization of American science. A Clear Yet Distant Echo: Modern-day Analogues of the Scientific Interest and Controversies Surrounding the Discovery of Neptune Greg Laughlin1, M. Brown2 1UC Santa Cruz, 2Caltech. 5:40 PM - 6:00 PM Room 613/614 Our understanding of the solar system and the physical Universe has progressed almost immeasurably during the 164.79 years that constitute an orbit of Neptune. Nevertheless, the drama surrounding the discovery of Neptune still resonates with an immediacy that is both completely relevant and entirely up to date. In this talk, we will argue that the central themes surrounding Neptune's discovery (including issues of priority, improvements in observational and theoretical technique, and the nature of what constitutes an acceptably specific scientific prediction) all have readily evident analogues in the planet-hunting and solar system discovery efforts that are being carried out today. To support our arguments, we will make specific connections to (1) the ongoing effort to map and characterize the solar system's trans-Neptunian inventory, and (2) the search for extrasolar planets orbiting nearby stars. Monday, January 10, 2011, 8:30 AM - 9:20 AM 101 Kavli Lecture: Cassini Eyes the Rings of Saturn Invited Session Ballroom 6AB 101.01 Cassini Eyes the Rings of Saturn Carolyn C. Porco1 1CICLOPS, Space Science Institute. Ballroom 6AB For the past 6.5 years, NASA's Cassini spacecraft has been in orbit around the planet Saturn. In that time, Saturn has journeyed from the height of southern summer through early northern spring, allowing ample opportunity to observe changes in the planet's rings under a variety of lighting and viewing conditions. This presentation will highlight some of Cassini's most significant discoveries in this disk of icy rubble, emphasizing the connection between Saturn's rings and other astrophysical disk systems, such as protoplanetary disks and the giant spiral galaxies. Monday, January 10, 2011, 9:00 AM - 6:30 PM 139 NANOGrav Posters Poster Session Exhibit Hall 139.01 Using Cyclic Spectroscopy of Pulsars to Correct for Interstellar Propagation Delay Dan Stinebring1, A. Spatzier1, J. Nelson1, S. Giri1, C. Haddad1, K. Kundert1, M. Larkin1, J. N. Nelson1 1Oberlin College. Exhibit Hall Recently, Demorest et al. (2010) have demonstrated that, for pulsar observations, the phase of the e-m wave can be determined through a technique called cyclic spectroscopy. This is a major advance in high precision pulsar timing. We report on studies of how cyclic spectroscopy can be used to correct for interstellar propagation delays down to the 100 ns level. Substantial observing time on large telescopes will be necessary to put this important technique into practice. 139.02 Pulsar Phase Jitter and Cyclic Spectroscopy Derived Arrival Times Nipuni Palliyaguru1, M. McLaughlin1, D. Stinebring2 1West Virginia University, 2Oberlin College. Exhibit Hall In searching for gravitational waves with high-precision pulsar timing, we have analyzed the possibility of applying the method of cyclic spectroscopy (CS) to correct for the arrival time fluctuations of the signals. The main causes of these delays are interstellar medium effects such as electron density variations and multi-path scattering, timing noise, pulse shape changes, and pulse-to-pulse jitter. These phenomena affect the electromagnetic wave of the pulsar in both amplitude and phase. The CS method, developed recently by Demorest and collaborators (2010), takes into account the observed voltage signal of the pulsar in the frequency domain and computes a stable, integrable quantity. This quantity can, in principle, be used to determine the impulse response of the system, q(t). Determining q(t) at several observing frequencies should allow frequency dependent effects to be separated from achromatic effects. We have used simulated data assuming the observed signal to be a convolution of the intrinsic pulsar signal and q(t), with additive noise and phase jitter included. We can reconstruct the impulse response function from the simulated data and find an estimate of q(t). When done at several frequencies this allows an estimate for the true delay of the signal. We present the results of these simulations, focusing attention on the effects of pulse phase jitter. 139.03 Progress Towards a Pipeline for Continuous Gravitational Wave Searches in Pulsar Timing Data Justin Ellis1, F. Jenet2, M. McLaughlin1 1West Virginia University, 2University of Texas Brownsville. Exhibit Hall Gravitational Waves (GWs) are tiny ripples in the fabric of space-time predicted by Einstein’s General Relativity. Pulsar timing arrays (PTAs) are well poised to detect low frequency (10-9 - 10-7 Hz) GWs in the near future. There has been a significant amount of research into the detection of a stochastic background of GWs from supermassive black hole binaries (SMBHBs). Recent work (Sesana et al 2010) has shown that single continuous sources standing out above the background may be detectable by PTAs operating at a sensitivity sufficient to detect the stochastic background. The main source of continuous GWs in the pulsar timing frequency band are extremely massive and/or nearby SMBHs. Here we present progress towards a fully functional pipeline for continuous GW searches in pulsar timing data. This pipeline is based on a frequentist approach that relies on a matched filtering search of constructed template banks. We present methods for determining the optimal grid size in template space that maximizes the likelihood of detection and characterization of a given GW source. We also report progress on implementation of this pipeline into the TEMPO2 pulsar timing software package, in which the gravitational wave signal will be fit for in the pulsar timing residuals using a least squares fitting routine. This pipeline is versatile in that it can also be used for binary system parameter estimation and upper limit calculations on possible sources. 139.04 Optimizing a Pulsar Timing Array Ryan Shannon1, J. Cordes1 1Cornell Univ.. Exhibit Hall Nanohertz gravitational radiation can be detected through the long term analysis of pulse arrival times from a set of millisecond pulsars (a pulsar timing array). The sources of this emission include inspiraling massive black hole binaries and cosmic strings. Here, we assess the sensitivity of pulsar timing arrays to gravitational waves in the presence of a diverse range of noise sources both intrinsic and extrinsic to the pulsar. Noise sources intrinsic to the pulsar include terms associated with pulsar rotational irregularities (timing noise) and jitter of the radio emission region. Extrinsic noise includes terms associated with reflex motion of the pulsar about unmodeled circumpulsar asteroid belts and propagation of the pulsar radio emission through turbulent plasma in the interstellar medium. We describe the amenability of these noise sources to various mitigation techniques, such as observing with higher sensitivity telescopes and multi-frequency time of arrival fitting. We find that observations of more pulsars, observed with higher throughput (longer integrations times or faster observing cadences) are required to make a significant detection of gravitational radiation at cosmological levels and perform subsequent characterization of gravitational wave emitting sources. From this we conclude that pulsar timing is optimally conducted by using telescopes with a range of collecting areas, which can be achieved through coordinated global efforts utilizing current telescopes or a large array-based telescope. 139.05 Precision Millisecond Pulsar Timing: Space Velocities and Equivalence Principles Ingrid H. Stairs1, M. E. Gonzalez1, R. D. Ferdman2, P. C. C. Freire3, D. J. Nice4, P. B. Demorest5, S. M. Ransom5, R. N. Manchester6, G. B. Hobbs6, A. G. Lyne2, M. Kramer3, F. Camilo7 1Univ. of BC, Canada, 2University of Manchester, United Kingdom, 3MPIfR, Germany, 4Lafayette College, 5NRAO, 6CASS, Australia, 7Columbia University. Exhibit Hall We present high-precision timing results for 5 millisecond pulsars (MSPs), using data acquired with the Parkes and Arecibo telescopes. We measure the proper motion for each pulsar, infer 2-D space velocities, and update velocity distribution investigations of the MSP population, finding that binary and isolated MSPs have indistinguishable velocity distributions. We constrain binary inclination angles and hence masses for 2 of the pulsars in our sample. We use all the known wide-orbit pulsar--white-dwarf binaries to update previous limits on violation of the Strong Equivalence Principle and on a parameter describing violation of Lorentz invariance and momentum conservation. 139.06 High Precision Timing of Millisecond Pulsars at Arecibo and Green Bank David J. Nice1, P. B. Demorest2, M. E. Gonzalez3, R. D. Ferdman4, S. M. Ransom2, I. H. Stairs3, NANOGrav 1Lafayette College, 2NRAO, 3UBC, Canada, 4University of Manchester, United Kingdom. Exhibit Hall The NANOGrav consortium uses Arecibo and the GBT to make high-precision timing observations of twenty millisecond pulsars. All sources are observed at two frequencies using software coherent dedispersion systems. This program is motivated both by the search for a gravitational wave background and more traditional pulsar timing applications such as measuring binary orbits to test theories of gravitation and to measure neutron star masses. We will discuss the observing program and data analysis, and we will give highlights from the last five years of observations. 139.07 Characterizing the Radio Frequency Timing Stability of Fast and Millisecond Pulsars Isabel Mette Kloumann1, J. M. Rankin1 1University of Vermont. Exhibit Hall We propose measuring the average profile stabilization rate in millisecond pulsars. We consider the correlations between a pulsar's global average profile and subaverage profiles constructed using increasing numbers of pulses, thereby quantifying the number of pulses required to build a stable average profile. We adopt the methodology developed by Helfand, Manchester, and Taylor (Ap. J., 1975) and later employed by Rathnasree & Rankin (Ap. J., 1995) to calculate the stabilization rates of a sample of both fast and millisecond pulsars. A correlation coefficient is obtained by averaging the correlation coefficients of the global average profile with each subaverage profile of n pulses. By plotting how the correlation coefficient increases with n one can observe how the star's profile stabilizes as the number of pulses used to construct it increases. We look for values of n for which the correlation coefficient is statistically significant and interpret this value as the number of pulses required to compute a stable average profile of a given star. We expect n to be smaller for millisecond pulsars, as they typically exhibit very few intrinsic variations. This work considers the stars studied by Rathnasree & Rankin, as well as millisecond pulsars that are of interest to the pulsar timing community and in particular the NANOGrav (North American Nanohertz Observatory for Gravitational Waves) initiative. The authors would like to acknowledge support from the US National Science Foundation. 139.08 ARCC@UWM: The Arecibo Remote Command Center at the University of Wisconsin--Milwaukee Xavier Siemens1, C. Biwer1, J. Clayton1, J. Creighton1, D. Day1, D. Erb1, K. Gustavson2, F. Jenet3, D. Kaplan1, R. Karr1, M. Rohr1, K. Stovall3 1University of Wisconsin -- Milwaukee, 2Nicolet High School, 3University of Texas Brownsville. Exhibit Hall A low frequency stochastic background of gravitational waves could be detected by pulsar timing experiments in the next five to ten years. Increasing the number of time of arrival data sets available for gravitational wave searches will improve the sensitivity of a pulsar based gravitational wave detector. To achieve this goal, a group of faculty, staff, postdoctoral researchers, and a graduate student at the University of Wisconsin--Milwaukee are participating in a broad effort to increase the number of known stable pulsars collecting and analyzing the pulsar Arecibo L-band Feed Array (P-ALFA) survey data, and the Green Bank Northern Celestial Cap survey data. We have followed the pioneering model started at the University of Texas-Brownsville (UTB) to involve undergraduate and high school students in this research. In close collaboration with the group at UTB we have engaged two local high school teachers, several high school students, and about 15 UWM undergraduates in remotely commanding and observing using the Arecibo radio telescope and the Green Bank telescope, in searches in the collected data for new candidate pulsars, and follow-up observations of of potential pulsar candidates. In addition, the group is using its expertise in LIGO data analysis to improve gravitational wave searches in pulsar timing data. 140 Kepler Posters Poster Session Exhibit Hall 140.01 Kepler Target Pixel Files Susan E. Thompson1, S. McCauliff2, S. Bryson2, M. Still2, J. van Cleve2, J. Dotson2, J. Twicken2, T. Klaus2, M. Cote2, M. Fanelli2 1SETI Institute/NASA Ames, 2NASA Ames Research Center. Exhibit Hall In early 2011, the Kepler Mission will make available the pixel data for all observed targets, in addition to the aperture photometry light curves currently provided at the Multi-mission Archive at STScI (MAST). These target pixel files will contain images of the calibrated flux, the subtracted background, and the removed cosmic rays for the target at each cadence. Certain targets, such as highly variable stars, non-stellar targets, or saturated targets, require an analysis beyond fixed, optimal aperture photometry in order to retrieve all the information from the data. For a few cases we demonstrate the utility of the target pixel files in understanding the quality of the data and in performing specialized aperture photometry. Kepler was selected as the 10th mission of the Discovery Program. Funding for this mission is provided by NASA, Science Mission Directorate. 140.02 The Kepler Guest Observer Program Martin D. Still1, M. Fanelli1, K. Kinemuchi1, Kepler Science Team 1NASA Ames Research Center. Exhibit Hall Kepler is a NASA Discovery mission to identify and characterize Earth-size planets within the habitable zone around nearby stars. The Kepler instrument also provides an unprecedented opportunity to test and refine a diverse range of astrophysical paradigms with high-precision, uniform and rapid cadence data, containing none of the diurnal or seasonal gaps that limit ground-based observations. Kepler provides open opportunities to exploit existing data and propose for new targets and science. This poster provides directions to resources and data at the Kepler data archive at MAST and the Kepler Guest Observer Office. 140.03 Finding Planets from Variable Star Pulsation Arrival Times with Kepler Fergal Mullally1, K. Kinemuchi1, S. E. Thompson1, J. F. Rowe1 1Kepler Science Office. Exhibit Hall We examine the potential for planet detection using lightcurve arrival times around a variety of stars in the Kepler field. Arrival time analysis has been used to find planets around pulsars and sub-dwarf stars. When a variable star is orbiting the center of mass of a planetary system, its distance from the earth changes periodically. This change in distance is observed as a change in the observed arrival time of otherwise stable pulsations here on Earth. The sensitivity of the technique is set by the jitter of the pulsation period and phase, and the periods of detectable planets by the long term stability of the pulsation modes. We examine the limits that can be placed of a variety of variable stars using public data from the first quarter of observations by the Kepler space telescope. Kepler was selected as the 10th mission of the Discovery Program. Funding for this mission is provided by NASA, Science Mission Directorate 140.04 An Update to the Kepler Eclipsing Binary Catalog: the use of Pixel Time Series to Identify Blended Eclipsing Binary Systems Michael Rucker1, N. M. Batalha1, A. Prsa2, S. T. Bryson3, L. R. Doyle4, R. W. Slawson4, W. F. Welsh5, J. A. Orosz5 1Department of Physics and Astronomy, San Jose State University, 2Department of Astronomy and Astrophysics, Villanova University, 3NASA Ames Research Center, 4SETI Institute, 5Astronomy Department, San Diego State University. Exhibit Hall The Kepler telescope is providing a nearly seamless stream of photometric data of approximately 150,000 stars with unprecedented precision. The Kepler Eclipsing Binary (EB) catalog (based on the first 43 days of data; arXiv:1006.2815) is being continuously augmented as more data are collected and EBs are detected at longer periods. The catalog is expected to contain a small fraction of blends - cases where the eclipse signature is from a nearby source in the photometric aperture. In constructing the original catalog, obvious blends were identified and removed and/or reassigned to the appropriate point source. We build upon this work by performing pixel-level tests similar to those used to identify false positives amongst the Kepler exoplanet candidates. We summarize these tests here and provide examples that illustrate the types of blend scenarios that we have identified. Where appropriate and possible, we modified Kepler’s target list with the newly found Kepler star identification numbers. The changes reported here will affect the target lists which will go into effect on December 23, 2010 (start of Quarter 8). An updated version of the Kepler Eclipsing Binary catalog is available online at NASA’s Multimission Archive at STSci (MAST) website (http://archive.stsci.edu/kepler). 140.05 Pixel-Level Analysis Techniques for False-Positive Identification in Kepler Data Steve Bryson1, J. Jenkins2, R. Gilliland3, N. Batalha4, T. N. Gautier5, J. Rowe1, E. Dunham6, D. Latham7, D. Caldwell2, J. Twicken2, P. Tenenbaum2, B. Clarke2, J. Li2, H. Wu2, E. Quintana2, D. Ciardi5, G. Torres7, J. Dotson1, M. Still1 1NASA Ames Research Center, 2SETI/NASA Ames Research Center, 3Space Telescope Science Institute, 4SJSU/NASA Ames Research Center, 5Jet Propulsion Laboratory, 6Lowell Observatory, 7Harvard-Smithsonian Center for Astrophysics. Exhibit Hall The Kepler mission seeks to identify Earth-size exoplanets by detecting transits of their parent star. The resulting transit signature will be small (~100 ppm). Several astrophysical phenomena can mimic an Earth-size transit signature, most notably background eclipsing binaries (BGEBs). As part of a larger false-positive identification effort, pixel-level analysis of the Kepler data has proven crucial in identifying the likelihood of these confounding signals. Pixel-level analysis is primarily useful for the case of the transit being a BGEB. Several analysis techniques are presented, including: - measurement of centroid motion in and out of transit compared with detailed modeling of expected centroid motion, including an estimate of the transit source location - transit source location determination through a high-precision PSF-fit of the difference between in- and out-of-transit pixels, directly measuring the location of the transit source - source location determination through fitting the observed summed flux time series (or the light curve derived from the transit model) to each pixel's time series data. These techniques have been automated and are being considered for inclusion in the Kepler Science Operations Center Data Analysis Pipeline. They are supplemented by various diagnostic plots of the Kepler data as well as comparison with background stars identified by the Kepler Follow-up Observing Program (FOP). The final determination of whether an observed transit is a false positive integrates several sources, including pixel-level analysis and FOP results. Pixel-level techniques can identify BGEBs that are separated from the Kepler target star by more than a certain radius, called the "radius of confusion". The determination of the radius of confusion, and the role it plays in assigning the probability of the transit being due to a planet, is briefly discussed. The statistics from the latest false-positive list are provided. Funding for this mission provided by NASA's Discovery Program Office, SMD. 140.06 The Kepler Data Archive at MAST: What`s in it for me? Dorothy A. Fraquelli1, R. Thompson1, S. Tseng1, M. Smith1 1Computer Sciences Corp.. Exhibit Hall Hosted by MAST, the Multi-Mission Archive at Space Telescope, the Kepler Archive now contains over a year's worth of observations on more than 150,000 objects. The observations consist of light curves, both public and proprietary, target pixel files and full frame images (FFI). Supporting information includes data release notes, the Instrument Handbook, an Archive Manual and SPIE papers describing the instrument and data processing (in advance of the Kepler Data Hand Book). High level science products (HLSP) for the announced planets are available. The archive also contains the Kepler Input Catalog (KIC), the Kepler Target Catalog (KTC) and the Characteristics Table (CT). We will show examples of how to search for and retrieve data, including FFIs and light curves, how Kepler GOs and science team members can download their data from an ftp area, how to view public light curves and FFIs, and, for Kepler proposers, how to locate objects in the KIC. We will discuss the different ways of retrieving Kepler data. A companion poster details MAST's GALEX-Kepler cross-match catalog, a unique product that supplies UV colors to complement the KIC's ground-based observations. Demos of the web site are available at the STScI booth. 140.07 Public Kepler Data on the Bright Star Theta Cygni Michael Robert Haas1, S. T. Bryson1, J. F. Rowe1, M. D. Still2 1NASA Ames Research Center, 2BAER Institute. Exhibit Hall The bright star Theta Cygni (Kepler ID 11918630) has been observed by Kepler in both short (59 sec) and long (29.4 min) cadence for a period of approximately 50 days starting on MJD 55410. These observations were made at the request of the Kepler Guest Observer Office and are intended for immediate public release. The purpose is to demonstrate Kepler’s exquisite photometric precision on bright, highly saturated targets. Theta Cygni is a F3V/M3V binary with a visual magnitude of 4.9/13.0. The short-cadence data show evidence of granulation (i.e., convection) out to about 1 mHz (~100 c/d) and clear detection of numerous p-modes with a peak near 1.8 mHz (~150 c/d). The high-frequency noise floor has a 3-sigma upper envelope of 0.4 ppm. The amplitude of the p-modes agrees with the stellar effective temperature, indicating that the star has a thin convective layer. Since a custom aperture was employed, the light curves will be constructed manually and placed on the Guest Observer website (http://keplergo.arc.nasa.gov/). The corresponding pixel-level data will be available from the Kepler archive (http://archive.stsci.edu/kepler/). The Kepler mission can accommodate a small number of such bright targets every quarter. Observing proposals can be submitted annually to the peer-reviewed Guest Observer Program, or much less formally on a quarterly basis for Director’s Discretionary Time (see http://keplergo.arc.nasa.gov/GOprogramDDT.shtml). Kepler was selected as the 10th mission of the Discovery Program. Funding for this mission is provided by NASA, Science Mission Directorate. 140.08 Application of Bayesian Systematic Error Correction to Kepler Photometry Jeffrey E. Van Cleve1, J. M. Jenkins1, J. D. Twicken1, J. C. Smith1, M. N. Fanelli2 1SETI Institute/NASA Ames Research Center,, 2Bay Area Environmental Research Institute. Exhibit Hall In a companion talk (Jenkins et al.), we present a Bayesian Maximum A Posteriori (MAP) approach to systematic error removal in Kepler photometric data, in which a subset of intrinsically quiet and highly correlated stars is used to establish the range of “reasonable” robust fit parameters, and hence mitigate the loss of astrophysical signal and noise injection on transit time scales (<3d), which afflict Least Squares (LS) fitting. In this poster, we illustrate the concept in detail by applying MAP to publicly available Kepler data, and give an overview of its application to all Kepler data collected through June 2010. We define the correlation function between normalized, mean-removed light curves and select a subset of highly correlated stars. This ensemble of light curves can then be combined with ancillary engineering data and image motion polynomials to form a design matrix from which the principal components are extracted by reduced-rank SVD decomposition. MAP is then represented in the resulting orthonormal basis, and applied to the set of all light curves. We show that the correlation matrix after treatment is diagonal, and present diagnostics such as correlation coefficient histograms, singular value spectra, and principal component plots. We then show the benefits of MAP applied to variable stars with RR Lyrae, harmonic, chaotic, and eclipsing binary waveforms, and examine the impact of MAP on transit waveforms and detectability. After high-pass filtering the MAP output, we show that MAP does not increase noise on transit time scales, compared to LS. We conclude with a discussion of current work selecting input vectors for the design matrix, representing and numerically solving MAP for non-Gaussian probability distribution functions (PDFs), and suppressing high-frequency noise injection with Lagrange multipliers. Funding for this mission is provided by NASA, Science Mission Directorate. 140.09 Validation of Candidate Multiple-Transiting Planet Systems and Assessing Possible False Positives based on Photometric Observables Robert Morehead1, E. B. Ford1, Kepler Science Team 1University of Florida. Exhibit Hall Planetary systems with multiple planets that transit their host star are of great interest for studying the architecture of planetary systems (Steffen et al. 2010; Holman et al. 2010). Even space-based exoplanet transit surveys, such as CoRoT and Kepler, must be careful to exclude astrophysical false positives that can mimic the photometric signature of multiple-transiting planet system (MTPS). Due to large point spread functions, a putative MTPS might actually be: 1) a true MTPS, 2) a blend of an eclipsing binary and a star with a single transiting planet, 3) a blend of two eclipsing binaries, or 4) two stars each with a single transiting planet. Assessing the relative probability for each of these possibilities is important both for validating potential planets and for prioritizing the limited follow-up resources that can contribute to validation or confirmation of such systems. We introduce new observable parameters based on ratios of the measured transit durations in MTPSs, as well as the measured orbital periods and (when available) impact parameters. We explore the utility of these parameters for validating candidate MTPSs and/or rejecting false positives. For multiple planets around the same star, these parameters have values near one. The distribution of these parameters for certain blend scenarios can be markedly different. We investigate these distributions through Monte Carlo simulations of three different types of blends; planet-binary, binary-binary, and planet-planet and compare these to the distribution for true MTPSs. We present results based on previously released Kepler data and simulations using multiple distributions for the orbital inclinations, eccentricities, and binary star population. Kepler was selected as the 10th mission of the Discovery Program. Funding for this mission is provided by NASA, Science Mission Directorate 140.10 Kepler Eclipsing Binary Stars: on the Origin of Contact Binaries and the Degree of Thermal Contact Andrej Prsa1, E. F. Guinan1, S. Rucinski2, B. Kirk1, C. Villamil1 1Villanova University, 2University of Toronto, Canada. Exhibit Hall Contact binary stars (W UMa-type binaries) are one of most ubiquitous close binaries in our Galaxy. The components evolved into a system that shares a common envelope and features active mass transfer. Because of the components' proximity, orbital periods of these systems are short (2-18 hours) and the orbital velocities are large (100-300 km/s). It might be expected that contact binary envelopes are in thermal contact, yet the observations indicate otherwise. Further, the evolution of these stars is speculated to be due to either tidal/magnetic tightening of the orbit or to 3rd body interaction, yet to date there is no definitive consensus. Kepler holds great promise in resolving these puzzles since the ultra-high precision photometry allows us to model the target stars to unprecedented accuracy. In September 2010 we acquired high-resolution echelle spectra at the 4-m Mayall telescope (Kitt Peak, AZ) of 15 select contact binaries in the Kepler field at 5 phases distributed uniformly across the phase space. These observations provided us with the masses, projected semi-major axes, and center-of-mass radial velocities of program stars, and allowed us, in conjunction with the Kepler data, to completely characterize the absolute properties (masses, radii, temperatures, luminosities) of these prime W UMa-type binaries. Here we present a preliminary analysis of three select systems, KepIDs 8496820, 9392682, and 12305537, based on the public Kepler data and high-resolution spectroscopy. The final analysis of these and other stars will be supplemented with the proprietary Kepler data obtained through the Cycle II Guest Observer program 09-KEPLER09-0054, which we gratefully acknowledge. This work was funded in part by NSF/RUI grant AST-05-07542. 140.11 A Spectral and Lightcurve Study of 50+ Blue Stars from the Burrell-Optical-Kepler-Survey (BOKS) Jared Lalmansingh1, S. Howell2, D. Walter1, J. Cash1, K. Mighell2 1South Carolina State University, 2National Optical Astronomy Observatory. Exhibit Hall BOKS used the 0.6 m Burrell-Schmidt telescope over a period of 40 nights and identified 54,687 stars between 14 < r < 19 in the Kepler Mission’s field of view. Its primary goal was to detect Jupiter-sized and Hot Jupiter (Period = 3 - 9 days) short-period exoplanets within the survey field as well as to compile high precision stellar variability data that the Kepler Mission can use for comparison purposes and to characterize the hundreds of other variable stars within the survey region. We present the spectral classifications and light curve analysis of a sub-sample of 50+ blue stars within the BOKS field of view using BOKS lightcurve data and spectra from the Kitt Peak 2.1 meter telescope. The purpose of this study is to identify the variability of and provide characterization for the blue star population within the BOKS field. Support for this work was provided by NOAO and the NSF PAARE program to South Carolina State University under award AST-0750814. 140.12 A Method for Determining Precise Phase Shifts of Eclipses in EB Systems: Detecting Substellar, Non-Transiting Third Bodies in Kepler Mission Eclipsing Binary Light Curves. Robert W. Slawson1, L. R. Doyle1 1SETI Institute. Exhibit Hall A third body orbiting an eclipsing binary induces a small phase shift in the eclipses due to the light time effect as the binary system orbits about the three-body barycenter. The presence of the small third-body is revealed by a periodicity in the phase shifts consistent with a Keplerian orbit. We present a cross-correlation method that benefits from the nearly continuously sampled light curves now becoming available from the Kepler mission. For the template, we use a model light curve of the binary system that is stationary in phase (dP/dt=0, d?/dt=0, ...). A window function slides in time along both the observed light curve and template selecting a region for cross-correlation and the phase shift as a function of time is determined from the peak in the resulting correlation function. We examine the sensitivity limits, through numerical experiments, to the detection of substellar and planet sized masses in multi-year orbits about EBs from Kepler mission light curves. 140.13 Kepler Systems That Show Multiple Transiting Objects Jason H. Steffen1, D. C. Fabrycky2, E. B. Ford3, M. J. Holman4, J. J. Lissauer5, D. Ragozzine4, W. F. Welsh6, Kepler Science Team 1Fermilab, 2UC Santa Cruz, 3University of Florida, 4Harvard CfA, 5NASA Ames, 6San Diego State University. Exhibit Hall Exoplanetary systems that have multiple transiting planets provide unique and important insight into the formation, evolution, and dynamics of exoplanetary systems. Kepler has announced the discovery of a confirmed planetary system with multiple transiting planets (Kepler 9, Holman et al. 2010) as well as several candidate planetary systems that show multiple transiting objects (Steffen et al. 2010). Kepler 9 shows deviations from a constant period due to the ongoing dynamical interactions between the confirmed planets. From these transit timing variations (TTV) one can measure the planetary masses from the photometric data alone. The presence of several systems with multiple transiting candidates from the first quarter of data indicate that Kepler should continue to find systems with multiple transiting planets. Such systems will provide important, general information about the histories of planetary systems. 140.14 The Faring Behavior of G and K Dwarfs as Seen in the Kepler Q1 Data Peiyuan Mao1, D. Soderblom2, R. Osten2, J. Valenti2 1Lafayette College, 2Space Telescope Science Institute. Exhibit Hall The white-light photometric observations from the Kepler mission are the first ever look at the behavior of solar-type stars at ultra-high precision, and the light curves made available in the “Q1” data release show many astrophysical phenomena. Especially evident in a small fraction of the G and K dwarfs are flaring events, with rapid rises and exponential decays. These flares have much greater energies and longer decay time-scales than even the largest solar flares, which would be undetectable given Kepler’s 30-minute observing cadence. Moreover, stars that exhibit flares tend to show several flares during the 33.5 day interval covered by the Q1 data. Aside from the Kepler data itself, little is known about these stars and what sets them apart from other Kepler targets with similar rotation periods and variability amplitudes. We will show examples of flares in the Kepler light curves, describe our detection technique, and present our initial findings on this phenomenon. 140.15 Parameterizing and Modeling Eclipsing Binaries in The Kepler Field Using Kepler Quarter 2 and 3 Data Sean Morrison1, K. Mighell2, S. Howell2, D. Bradstreet3 1Appalachian State University, 2National Optical Astronomy Observatory, 3Eastern University. Exhibit Hall We present a preliminary analysis of Quarter 2 and Quarter 3 Kepler light curves for 56 eclipsing binary star systems from the Kepler Cycle 1 program 08-KEPLER08-0014, "A Calibration Study of Variable Stars in the Kepler Field" (PI: Mighell). We developed a C program to phase these long cadence (30 minute) data that determines the period and zero point with a typical precision of 0.0864 seconds for an orbital period of 1.019949 days. We have developed 3D models of the systems using Binary Maker 3 (BM3) by David Bradstreet. Spectra of 32 of the systems were obtained at the Kitt Peak National Observatory 2.1 m telescope using the GoldCam spectrometer. We have determined temperatures for some of the stars from the temperature ratios, based on the BM3 models, and the average temperatures for the spectral classifications of the stars which were derived from the 2.1-m spectra. The high photometric precision of the Kepler light curves allows us to identify significant star spots on a subset of the systems. Morrison was supported by the NOAO/KPNO Research Experiences for Undergraduates (REU) Program which is funded by the National Science Foundation Research Experiences for Undergraduates Program and the Department of Defense ASSURE program through Scientific Program Order No. 13 (AST-0754223) of the Cooperative Agreement No. AST-0132798 between the Association of Universities for Research in Astronomy (AURA) and the NSF. 140.16 Cross Matching of Available GALEX Objects with Kepler Targets at MAST Myron Smith1, B. Shiao2, Kepler 1Computer Sciences Corp., 2Space Telescope Science Institute. Exhibit Hall The recent release of the GALEX Release 6 dataset includes 72 sky "tiles" overlapping some 60% of the Kepler Field of View. MAST (Multi-Mission Archive at Space Telescope Science Institute) has constructed a cross-match catalog of all matches of GALEX objects with 5" of the coordinates for objects in the Kepler Input Catalog (KIC) and vice-versa. The results permit the addition of UV colors (near-UV and/or far-UV, centered at about 2300 Angstroms and 1500 Angstroms, respectively) to the SDSS program's griz filters that the Kepler ground-based support photometric program emulated. Until now the absence of an ultraviolet filter for this ground survey of KIC objects has meant that it was not possible to clearly identify hot (OBA-type) objects. The addition of the GALEX UV magnitudes will address this deficiency. In addition, the (FUV-NUV) vectors for ISM reddening and stellar temperature are very different, allowing the former degeneracy of the two terms to be lifted. We exhibit on-line tools to enable users to obtain UV, griz, and 2MASS colors to aid in the search of targets and to investigate general distributions of objects in the KIC. We discuss completeness of the cross-match survey with the KIC catalog. We point out that the numbers of detections are primarily limited by the far-UV and near-UV effective apertures of GALEX. 140.17 Kepler Light Curves of AGN Michael T. Carini1, W. Welsh2 1Western Kentucky University, 2San Diego State University. Exhibit Hall The Kepler mission is observing the same region of the sky for its entire mission lifetime, allowing virtually uninterrupted optical observations of any object in its field of view. This provides the opportunity to obtain optical light curves of AGN of unprecedented duration and sampling. During cycle 1, we obtained observations of two bright AGN in the Kepler field of view: the Seyfert 1 galaxy ZW 229.015 and the Seyfert 2 galaxy IGR J19473+4452. We present the light curves of these sources and discuss their variability properties. Because the Kepler Pipeline is optimized for detecting transiting planets, not photometry of extended sources, we also discuss potential systematic problems and cautions one must have when interpreting these light curves. 140.18 Mining the Kepler Mission Database: Rotations, Starspots, Ages and Possible Tidal Interactions of Stars with Close-in Planets Greg Feiden1, E. Guinan2, T. Boyajian3, Y. Kok4, O. Basturk5, A. Roberson6, I. Ribas7 1Dartmouth College, 2Villanova University, 3Georgia State University, 4University of Sydney, Australia, 5Ankara University, Turkey, 6Pennsylvania State University, 7Institut de Ciencies de l'Espai, Spain. Exhibit Hall The first public data release from the Kepler Space Telescope contained over 156,000 stars which had been monitored continuously for approximately 33 days. With continuous photometric monitoring and unprecedented ultra-high precision, the Kepler dataset is an splendid resource for investigating stellar rotation (and age) via starspots as well as for investigating starspot fractional coverage and distributions, starspot lifetime and differential rotation as a function of spectral type and rotation/age. Here, we narrowed our focus to the ~306 planetary candidates, mostly main sequence late F, G and K stars, released during June 2010 (see Boruki et al. 2010). This is an attractive data set for the study of starspots properties since these stars host transiting planets with orbital planes almost exactly aligned with our line-of-sight and will generally have the host stars' rotation axes perpendicular to the planetary orbital plane. Thus, the inclination of the star's rotation axis can be assumed known and should (in most cases) be at right angles to our line-of-sight. Using a Lomb-Scargle Periodogram analysis, we have extracted reliable rotation periods and spot coverages for stars which showed evidence for starspots. From the measured rotation periods, we were able to determine, empirically, the age of the stellar system (using Villanova rotation-age relations) and investigate the potential tidal evolution of the planet-star system. However, we found good evidence that rotation-age relations do not apply to stars that host short-period, Jupiter sized planets. The aforementioned stars show a definite tendency towards star-rotation-planet orbital synchronization. The initial results of this exploratory program will be discussed. This project was initiated at the 2010 Sagan Exoplanet Summer Workshop hosted by NExScI at Caltech. We wish to thank NASA and the organizers of the workshop - in particular Dawn Gelino and Carolyn Brinkworth. EG wishes also to acknowledge support from NSF/RUI Grant AST-10-09903. 140.19 Piecing Together Planet Populations: How RV Super-Earth Frequency Predictions Measure up to Kepler’s Planet Candidates Angie Wolfgang1, G. Laughlin1 1University of California, Santa Cruz. Exhibit Hall Based on the mass and period distributions of the super-Earths discovered by the Geneva Extrasolar Planet Search, there are expected to be planets less massive than Neptune orbiting a large fraction of main sequence stars in periods of 50 days or less. Expanding on this prediction, we employ a Monte Carlo method to create populations of super-Earths with varying compositions, mass distributions, and period distributions. We then compare the results of these simulations with the planet candidates announced by Kepler on June 15, 2010, calculating a statistical best fit to identify the radial velocity super-Earth population which is most likely to reproduce Kepler’s population of planet candidates. 140.20 Kepler Measurements of M Star Variability Geoffrey Bryden1, J. Stauffer2, D. R. Ciardi3, NStED Science Team 1JPL, 2Caltech, 3NExScI. Exhibit Hall Late-type stars may be ideal candidates for detection of Earth-mass planets - lower stellar mass corresponds to larger radial-velocity amplitude and deeper transit depth for a given planet mass/size. Low-mass stars are only good targets, however, if they can be observed at noise levels similar to those for solar-type stars. As an exploration of the inherent variability of low-mass stars, we have identified a sample of 63 nearby M dwarfs within the Kepler field of view. The Kepler lightcurves for these stars generally vary by ~1% over the 33-day observational window. After subtraction of gradual long-term trends, only a handful of the stars exhibit variability above the photon-noise limit (typically 0.1-1.0 mmag). We conclude that >90% of M dwarfs are quiet within the several hour timeframe appropriate for detection of planetary transits. 140.21 Confirming sub-Neptunian Transiting Exoplanets with Kepler Natalie M. Batalha1, Kepler Science Team 1San Jose State University. Exhibit Hall NASA's Kepler Mission, launched in March 2009, uses transit photometry to detect and characterize exoplanets with the objective of determining the frequency of earth-size planets in the habitable zone. The instrument is a wide field-of-view (115 square degrees) photometer comprised of a 0.95-meter effective aperture Schmidt telescope feeding an array of 42 CCDs that continuously and simultaneously monitors the brightness of up to 170,000 stars. In January, 2010, the team announced its first 5 planet discoveries identified in the first 43 days of data and confirmed by radial velocity follow-up. The "first five" are all short-period giant planets, the smallest being comparable in size to Neptune. Collectively, they are similar to the sample of transiting exoplanets that have been identified to date, the roster of which currently hovers around 100. In August 2010, an additional two planets, each orbiting the star Kepler-9, were confirmed by a combination of radial velocity and transit timing measurements. A third, smaller planet in the same system was validated stastistically by probing the parameter space for potential false-positives. Throughout 2010, a concerted effort was made to push radial velocity confirmation down toward the smaller planets. Recent progress on our efforts to confirm such candidates is discussed. 141 Gamma Ray Bursts Poster Session Exhibit Hall 141.01 High Metallicity LGRB Hosts John Graham1, A. Fruchter2, E. Levesque3, L. Kewley3, J. Brinchmann4, S. Charlot5, A. Levan6, N. Tanvir7, S. Patel8, K. Misra2, K. Huang9, D. Reichart10, M. Nysewander2 1STScI & JHU, 2STScI, 3IFA, 4Leiden, Netherlands, 5Bordeaux, France, 6Warwick, United Kingdom, 7Leicester, United Kingdom, 8National Space Science & Technology Center, 9JHU, 10UNC. Exhibit Hall One of the most powerful means to study the formation and evolution of gamma-ray bursts is by observing there environments. While short bursts have been detected in nearby galaxies of all types, long burst hosts are dominated by blue irregulars leading to speculation of metal poor host galaxies, a result which has now been confirmed via emission line metallicity diagnostics. However beginning with LGRB 051022 at log(O/H)+12 = 8.77 (using the R23 method with Kobulnicky & Kewley 2004 scale) three exceptions to this trend have been found. This extends the metallicity range of LGRB hosts to that found throughout the Milky Way, challenges conventional wisdom that LGRBs require low metallicity progenitor environments and has significant implications in understanding LGRB formation. Here I present the results of our observations of two of these super-solar metallicity host galaxies, analysis of the high Z host population with respect to various comparison samples, and ongoing efforts to more directly probe the metallicities of the burst progenitors. 141.02 The Stellar Ages and Masses of Short GRB Host Galaxies: Investigating the Progenitor Delay Time Distribution and the Role of Mass and Star Formation in the Short GRB Rate Camille N. Leibler1, E. Berger1 1Harvard University. Exhibit Hall We present multi-band optical and near-infrared observations of 19 short ?-ray burst (GRB) host galaxies, aimed at measuring their stellar masses and population ages. The goals of this study are to evaluate whether short GRBs track the stellar mass distribution of galaxies, to investigate the progenitor delay time distribution, and to explore any connection between long and short GRB progenitors. Comparing the distribution of stellar masses found using a single-stellar population model to the general galaxy mass function, we find that short GRBs track the cosmic stellar mass distribution only if the late-type hosts generally have maximal masses. However, there is an apparent dearth of early-type short GRB hosts compared to the equal contribution of early- and late-type galaxies to the cosmic stellar mass budget. These results suggest that stellar mass may not be the sole parameter controlling the short GRB rate, and raise the possibility of a two-component model with both mass and star formation playing a role (reminiscent of the case for Type Ia supernovae). If short GRBs in late-type galaxies indeed track star formation activity, the resulting typical delay time is ? 0.2 Gyr, while those in early-type hosts have a typical delay of ? 3 Gyr. Using the same stellar population models to fit 22 long GRB host galaxies in a similar redshift range we find that they have significantly lower masses and younger population ages. Most importantly, the two GRB host populations remain distinct even if we consider only the star-forming hosts of short GRBs, supporting our previous findings (based on star formation rates and metallicities) that the progenitors of long GRBs and short GRBs in late-type galaxies are distinct. This work was partially supported by Swift AO5 grant #5080010 and AO6 grant #6090612. Additional support was provided by the Harvard College Research Program. 141.03 A Beaming-Independent Estimate of the Distribution of Gamma Ray Burst Energies Isaac S. Shivvers1, E. Berger1 1Harvard University. Exhibit Hall AAS 217 Winter Meeting Abstract Submission Isaac Shivvers and Dr. Edo Berger Harvard University A Beaming-Independent Estimate of the Distribution of Gamma Ray Burst Energies The single most important parameter of any cosmological explosion is the energy release. Energy measurements provide insight into the progenitor object and the explosion mechanism. The measurement of gamma-ray burst (GRB) energies has, traditionally, been a complicated problem due to highly non-spherical energy distributions and relativistic beaming effects. However, on timescales of >100 days GRBs become roughly non-relativistic and spherical. Using radio observations from the Very Large Array at times >100 days after the burst, we are able to calculate the energies of 20 bursts free from the large corrections needed when using early-time observations. We find a median energy in good agreement with results calculated through detailed analysis of multi-wavelength light curves. The similarity between methods provides further evidence that the bulk of the energy budget of GRBs is in the relativistic outflow and not in slower, lagging material. Our results were achieved economically, with only a few radio-wavelength flux measurements per GRB. We suggest that similar future observations with the Expanded VLA will provide unique insight into GRB energetics. 141.04 Quantifying GRB Pulse Shape Evolution to Study the Pulse Scale Conjecture Daniel Miller1, R. J. Nemiroff1, J. Holmes1, A. Shahmoradi1 1Michigan Technology University. Exhibit Hall The asymmetry of isolated gamma ray burst pulses is quantified by a simple ratio of rising to decaying fluence. This ratio can be defined in a background independent way by using only the peak of the pulse. This ratio is used to explore the prevalence of the Pulse Scale Conjecture (PSC; Nemiroff 2000) for a series of the brightest isolated BATSE GRB pulses known. The PSC posits that the shape of a GRB pulse is invariant across energy channels, scaling only in time and brightness. Within statistical uncertainties, it is found that some GRB pulses hold well to the PSC, whereas others do not. Moreover, for some GRB pulses, the PSC appears to hold only between specific energy channels. Examples will be shown and discussed. 141.05 Evidence for a Correlation Between Gamma-Ray Burst Variability and the Optical Afterglow Onset Sarah Yost1 1St John's Univ.. Exhibit Hall The intrinsic variability (V) of prompt gamma-ray emission from gamma-ray burst (GRB) events is compared to the properties of the subsequent afterglow onset, yielding evidence of a correlation between V and the the optical onset's peak. We used Liang et al.'s (2009) fitted properties of the optical onset bump in 16 events with an observed optical rise and known redshift, and calculated V from the lightcurves in the Swift gamma-ray data archive. The optical onset properties are known to be mutually correlated; comparing these optical bump properties to V shows positive correlations at the 3-sigma level with (de-redshifted) width, peak time, rise, and decay times and negative correlations with peak flux and the ratio of rise to decay times. When the bump peak time or width are expressed as a ratio of the GRB duration (T90), the correlation evidence with V is weaker. 141.06 Pulse Scaling Properties of Gamma-Ray Bursts Justin Holmes1, R. J. Nemiroff1, D. Miller1 1Michigan Technological University. Exhibit Hall Gamma-ray bursts (GRBs) hold potential as standard candles for the high redshift universe. To help identify relationships which may arise in GRBs that could lead to a standard candle, isolated pulses from a number of very bright GRBs were inspected regarding their pulse scaling nature. A direct test of the pulse scale conjecture was conducted using energy channel data from the Burst and Transient Source Experiment (BATSE).  The test consisted of taking a light curve for a bright GRB pulse from a specific BATSE energy channel, scaling it in brightness and time, and finding the best statistical fit for the same GRB pulse in a different BATSE energy channel. Many of the GRB pulses tested showed a statistically acceptable scaling between at least two BATSE energy channels. 141.07 Search for Late Jet Breaks in X-ray Afterglows of Gamma-Ray Bursts David N. Burrows1, J. Racusin2 1Penn State Univ., 2NASA/GSFC. Exhibit Hall Gamma-ray bursts are the most energetic events known since the Big Bang. Because both the prompt emission and the afterglow of GRBs is highly beamed, determination of their actual explosion energies depends on measurement of the beaming angle, which can be estimated on the basis of the detection of an achromatic jet break in the light curve. Jet break measurements for Swift GRBs have been rare; as a result, we have undertaken a program of studying X-ray GRB afterglows using the Chandra observatory to obtain very late-time flux measurements. When compared with earlier Swift XRT flux measurements, these allow the measurements of late jet breaks in some bursts, and allow strict limits to be placed on jet break times in other cases. We will present a progress report on this work and its implication for GRB energetics. 142 AGN, QSO, Blazars Poster Session Exhibit Hall 142.01 15 GHz Radio Variability of Gamma-Ray Blazars Joseph Richards1, W. Max-Moerbeck1, V. Pavlidou1, T. J. Pearson1, A. C. S. Readhead1, M. A. Stevenson1, O. G. King1, R. Reeves1, E. Angelakis2, L. Fuhrmann2, J. A. Zensus2, S. E. Healey3, R. W. Romani3, M. S. Shaw3, K. Grainge4, G. B. Taylor5, G. Cotter6 1California Institute of Technology, 2Max-Planck-Institut-für-Radioastronomie, Germany, 3Stanford University, 4University of Cambridge, United Kingdom, 5University of New Mexico, 6University of Oxford, United Kingdom. Exhibit Hall Since 2007, the Owens Valley Radio Observatory (OVRO) 40 meter telescope has been engaged in an intensive fast-cadence gamma-ray blazar monitoring program, observing about 1500 objects twice per week. Using our intrinsic modulation index method and careful likelihood analyses, we find that gamma-ray loud objects associated with Fermi 1LAC sources in our sample demonstrate radio variability amplitudes significantly larger than do gamma-ray quiet objects. We also find significant differences in variability amplitude between flat spectrum radio quasars and BL Lacertae objects within our sample as well as possible evidence for cosmological evolution of variability amplitude. 142.02 Physical Significance Of The Time Lags In Radio/gamma-ray Cross-correlations For Fermi-gst Blazars On The Ovro 40m Blazar Monitoring Program Walter Max-Moerbeck1, J. L. Richards1, V. Pavlidou1, T. J. Pearson1, A. C. S. Readhead1, M. A. Stevenson1, O. King1, R. Reeves1, E. Angelakis2, L. Fuhrmann2, J. A. Zensus2, S. E. Healey3, R. W. Romani3, M. S. Shaw3, K. Gainge4, G. B. Taylor5, G. Cotter6 1California Institute of Technology, 2Max-Planck-Institut für Radioastronomie, Germany, 3Stanford University, 4University of Cambridge, United Kingdom, 5University of New Mexico, 6University of Oxford, United Kingdom. Exhibit Hall The OVRO 40 m telescope has been monitoring ~1500 blazars since 2007. The sources are observed twice per week at 15 GHz. The sample contains all CGRaBS sources and the gamma-ray blazars detected by Fermi which are visible from OVRO. The availability of a large sample of sources with good cadence at radio and gamma-ray offers the opportunity to test the suggestion of correlated variability between these two bands. A Monte Carlo method to assess the physical significance of the cross-correlations taking into account the properties of the light curves and the uneven sampling is presented. Application to an early data set shows that in most cases the cross-correlations are not significant and that longer time duration light curves are required. 142.03 Testing the Radiative-Driving Hypothesis of Quasar Outflows Michele A. Stark1, R. Ganguly1, S. C. Gallagher2, R. Gibson3, M. S. Brotherton4 1University of Michigan - Flint, 2University of Western Ontario, Canada, 3University of Washington, 4University of Wyoming. Exhibit Hall Outflows are seen prominently in the UV spectra of Broad Absorption Line (BAL) QSOs. Models of radiatively-driven outflows predict that the velocity should scale with UV luminosity. Observations show that the UV luminosity only provides a cap to the velocity. One explanation is that the X-ray absorbing gas in an individual quasar provides a shield that improves its radiative-driving efficiency. That is, quasars with thick shields can accelerate gas to higher velocity. X-ray observations of BALQSOs support this in the sense that BALQSOs with more soft X-ray absorption tend to have higher velocity outflows. But there is much scatter in this trend, making the underlying physics difficult to extract. To combat this, we conducted an experiment using exploratory Chandra-ACIS observations of 12 carefully-selected z=1.7-2.0 BALQSOs. These BALQSOs were chosen to have very narrow ranges in (1) UV luminosity, (2) UV spectral shape, and (3) absorption velocity width. Within this otherwise uniform sample, the outflow velocities range from 4500km/s to 18000km/s, a factor of four. All objects are detected in the full band (0.5-8keV), with count rates in the range (0.5-5)e-3 cps, and have hardness ratios in the range -0.6 to 0.3. We compare the X-ray brightnesses and spectral shapes of our sample with those of more diverse samples of BALQSOs. We gratefully acknowledge support through Chandra grant GO9-0120X. 142.04 Toward a Prescription for Feedback from Quasar Outflows Rajib Ganguly1, M. Bourjaily1, J. Munsell1, M. S. Brotherton2, A. Bhattacharjee2, J. Runnoe2, J. C. Charlton3, M. Eracleous3 1Univ. of Michigan-Flint, 2Univ. of Wyoming, 3The Pennsylvania State University. Exhibit Hall Models have shown that quasars are a crucial ingredient in the evolution of massive galaxies. Outflows play a key role in the story of quasars and their host galaxies, by helping regulate the accretion process, the star-formation rate and mass of the host galaxy (i.e., feedback). The prescription for modeling outflows as a contributor to feedback requires knowledge of the outflow velocity, distance, geometry, and column density. In particular, we need to understand how these depend on physical parameters and how much is determined stochastically (and with what distribution). For this purpose, we are examining a sample of 14000 z=1.7-2.0 quasars from the Sloan Digital Sky Survey. This redshift range permits the following from the SDSS spectra: (1) separation of objects that do and do not exhibit outflows; (2) classification/measurement of outflow properties (ionization, velocity, velocity width); and (3) estimates of the quasar black hole mass. To this, we are adding photometry from GALEX, 2MASS, and ROSAT in an effort to characterize more fully the quasar SEDs. ROSAT photometry provides estimates of the level of soft X-ray absorption, which helps regulate the velocity of outflows. GALEX photometry samples the extreme ultraviolet range where several high ionization species, that may be present in the outflows, absorb light. 2MASS photometry samples the rest-frame optical, where the effects of absorption and dust reddening are minimal, yield better estimates of the bolometric luminosity (hence, Eddington ratio). In this poster, we will present preliminary measurements of the amount of absorption in the soft X-ray and extreme ultraviolet bands as a function of both outflow properties and quasar physical properties. This material is based upon work supported by the National Aeronautics and Space Administration under Grant No. 09-ADP09-0016 issued through the Astrophysics Data Analysis Program. 142.05 Recent Star-formation in Post-Starburst Quasars Shonda Townsend1, R. Ganguly1, A. Strom2, S. Cales3, M. S. Brotherton3 1University of Michigan - Flint, 2University of Arizona, 3University of Wyoming. Exhibit Hall Post-Starburst Quasars (PSQ, alternatively Q+As) show simultaneously the spectrum of a massive A-type stellar population and a quasar. The prototype PSQ, UNJ1025-0040, shows a UV excess over the quasar spectrum, indicating more recent star-formation (Brotherton et al 2002). To gauge the frequency and distribution of these younger stellar populations in PSQs, we have collected GALEX (GR45) and 2MASS photometry for 409 objects. The objects are catalog 609 spectroscopically-selected PSQs from Brotherton et al. (2010) that uses similar criteria as Zabludoff et al. (1996) for post-starburst galaxies (PSG, E+A). For comparison, we have compiled two samples: (1) 16,000 quasars that is matched in redshift (0.01-0.7) and Sloan-u magnitude (16.1-21.2), which is blueward of the Balmer edge and provides the least contamination from the massive stellar population; and (2) 500 PSGs from Goto et al. (2007). 389 (55) PSQs show an NUV (FUV) excess over the expected UV flux if the underlying quasar were ``normal.’’ 126 (460) objects show an NUV (FUV) decrement. The observed NUV to u-band flux ratio of the median PSQ rises from ~1 at z=0.01 to 2.5 at z=0.4, while the same for the median QSO remains at ~1. The observed FUV to u-band flux ratio of the median QSO rises slightly from ~0.6 to ~0.8 over the redshift range 0.05-0.2, whereas the median PSQ is nearly a factor of three lower. The disparity between the median PSQ and QSO suggests the presence of young stars that add in NUV light, but not FUV light. To quantify the youth and mass of this putative population, we will present preliminary efforts to model PSQs using two simple stellar populations, an underlying quasar, and dust reddening. We acknowledge funding from GALEX through grant NNX10AC63G. 142.06 Parsec-Scale Localization of the Quasar SDSS J1536+0441A, a Candidate Binary Black Hole System J. M. Wrobel1, A. Laor2 1NRAO, 2Technion, Israel. Exhibit Hall The radio-quiet quasar (RQQ) SDSS J1536+0441A shows two broad-line emission systems, recently interpreted as a binary black hole (BBH) system with a subparsec separation; as a double-peaked emitter (DPE); or as both types of systems. The NRAO VLBA was used to search for 8.4 GHz emission from SDSS J1536+0441A, focusing on the localization region for the broad-line emission, of area 5400 mas2 (0.15 kpc2). One source was detected, with a diameter of less than 1.63 mas (8.5 pc) and a brightness temperature Tb > 1.2 x 107 K. New NRAO VLA photometry at 22.5 GHz, and earlier photometry at 8.5 GHz, gives a rising spectral slope of alpha = 0.35+/-0.08. The slope implies an optically thick synchrotron source, with a radius of about 0.04 pc, and thus Tb ~ 4.8 x 1010 K. The implied radio sphere at the rest frequency 31.2 GHz has a radius of 800 gravitational radii, just below the size of the broad line region in this object. Observations at higher frequencies with the EVLA and ALMA can probe whether or not the radio sphere is as compact as expected from the coronal framework for the radio emission of RQQs. The NRAO is a facility of the NSF operated under cooperative agreement by AUI. 142.07 Galaxy-scale Clouds Of Ionized Gas Around Agn - History And Obscuration Drew Chojnowski1, W. C. Keel2 1Texas Christian University, 2University of Alabama. Exhibit Hall Motivated by the discovery of Hanny's Voorwerp, a 45-kpc highly-ionized cloud near the spiral galaxy IC 2497, and accompanying evidence for strong variability of its AGN over 105 year scales, members of the Galaxy Zoo project have carried out surveys for similar (albeit smaller) ionized clouds around galaxies both with and without spectroscopic AGN. The color-composite SDSS images detect strong [OIII] in the g band at low z, allowing a useful color search of Galaxy Zoo targets. In addition, a targeted search was made of over 16,000 spectroscopic AGN and candidates. We used SDSS data to produce crude [OIII] images of the top candidates, and obtained long-slit optical spectra from KPNO and Lick for 30 of the most promising. Roughly half of the spectra showed extended [OIII]?5007 emission, some exceeding 30 kpc in radial extent. Of the 16 extended clouds we identified, 11 lie in strongly interacting or merging systems, probably because these events leave cold gas out of the plane to be ionized. Most nuclei of extended cloud hosts are type 2 Seyferts. We consider the energy budgets, between ionizing luminosity required for the most distant line emission and the FIR output of the nucleus, to see whether any suggest strong variability rather than obscuration. Several galaxies have such strong mismatches that obscuration alone becomes implausible as an explanation for the strong ionizing continuum, and are candidates for fading events similar to that in IC 2497 and Hanny's Voorwerp. This project was funded by the National Science Foundation Research Experiences for Undergraduates (REU) program through grant NSF AST-1004872. 142.08 The History And Environment Of A Faded Quasar: HST Observations Of Hanny's Voorwerp And IC 2497 William C. Keel1, C. Lintott2, K. Schawinski3, V. Bennert4, D. Thomas5, A. Manning1, S. D. Chojnowski6, H. van Arkel7, S. Lynn8, Galaxy Zoo team 1Univ. of Alabama, 2Adler Planetarium, 3Yale Univ., 4UCSB, 5Univ. of Portsmouth, United Kingdom, 6Texas Christian Univ., 7CITAVERDE College, Netherlands, 8Oxford Univ., United Kingdom. Exhibit Hall Perhaps the signature discovery of the Galaxy Zoo citizen-science project has been Hanny's Voorwerp, high-ionization cloud extending 45 kpc from the spiral galaxy IC 2497. It must be ionized by a luminous AGN, either deeply obscured or having dimmed dramatically within 200,000 years. We explore this system using HST imaging and spectroscopy. The disk of IC 2497 is warped, with complex dust absorption near the nucleus; the near-IR peak coincides closely with the VLBI core marking the AGN. STIS spectra show the AGN as a low-luminosity LINER, with ionization parameter log U= -3.5, matching its weak X-ray emission. The nucleus is accompanied by an expanding loop of ionized gas ? 500 pc in diameter, opposite Hanny's Voorwerp. The loop's Doppler span 300 km/s implies kinematic age < 700,000 years. We find no high-ionization gas near the core, further evidence that the AGN is seen at a low radiative output (perhaps now dominated by kinetic energy). [O III] and H? +[N II] ACS images show fine structure in Hanny's Voorwerp, including limb-brightened sections suggesting modest interaction with a galactic outflow. We identify small regions ionized by recent star formation, unlike the AGN ionization of the overall cloud. These H II regions contain blue continuum objects, consistent with young stellar populations; these occur where projected closest to IC 2497, perhaps meaning that the star formation was triggered by compression from an outflow. The ionization-sensitive [O III]/H? ratio shows broad bands across the object, and no discernible pattern with emission-line structures or near the prominent "hole" in the ionized gas. These results fit with our picture of an ionization echo from an AGN whose ionizing luminosity has dropped by a factor >100 within the last 200,000 years. Such rapid fluctuations in luminosity could alter our understanding of AGN demographics. Supported by NASA/STScI. 142.09 Twenty-Year Optical Variability of The Blazar PKS 1749+096: Exponential Outbursts? Thomas J. Balonek1, M. T. Lam1, P. A. Patrick1, E. L. Scott1, A. J. Kaercher1, J. Rupert2, T. Taber2, P. Hegel3, Y. H. N. Tam4, A. Morin5, K. Levandowski6, E. L. Graber7, T. S. Quirk8 1Colgate Univ., 2Vassar Coll., 3Wesleyan Univ., 4Williams Coll., 5RPI, 6Wellesley Coll., 7Univ. Michigan, 8Siena Coll.. Exhibit Hall We present the twenty-year R-band optical variability light curve for the BL Lac type quasar PKS 1749+096. We investigate the characteristic timescales and intensity of outbursts and flares by fitting exponential profiles to the variations. PKS 1749+096 underwent strong optical outbursts during the summers of 2007 and 2008, reaching its brightest optical level in two decades, and exhibited an inactive period during summer 2009. We compare these two outbursts with lower amplitude well-sampled variations in 2000 through 2003. Observations were obtained as part of the intensive blazar variability monitoring program at the Colgate University Foggy Bottom Observatory (FBO). We gratefully acknowledge support for student research through an REU grant to the Keck Northeast Astronomy Consortium from the National Science Foundation, the NASA / New York Space Grant, and the Justus and Jayne Schlichting Student Research Fund at Colgate University. 142.10 Time Series Analysis of the Quasar PKS 1749+096 Michael T. Lam1, T. J. Balonek1 1Colgate University. Exhibit Hall Multiple timescales of variability are observed in quasars at a variety of wavelengths, the nature of which is not fully understood. In 2007 and 2008, the quasar 1749+096 underwent two unprecedented optical outbursts, reaching a brightness never before seen in our twenty years of monitoring. Much lower level activity had been seen prior to these two outbursts. We present an analysis of the timescales of variability over the two regimes using a variety of statistical techniques. An IDL software package developed at Colgate University over the summer of 2010, the Quasar User Interface (QUI), provides effective computation of four time series functions for analyzing underlying trends present in generic, discretely sampled data sets. Using the Autocorrelation Function, Structure Function, and Power Spectrum, we are able to quickly identify possible variability timescales. QUI is also capable of computing the Cross-Correlation Function for comparing variability at different wavelengths. We apply these algorithms to 1749+096 and present our analysis of the timescales for this object. Funding for this project was received from Colgate University, the Justus and Jayne Schlichting Student Research Fund, and the NASA / New York Space Grant. 142.11 Feedback from radio-quiet quasars Nadia L. Zakamska1, J. E. Greene2 1KIPAC/Stanford, 2UT Austin. Exhibit Hall The correlations between properties of supermassive black holes and stellar spheroids in nearby galaxies strongly suggest that there is a physical connection between these two components, even though their masses and physical scales are vastly different. There is growing evidence that radio-loud active galactic nuclei exert a strong feedback on the gas in their host galaxies, providing a possible mechanism for such connection. However, as only a minority of active galaxies are radio-loud at any given time, the radio-loud feedback may only be a part of the explanation. Here we report the discovery of powerful outflows from radio-quiet quasars observed in the emission lines of the photo-ionized gas. 142.12 Optical Spectra of the Teacup AGN Justin Gagne1, D. M. Crenshaw1, W. C. Keel2, T. C. Fischer1 1Georgia State University, 2University of Alabama. Exhibit Hall We present optical spectra of the "Teacup AGN", at a redshift of 0.085, discovered in the Sloan Digital Sky Survey (SDSS). The spectra were obtained with the Lowell Observatory 1.8-m Perkins telescope. The SDSS image shows a "handle" of ionized gas extending out to 5'' (8 kpc) away from the nucleus of the galaxy. Our optical spectra reveal a myriad of emission lines resembling those from a typical Seyfert 2 galaxy. We use dereddened emission-line ratios to investigate the physical conditions in the gas and to estimate the luminosity of the hidden AGN. 142.13 Multi-wavelength Probes of Obscuration Towards the Narrow Line Region in Seyfert Galaxies Steven B. Kraemer1, H. Schmitt2, M. Crenshaw3, M. Melendez4, J. Turner5, M. Guainazzi6, R. Mushotzky7 1Catholic University of America, 2NRL, 3Georgia State University, 4Johns Hopkins University, 5UMBC, 6ESA, Spain, 7University of Maryland. Exhibit Hall We present a study of reddening and absorption towards the Narrow Line Regions (NLR) in active galactic nuclei (AGN) selected from the Revised Shapley-Ames, 12mu, and Swift/Burst Alert Telescope samples. For the sources in host galaxies with inclinations of b/a > 0.5, we find that mean ratio of [O III] 5007 and [O IV] 28.59mu, is more than a factor of 2 lower in Seyfert 2s than Seyfert 1s. The combination of low [O III]/[O IV] and low [O III] 4363/5007 ratios in Seyfert 2s suggests more extinction of emission from the inner NLR than in Seyfert 1s. Similar column densities of dusty gas can account for the suppression of both [O III] 5007 and [O III] 4363. Also, we find that the X-ray line O VII 22.1A is weaker in Seyfert 2s, consistent with absorption by the same gas that reddens the optical emission. If Seyfert 2 galaxies have similar intrinsic [O III] spatial profiles as Seyfert 1s, the external dusty gas must extend far out along the NLR and, perhaps in the form of nuclear dust spirals. 142.14 Determining AGN Feedback Parameters from Seyfert Galaxy Outflows D. Michael Crenshaw1, S. B. Kraemer2, H. R. Schmitt3, T. C. Fischer1 1Georgia State Univ., 2The Catholic University of America, 3Naval Research Laboratory. Exhibit Hall Mass outflows of ionized gas, detected through Hubble Space Telescope observations of blueshifted UV absorption lines and spatially-resolved emission lines, are common in nearby AGN. We review the constraints that these observations place on the structure of AGN winds, and provide estimates of the mass outflow rates and kinematic luminosities needed for AGN feedback models. 142.15 Double-Peaked Emission Lines in the Seyfert Galaxy Markarian 78: Mass Outflows from a Single AGN Travis C. Fischer1, D. M. Crenshaw1, S. B. Kraemer2, H. R. Schmitt3 1Georgia State University, 2The Catholic University of America, 3Naval Research Laboratory. Exhibit Hall We present a study of the outflowing ionized gas in the resolved narrow-line region (NLR) of Mrk 78 using observations from Space Telescope Imaging Spectrograph (STIS) and Faint Object Camera (FOC) aboard the Hubble Space Telescope (HST). We determine that the double set of emission lines seen in ground based observations are due to an asymmetric distribution of outflowing gas in the NLR. In successfully fitting a single AGN model to Mrk 78, we show that it is possible to explain double emission lines seen in radial velocity offsets of AGN similar to Mrk 78 without the requirement of dual supermassive black holes. 142.16 Quasars in the Extreme UV: Spectral Indices and Potential Emission Lines, and Implications for He II Reionization David Syphers1, S. Anderson2, W. Zheng3, A. Meiksin4 1University of Colorado, 2University of Washington, 3Johns Hopkins University, 4University of Edinburgh, United Kingdom. Exhibit Hall The extreme UV (EUV, <912 A) region of quasar spectra is poorly understood, because the high opacity of intervening hydrogen absorption systems makes it very difficult to observe. In the course of identifying a large number of new sightlines for the He II Gunn-Peterson test, we have amassed an unprecedentedly large collection of quasar spectra covering 250-500 A (rest frame). This allows us to examine emission lines in this largely unexplored region, as well as the average EUV spectral index. This continuum slope is poorly constrained, but vitally important for understanding the ionizing UV background in the IGM, as well as the progress of He II reionization. Our sample complements that of the few other EUV spectral index studies, which mostly extrapolate from longer wavelengths. Cloudy photoionization models of the broad emission line region (BELR) over a high-dimensional parameter space predict detectable He II Ly-alpha emission, with any other lines absent or very weak. Observationally, we find He II Ly-alpha is only rarely present, and sometimes other emission lines are present. We consider a number of possible explanations for weak He II Ly-alpha, including absorption from the IGM and absorption intrinsic to the quasar, and find that although no single explanation suffices, together they may. We find that BELR turbulence is an effective way of increasing the strength of metal lines relative to H and He, and may plausibly explain the presence of EUV metal lines. We offer a few, very tentative identifications of EUV metal lines seen in some spectra. Updates to ongoing HST He II studies will also be briefly described. We gratefully acknowledge NASA/STScI funding for HST program numbers 10907, 11215, 11982, and 12178. 142.17 Variable High Velocity Winds from Broad Absorption Line Quasars Kenza S. Arraki1, D. Haggard2, S. Anderson3, P. Green4, T. Aldcroft4 1New Mexico State University, 2Northwestern University, 3University of Washington, 4Harvard-Smithsonian Center for Astrophysics. Exhibit Hall We study broad absorption line quasars (BALQSOs) because these objects, in particular, probe the high velocity gas ejected by luminous accreting black holes. The variability timescales of BALs can help constrain the size, location, and dynamics of the emitting and absorbing gas near the supermassive black hole. We have obtained multi-epoch spectroscopy of seventeen BALQSOs from the Sloan Digital Sky Survey (SDSS) using the Fred Lawrence Whipple Observatory's 1.5m telescope's FAST Spectrograph. These objects were first identified as BALQSOs in SDSS, observed with Chandra, and then with FAST at 1, 3, 9, 27, and 81 day timescales. Additional observations are acquired for 1 and 2 year cadences. We also obtain a set of non-BAL quasar spectra of similar redshift and luminosity as controls. We identify significant variability and assess its magnitude and frequency in the observed spectra of our BAL QSOs and determine which constraints our investigations can put on the outflows impacting the BAL region. 142.18 The Western Radio Lobe of Fornax A: Nature of the X-ray Emission Electra Panagoulia1, P. Nulsen2, R. Kraft2, L. David2, W. Forman2, C. Jones2, B. McNamara3 1University of Southampton, United Kingdom, 2Harvard Smithsonian Center for Astrophysics, 3Waterloo University, Canada. Exhibit Hall An XMM-Newton observation of the western radio lobe of Fornax A has cast doubt on previous interpretations of the X-ray emission as inverse Compton scattered cosmic microwave background radiation. Imaging and spectroscopy both support a thermal origin for at least part of the detected X-ray emission. However, analysis of the XMM-Newton data is complicated by a significant level of background flaring. We will present a new analysis of the X-ray data, paying careful attention to removal of background. Implications of these results for the radio lobe and its group environment will be discussed. 142.19 Using Non-linear X-ray Variability to Explore the Core of Active Galaxy 3C 390.3 Sean Quinn1, K. Marshall2 1Rochester Institute of Technology, 2Bucknell University. Exhibit Hall Luminous variability of active galaxies is a universal phenomenon; however, there is no universally accepted causal mechanism. This study investigated variability of the broad line radio galaxy 3C 390.3. We concentrated on variability in the X-ray regime (2-10 keV), which is quite rapid-a consequence of the radiation source being proximal to the super massive black hole. Such variability can be explained by accretion disk models; however, there are numerous plausible but physically distinct models. We sought to isolate a particular accretion model which accurately describes the X-ray features for this galaxy. After performing a detailed time series analysis, with a focus on linearity tests, our results imply with high confidence that a non-linear multiplicative model is generating the variability. Given this criterion, we assert that the propagating viscosity fluctuation model is best suited for describing the observed X-ray behavior of this galaxy. This work was supported by the Bucknell University REU program which is funded by the National Science Foundation. 142.20 Fornax A's Western Radio Lobe Composition Jason J. Kong1, P. E. J. Nulsen2, R. P. Kraft2 1University of California at Berkeley, 2Harvard Smithsonian Astrophysical Observatory. Exhibit Hall We present an analysis of the western radio lobe of Fornax A based on an XMM-Newton observation. We find little evidence for the inverse-Compton scattering of the cosmic microwave background as reported previously. The spectra in the energy range of 0.5-5 keV are well fitted by a thermal plus power law model for every spectral region we extracted. With a fixed photon index of 1.68, the X-ray flux density at 1 keV from the power law fit was measured to be < 28 nJy at the 90% confidence level, leading to a lower limit on the magnetic field in this region of 6 micro-Gauss. Our spectral fits suggest that there is hot gas surrounding the radio lobe. A filament of dense, cool gas extends from the central galaxy in the direction of the radio lobe of Fornax A. Spectral fits give a temperature of kT=0.76 keV over the radio lobe and kT=0.32 keV for the cool filament. The thermal emission from the radio lobe region is best explained as emission from a thin shell of shocked gas swept up by the rapidly expanding lobe. This work is supported in part by the NSF REU and DOD ASSURE programs under NSF grant no. 0754568 and by the Smithsonian Institution. 142.21 Eclipses of the Inner Accretion Disk in NGC 1365 by Broad Line Region Clouds Laura Brenneman1, G. Risaliti1, M. Elvis1 1Harvard-Smithsonian Center for Astrophysics. Exhibit Hall We present new data obtained from a Suzaku AO5 Long Program observation of NGC 1365, a unique source that has in the past displayed both a prominent, relativistically broadened iron line and evidence for Compton-thin and Compton-thick eclipses of the inner disk region. These eclipse events allow us to constrain the structure and geometry of the inner disk and the intrinsic absorber(s) with unprecedented detail, and enable us to rule definitively on the emission vs. absorption origin of the putative broad iron line in this source. 142.22 Evidence Against the Unification of Quasars and Radio Galaxies from a New Sample of Luminous Radio Sources Todd A. Boroson1 1NOAO. Exhibit Hall A new sample of high-luminosity extragalactic (0.1 < z < 0.5) radio sources has been constructed using SDSS and three radio surveys: WENSS, NVSS, and FIRST. Initial matching of SDSS with WENSS (325 MHz), including the possibility of sources without radio cores, ensures that the sample is not contaminated by anisotropic radio core emission. This technique finds many more sources than existing catalogs based on SDSS matches with FIRST or NVSS. The resulting list comprises 86 objects in a complete sample having log luminosity density > 26.5 W/Hz at 325 MHz in the rest frame. An additional 26 objects are found that were targeted by SDSS as matches with FIRST or ROSAT sources. Optical properties (luminosities, spectral classification, emission line strengths) and radio properties (spectral index, source morphology, projected linear size) have been measured and tabulated. The distribution of projected linear sizes is particularly interesting; when divided into subsets with and without broad lines, the objects with broad lines (quasars) tend to have larger projected sizes at 1.4 GHz than those without broad lines (radio galaxies). The medians of the size distributions are 200 kpc for the radio galaxies (52 objects) and 350 kpc for the quasars (34 objects). This is different from the classic test by Barthel (1989) from which he argued that radio-loud quasars could be unified with radio galaxies by orientation. 142.23 Gamma-Ray Blazar Light Curves at 230 GHz from February 2009-November 2010 Ann E. Wehrle1, A. C. Zook2, M. A. Gurwell3, S. C. Unwin4 1Space Science Institute, 2Pomona College, 3Harvard-Smithsonian Center for Astrophysics, 4Jet Propulsion Laboratory/Caltech. Exhibit Hall We present 230 GHz continuum fluxes of blazars on the Fermi LAT Monitored Source List and of several blazars added after the Fermi LAT team reported flaring activity. Our science goal is to determine how and where relativistic charged particles emit synchrotron radiation and also act as scatterers of low energy photons (from jets, dust, the Broad Line Region and the hot corona) up to gamma ray energies. The data were obtained at approximately two-three week intervals at the Submillimeter Array, beginning in February 2009 and ending in November 2010. This program provides more evenly and frequently sampled data than the Submillimeter Array's ongoing flux density monitoring of quasars that are typically bright in the mm/submm bands, in order to optimally choose quasars for use as interferometric calibration sources (led by M. Gurwell (CfA); see http://sma1.sma.hawaii.edu/callist/callist.html/ ). The resulting light curves may be correlated with Fermi LAT photometry, Swift and RXTE observations, and related ground based monitoring programs. From the comparison, time delays between high and low levels at different bands can be derived. We can also compare the relative amplitudes at millimeter and gamma ray bands of flaring and quiescent levels. A. Wehrle acknowledges support from the NASA Space Interferometry Mission preparatory science program through JPL Subcontract 1283664 to the Space Science Institute. 142.24 Multi-Wavelength Variability of Fermi Selected Blazars Meghan Frate1, K. Marshall1, M. Aller2, H. Aller2, H. Miller3, J. Eggen3, D. Gudkova3, H. Marine3, J. Maune3 1Bucknell University, 2U. of Michigan, 3GSU. Exhibit Hall It is known that blazars are among the most variable and luminous objects in the sky due to their orientation relative to our line of sight. Our work has been to map the variability in four energy bands to search for correlations, in hopes of finding better relationships between the energy bands and supplementing existing multi-wavelength studies. We’ve done this with seven blazars monitored by the Fermi Gamma-ray Space Telescope and collected radio, optical, and X-ray data. We found strong correlation between optical and gamma-ray emissions in most of our objects, with X-rays generally uncorrelated with all other wavelengths, and were able to match these results up to existing emission models. 142.26 Vri/gri Photometry And Polarimetry Of Blazars At The Table Mountain Observatory, 2005-2010 Alma C. Zook1, M. M. Amezcua1, M. W. Hasling1, W. A. Morrison1 1Pomona College. Exhibit Hall We present VRI/gri photometry and polarimetry of several objects studied by the blazar monitoring program at Pomona College’s Table Mountain Observatory, which has now been operating for six summers. Initially only VRI photometric observations were possible; a polarimeter was added and tested during the summer of 2007 and a set of gri filters added in 2008. A total of sixteen blazars have been monitored during this time, most notably 3C279, 1510-089, 1611+343, 1652+398 (= Mrk 501), 1727+502, 3C 371, 1959+650, and 3C 454.3. The blazar 3C454.3 is particularly interesting, since it has undergone two outbursts during the monitoring period, in May 2005 and July 2007. 142.27 Investigating The AGN Population In Cluster Environments Across Different Wavelengths Eleanor Byler1, D. Norman2 1Wellesley College, 2NOAO. Exhibit Hall Currently, there is no complete picture of AGN formation and evolution in galaxy clusters. A general understanding of the AGN population has been impeded by cluster and selection biases and recent studies have shown that there is a large population of obscured or optically unremarkable AGN in galaxy clusters. We used SDSS data to look at the AGN distribution in 12 clusters over a range of redshifts (z = 0.16 - 0.35) and compared the optical and X-ray AGN content with that of six ‘blank’ fields. We found that on average the cluster fields had a small optical AGN excess as compared to blank fields. The AGN population and distribution was also compared by cluster morphology, and non-virialized clusters were found to have a higher X-ray and optical AGN content than virialized clusters. We also compare our optical AGN to Gilmour et al.’s (2009) X-ray survey to compare assumptions made about cluster membership. Byler was supported by the NOAO/KPNO Research Experiences for Undergraduates (REU) Program, which is funded by the National Science Foundation Research Experiences for Undergraduates Program and the Department of Defense ASSURE program through Scientific Program Order No. 13 (AST-0754223) of the Cooperative Agreement No. AST-0132798 between the Association of Universities for Research in Astronomy (AURA) and the NSF. 142.28 Unusual Swift-BAT Detected AGN James Hogg1, L. Winter1 1University of Colorado. Exhibit Hall The goals of our study were to analyze two odd AGN sources, NVSS 193013+341047 and IRAS 05218-1212, and determine if they were Compton-thick and low-redshift ERO analogs. The sources are strange because initial Swift XRT data lead us to believe the sources could be Compton-thick, typical of Seyfert 2 galaxies but they have broadlines in their optical spectra, typical of Seyfert 1 galaxies. These are two contradictory categorizations which made these sources very unique. In addition to the puzzling spectra, their SEDs are similar to the SED of a high redshift ERO and unlike things we typically see at their lower redshift. In order to study these sources further, we acquired and reduced higher quality XMM-Newton X-ray data. We then modeled the two spectra using XSPEC and learned that both sources had many complex components. From the higher quality data, we determined that they were heavily obscured, but not to the point of being considered Compton-thick. Both of the spectral fit models were heavily dependent on partial covering and reflection models. We found very high covering fractions and high column densities in both of our models, which was consistent with the galaxies being heavily obscured as we initially assumed. Further, we believe that future study of the sources as low-redshift ERO analogs can assist in better understanding of the early universe EROs we often see. If further study confirms the analogous relationship, these sources provide a great opportunity to add to our scientific knowledge about ERO evolution. 142.29 XMM Follow-Up Observations of Three Swift BAT-Selected Active Galactic Nuclei Margaret Trippe1, C. Reynolds1, M. Koss1, R. Mushotzky1, L. Winter2 1University of Maryland, 2University of Colorado. Exhibit Hall We present follow-up XMM observations of three AGN that were selected from the Swift BAT hard X-ray survey as candidate Compton-thick AGN: ESO 417-G006, IRAS 05218-1212, and MCG -01-05-047. The XMM spectra, however, rule out reflection-dominated models based on the weakness of the observed Fe K-alpha lines. Instead, the spectra are well-fit by a model of a powerlaw continuum obscured by a Compton-thin absorber, plus a soft excess. This result is consistent with previous follow-up observations of two other flat-spectrum BAT detected AGN. Thus, out of the six AGN in the 22-month BAT catalog with flat Swift XRT spectra, all five that have had follow-up observations are not likely Compton-thick. 142.30 Variability in Quasar Broad Absorption Line Outflows Daniel M. Capellupo1, F. Hamann1, J. C. Shields2, T. A. Barlow3, J. P. Halpern4, P. Rodriguez Hidalgo5 1University of Florida, 2Ohio University, 3California Institute of Technology, 4Columbia University, 5Pennsylvania State University. Exhibit Hall Broad absorption lines (BALs) in quasar spectra identify high velocity outflows that likely exist in all quasars and could play a major role in feedback to galaxy evolution. Studying the variability in these BALs can help us understand the structure, evolution, and basic physical properties of these outflows. We are conducting an ongoing BAL monitoring program that has produced over 160 spectra of 24 luminous quasars at z of 1.2-2.9, covering time-scales from 7 days to 7.7 years in the quasar rest-frame. We first investigate changes in the CIV 1550A BALs, and we see a variety of phenomena, including some absorption that either appeared or disappeared completely and other BALs that did not change at all over the whole observation period. The incidence of variability declines from 65% to 39% between the time domains of several years and a few months, and typically, only portions of the BAL troughs vary. We also compare the variability in the CIV 1550A BAL to the SiIV 1400A BAL to help distinguish between moving clouds and ionization changes as the cause of the variability. Using the multiple epochs of data from our program, we can characterize the variability over time in individual objects. Our most recent data covers the poorly sampled time domain of <1 month in the quasar rest-frame, which we can use to put constraints on the location of the outflowing gas. 142.31 Multi-frequency Optical-depth Maps And The Case For Free-free Absorption In Two Compact Symmetric Objects: 1321+410 And 0026+346 Thomas M. Perry1, J. M. Marr1, J. W. Read1, G. B. Taylor2 1Union College, 2University of New Mexico. Exhibit Hall We obtained VLBI observations at six frequencies of two Compact Symmetric Objects, 1321+410 and 0026+346. By comparing the lower frequency maps with spectral extrapolations of the higher frequency maps, we produced maps of the optical depth as a function of frequency. The optical-depth maps of 1321+410 are strikingly uniform, consistent with a foreground screen of absorbing gas; the optical depths as a function of frequency are consistent with free-free absorption; and no net polarization was detected. We conclude that the case for free-free absorption in 1321+410 is strong. The optical-depth maps of 0026+346 exhibit structure but the morphology does not correlate with that in the intensity maps, in conflict with that expected in the case of synchrotron self-absorption. No net polarization was detected. The frequency dependence of the optical depths does not fit well to a simple free-free absorption model, but this does not take into account possible structure in the absorbing gas on smaller scales. We conclude that free-free absorption by a thin amount of gas with structure on the scale of our maps and smaller is possible in 0026+346, although no definitive conclusion can be made. A compact feature between the lobes in 0026+346 has an inverted spectrum even at the highest frequencies, suggesting that this component is synchrotron self-absorbed. We infer this to be the location of the core. We estimate an upper limit to the magnetic field in the core of 50 Gauss at a radius of 1 pc. This research was supported by an award from the Research Corporation, a NASA NY Space Grant, and a Booth-Ferris Research Fellowship. The VLBA is operated by the National Radio Astronomy Observatory, a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. 142.32 Polarized Radio Source Counts and the Evolution of Galactic Magnetism Christopher A. Hales1, B. M. Gaensler2, R. P. Norris3, E. Middelberg4 1The University of Sydney / Australia Telescope National Facility, Australia, 2The University of Sydney, Australia, 3Australia Telescope National Facility, Australia, 4University of Bochum, Germany. Exhibit Hall Polarized radio source counts can address important unsolved problems in astrophysics such as the fundamental origin and subsequent evolution of large-scale coherent magnetic fields observed in galaxies, which remain poorly constrained by observational data. Here we present differential source counts of polarized radio galaxies using the Australia Telescope Compact Array, where we have imaged two 3.5 square degree fields at 1.4 GHz to a depth of ~20 microjanskys per beam in polarization. We discuss the nature of our faint polarized radio sources (which extend beyond z~2) using multiwavelength cross-identifications, and investigate the distribution of fractional polarization for our sources. Our polarized source counts can be used to place immediate constraints on evolutionary models of radio sources as well as the evolution of their magnetic fields with cosmic time. 142.33 A Stochastic Model for the Luminosity Fluctuations of Accreting Black Holes Brandon C. Kelly1, M. Sobolewska1, A. Siemiginowska1 1Harvard-Smithsonian Center for Astrophysics. Exhibit Hall I will present a new statistical model for the X-ray fluctuations of accreting black holes. The model is formulated in the time domain via a set of stochastic differential equations, and fitting the model is done in the time domain via a likelihood-based approach. Out technique is not biased by red noise leak, aliasing, irregular sampling, and measurement error, and is computationally efficient. We apply our model to the RXTE+XMM X-ray lightcurves of 10 local AGN and show that our model is both a good fit to the data, and is able to recover previous results with increased accuracy. We find a tight anti-correlation between the black hole mass and the amplitude of the driving noise field in our model, which is proportional to the amplitude of the high frequency X-ray PSD, and we estimate that this parameter gives black hole mass estimates to within ~ 0.2 dex precision. 142.34 Modeling the Distribution of Linear and Circular Polarization from AGN Jet Cores Christopher B. Wotta1, D. C. Homan1, M. L. Lister2 1Denison University, 2Purdue University. Exhibit Hall We present the results of full radiative transfer simulations of AGN jet cores to study the common physical properties of jets, such as their magnetic field structure and particle properties, that may be responsible for the observed distributions of polarization. To constrain these values we compare the results of our simulations to the first epoch MOJAVE observations of a complete, flux-density limited sample of AGN jets at 15 GHz. A key feature of the observational data is a lack of correlation between observed linear and circular polarization, and we found that this lack of correlation could be reproduced in our simulations if the circular polarization is produced stochastically, likely by Faraday conversion, in a magnetic field dominated by tangled components on a length scale of ~ 1/15 to 1/20 of a jet diameter. The tangled field components must also be shocked to explain the levels of observed linear polarization. We note that other possible explanations exist for the lack of observed correlation between linear and circular polarization, including un-resolved sub-structure and Faraday depolarization in external screens. This work has been supported by National Science Foundation grants AST-0707693 and AST-0807860. 142.35 Hydrodynamic Simulations of Double-Bent Radio Sources Jacob Miller1, B. Morsony1 1University of Wisconsin. Exhibit Hall Using three-dimensional hydrodynamic modeling, we simulate the development and evolution of Active Galactic Nuclei in galaxy groups in order to better understand the relationship between jet curvature and various properties of the Intergalactic Medium and of the AGN itself, with an emphasis on the use of radius of curvature as a density probe of the IGM. 142.36 Hubble/COS Observations of AGN Ionizing Continua Matthew L. Stevans1, J. M. Shull1, C. W. Danforth1 1University of Colorado - Boulder. Exhibit Hall The high-throughput Cosmic Origins Spectrograph (COS) installed on the Hubble Space Telescope (HST) allows us to obtain high-quality UV spectra of active galactic nuclei (AGN), many of which served as background targets for studies of the low-redshift intergalactic medium (IGM). We present power-law continuum fits for a sample of 13 AGN with redshifts 0.0296 < z < 0.852, sufficient to explore their far ultraviolet (FUV) and extreme ultraviolet (EUV) continua. New spectra from HST/COS provide spectral coverage in the rest-frame Lyman continuum of AGN at z > 0.24, with high sensitivity and moderate resolution (20 km/s) in the G130M grating. This allows broad emission lines (Ne VIII, O IV) to be resolved. In cases when Far Ultraviolet Spectroscopic Explorer (FUSE) and International Ultraviolet Explorer (IUE) data are available, we create and fit composite spectra covering between 900 - 3300 Å; in the observed frame. We compare COS-based power-law spectra to these data. Describing the EUV continuum fluxes by a power-law spectrum, F? = A ?? with index ?, gives insight into the formation of emission lines, defines the "big blue bump" in the spectral energy distribution of AGNs, and constrains the ionization state of the IGM. We examine our results for correlations of spectral slope with redshift and compare our results to previous spectral fits from HST/FOS (Telfer et al. 2002, ApJ, 565, 773) and FUSE (Scott et al. 2004, ApJ, 615, 135). This work is supported by the COS-support grant from the STScI (NNX08-AC14G).   142.37 Multi-wavelength Monitoring of 6 Gamma-ray Blazars at Maria Mitchell and Other Observatories Stephanie Sallum1, S. G. Jorstad2, A. P. Marscher2, G. Walker3, V. Strelnitski3, V. M. Larionov4 1MIT & Maria Mitchell Obs., 2Boston U., 3Maria Mitchell Obs., 4St. Petersburg U., Russian Federation. Exhibit Hall We have observed 6 gamma-ray bright blazars in the B and R bands (and V and I bands for some sources) using the Maria Mitchell Observatory 17” Dall-Kirkham and 24” Ritchey-Chretien reflectors during 2010. In all of the blazars, we have detected variability on a timescale of days to weeks; in OT+081, a dramatic outburst occurred in August 2010 when the flux at R band increased by 3.5 magnitudes. We supplement our optical R band observations with data taken at other telescopes, including RXTE, Swift, and public data from the Fermi Gamma-Ray Space Telescope’s Large Area Telescope. This allows us to form the spectral energy distribution (SED) of each blazar. We further support our dataset by comparing our multi wavelength light curves with 43 GHz VLBA images of the radio jets at 43 GHz for all of the objects. We discuss the connection between variations in the optical bands and at other frequencies, as well as the physical constraints that time delays and SEDs impose on the high-energy emission mechanism. The research at Boston U. was supported by NSF grant AST-0907893 and NASA grant NNX08AV65G (Fermi). The research at Maria Mitchell Obs. was supported by the NSF/REU grant AST-0851892 and by the Nantucket Maria Mitchell Association. 142.38 A Spitzer Survey of Hot Spots in Radio Lobes Michael W. Werner1, V. Gorjian1, J. Livingston1, D. Jones1, D. Murphy1, D. Meier1, C. Lawrence1, A. Readhead2 1JPL/Caltech, 2Caltech. Exhibit Hall We present the results of a survey at infrared wavelengths of the emission from hotspots in the lobes and jets of energetic radio sources. Our sample is chosen from the work of Hardcastle et al (2004), who analyze x-ray and radio data on a number of hot spots. For nine hot spots we used infrared data from the Spitzer archive - generally in all four IRAC bands - while for another 17 we carried out new observations with Warm Spitzer in the IRAC band at 3.6um. For 17 hotspots, 7 archival and 10 from the warm mission, we have infrared detection(s) and present an x-ray/infrared/radio SED, often with additional optical data also presented by Hardcastle et al. For another 9 hotspots (2 archival and 7 newly observed) we have only upper limits from the Spitzer observations to go with the x-ray and radio detections. We compare the multiwavelength SEDs with the predictions of synchrotron self Compton and pure synchrotron models for the hotspots. This research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration 142.39 Optical Analysis Of A Binary Black Hole's Host Galaxy 0402+379 Steffanie Peterson1, R. Zavala2 1Northern Arizona University, 2United States Naval Observatory Flagstaff Station. Exhibit Hall We present results from optical data analysis of the active galactic nucleus (AGN) host galaxy 0402+379. This AGN hosts two binary black holes, which have a projected separation of only 7.3 parsecs. This separation is two times closer than any other known system. The data were taken with WIYN in December 2008 in broadband filters g, r and i as well as in narrowband filters W13, W25, W26 and K814. We analyze the narrowband data to find regions of H?, NII and SII emission, indicating star forming regions. We determine the stellar age distribution within the host galaxy from the g/r/i colors. We conclude that the morphology of the host galaxy is elliptical using De Vaucouleurs' Law with our calculated surface brightness. We use this morphological information to estimate the relative date of the merger to be approximately 2 Gyr ago. We also conclude that a third galaxy is interacting with the host galaxy, which may provide a means of reducing the system's angular momentum and facilitating coalescence. 142.40 WFC3 Imaging Of z=6 QSO Hosts: A Method For PSF Characterization And Subtraction Matt Mechtley1, R. A. Windhorst1, G. Schneider2, S. H. Cohen1, X. Fan2, N. P. Hathi3, W. C. Keel4, A. Koekemoer5, H. Rottgering6, R. E. Ryan7, D. P. Schneider8, M. A. Strauss9, H. Yan10 1Arizona State University, 2University of Arizona, 3Carnegie Observatories, 4University of Alabama, 5Space Telescope Science Institute, 6University of Leiden, Netherlands, 7University of California, Davis, 8Pennsylvania State University, 9Princeton University, 10The Ohio State University. Exhibit Hall We present an observation and analysis plan for using the Wide Field Camera 3 IR Channel on the Hubble Space Telescope to carefully characterize and subtract the central point source from a redshift 6 QSO, in an attempt to image and conduct photometry on the underlying host galaxy. We discuss parameters affecting measurement of the instrument point spread function (PSF), including thermally-induced secondary mirror de-focus ("spacecraft breathing"), object spectral slope, and IR channel image persistence. We describe in detail our plan to address these effects or measure them on-orbit, and the criteria used to select the star with which we will make these PSF measurements. We also present our data analysis strategy, including models of breathing-induced PSF variation, and point source subtraction in simulated images. Depending upon the HST cycle 18 observation schedule, we will also discuss preliminary results if our first set of data is available. Support for HST GO program #12332 is provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. 142.41 Radio Band Linear Polarization as a Probe of the Origin of Gamma-Ray Emission from Blazars Margo F. Aller1, P. A. Hughes1, H. D. Aller1 1Univ. of Michigan. Exhibit Hall To test the hypothesis that shocks play a role in the production of the gamma-ray flares detected by Fermi and to identify jet conditions during gamma-ray flares, we are intensively monitoring the linear polarization and total flux density of a core group of about two dozen radio-and-gamma-ray-bright AGN with the University of Michigan radio telescope to look for the expected shock signature: an increase in the degree of linear polarization and an ordered swing in electric vector position angle. We have observed increases in fractional linear polarization of order ten degrees and swings in electric vector position angle of order tens of degrees in several sources during gamma-ray flares. We present centimeter-band light curves for OJ287, PKS 1510-089, and OT 081 illustrating this signature and compare the spectral evolution apparent in the light curves with simulations from new radiative transfer calculations allowing for the propagation of shocks in the relativistic jet outflows at any orientation to the flow direction. These simulations are able to reproduce the primary features of the observed light curves.This research was supported by NASA Fermi grants NNX09AU16G and NNX10AP16G, NSF grant AST-0607523, and by the University of Michigan. 142.42 AGN Inner Structure with NuSTAR Martin Elvis1, L. Brenneman1, M. Young2, F. Civano1, G. Risaliti1, D. Stern3, F. Harrison3, NuSTAR Team 1Harvard-Smithsonian CfA, 2Penn State University, 3California Institute of Technology. Exhibit Hall The inner structure of AGNs has a standard model, but the model is poorly tested. The model is that of an accretion disk surrounded by a hot corona. The disk produces the primary optical and UV emission, the corona upscatters these photons to X-rays, and a fraction of those X-rays are re-processed in the disk, which fluoresces to produce the Compton Hump (E>10keV) and an Fe-K emission line that is broadened by disk rotation and general relativity. Since few corona temperatures have been measaured, we cannot separate the Compton y-parameter into its temperature (kt) and optical depth (Tau) components. As we lack high signal-to-noise >10keV spectra the parameters of the red wing to the 6.4keV Fe-K line are poorly determined in all but a few cases, limiting our knowledge of the disk inner radius and black hole spin - or our ability to test alternative, e.g. multi-Nh screens. NuSTAR will provide the first high S/N spectra of AGNs above 10keV. We present detailed simulations that demonstrate that the kT-Tau degeneracy can be very cleanly broken. In conjunction with Suzaku or XMM-Newton spectra we show that the red wing Fe-K profile can be exquisitely determined, giving the black hole spin parameter with small uncertainties. We also show that NuSTAR can span wide ranges of black hole mass and Eddington ratio with a reasonable observing program. 142.43 Determination of the Infrared Luminosity of Active Galactic Nuclei (AGN) Varoujan Gorjian1, K. Meredith2, H. Petach2, E. Ramseyer2, T. Spuck2, M. Abajian3, NITARP Luminous Data Miners Team 1JPL, 2NITARP, 3NITARP/IPAC. Exhibit Hall Using archival data from the Spitzer and GALEX Space Telescopes we have plotted a UV-IR color-magnitude diagram for AGN. The previous difficulty in determining the IR luminosity of AGN using this technique has been that AGN have varying levels of obscuration in the UV, also they are variable and previous observations were often taken at widely differing times. As a result, color-magnitude diagrams sometimes had UV and IR data points acquired decades apart. These issues were mitigated in this study i) by using data that were collected much closer in time to each other, since both telescopes were launched and carried out most of their observations within the same 5 year period and ii) by choosing Type I AGN, which show the least amount of obscuration. 142.44 Observations Of Gamma-ray Loud Blazars With The VLBA At 5 GHz Justin Linford1, G. B. Taylor1, R. Romani2, A. C. S. Readhead3, R. Reeves3, J. L. Richards3, J. F. Helmboldt4 1University of New Mexico, 2Stanford University, 3California Institute of Technology, 4Naval Research Laboratory. Exhibit Hall The Fermi Gamma-ray Space Telescope has been scanning the sky for more than a year. About half of the sources detected by Fermi’s Large Area Telesope (LAT) are active galactic nuclei (AGN). Nearly all of these gamma-ray loud AGN are blazars; strong, compact radio emitters that exhibit variability in their flux and apparent superluminal motion in their jets. Several groups are currently monitoring the radio properties of these gamma-ray loud blazars. We present results from both archival and contemporaneous observations of ~200 LAT-detected blazars using the Very Long Baseline Array (VLBA) at a frequency of 5 GHz (wavelength of 6 cm). Our large, flux-limited sample provides unique insights into the mechanism that produces strong gamma-ray emissions. We explore the parsec-scale properties of the cores and jets of these highly energetic objects, including core polarization. We compare the gamma-ray loud blazars to their gamma-ray quiet counterparts in the VLBA Imaging and Polarimetry Survey (VIPS). We also investigate the differences between the BL Lacertae objects (BL Lacs) and flat-spectrum radio quasars (FSRQs). 142.45 Emission Line Properties of a Low-Redshift Quasar Sample Amanda Truitt1, K. M. Leighly1 1University of Oklahoma. Exhibit Hall We report the results of analysis of a sample of 81 low-redshift quasar spectra drawn principally from the Sloan Digital Sky Survey. The spectra were chosen to have sufficiently narrow lines that the FeII multiplets can be discerned, and to be minimally contaminated by galaxy emission. We fit the spectra uniformly with a model consisting of a power law, FeII templates, and Balmer lines, and we include [OIII] even when we cannot identify the line in the spectrum by eye. We confirm some previously known correlations, and find some new ones. We confirm a strong correlation between H? FWHM and monochromatic luminosity at 5500 Angstroms, but we also find a strong correlation between [OIII] FWHM and luminosity. We confirm a correlation between [OIII] blueshift and [OIII] FWHM, but we extend that correlation to larger blueshifts (up to ~900 km/s) and larger velocity widths (up to >2000 km/s). This result is a consequence of our model fitting approach, and we note that the [OIII] component is generally statistically significant in the fit. We also confirm a strong correlation between power law slope and luminosity. We investigate the properties of the Balmer lines in this sample using a Boltzmann plot approach. While the Balmer lines may not be emitted by thermal gas, we find that the temperature inferred is related to the Balmer line properties because objects with high temperatures exhibit Balmer continuum while objects with low temperatures do not. The derived temperature is weakly anticorrelated with luminosity and associated parameters, but there are no strong correlations with other parameters. Additional analysis and results will be discussed. This research is funded by NSF AST-0707703. 142.46 Kinematic Signatures of Seyfert AGN Fueling on Scales from 1 kpc to 10 pc Erin K. Hicks1, R. I. Davies2, E. Emsellem3, W. Maciejewski4, M. A. Malkan5, T. Quinn1 1University of Washington, 2Max Planck Institute, Germany, 3ESO, Germany, 4Liverpool John Moores University, United Kingdom, 5University of California, Los Angeles. Exhibit Hall Aiming to constrain the dynamical processes that dictate black hole accretion rates in Seyfert galaxies, we have begun a program in which we simultaneously probe the stellar and molecular gas kinematics from 1 kpc down to ~10 pc in matched samples of Seyfert and quiescent galaxies. Using adaptive optics-assisted integral field K-band spectroscopy we identify differences in these samples including gas content within the central ~100 pc, prevalence of thick nuclear gas disks, significance of non-circular motions, frequency of central stellar dispersion drops indicative of past inflow of the interstellar medium, and characteristics of the nuclear star formation (rates and age of last episode). Preliminary results will also be presented from an ongoing effort to interpret the non-circular kinematic signatures observed in the molecular gas via theoretical dynamical models, which will enable us to determine the primary mechanisms responsible for Seyfert AGN fueling and assess their potential impact on galaxy evolution. 142.47 Time-Variability of the Circular Polarization From Active Galactic Nuclei At Multiple Frequencies Hugh D. Aller1, M. Aller1 1Univ. of Michigan. Exhibit Hall We have monitored a group of bright AGN at 14.5, 8.0 and 4.8 GHz with the University of Michigan 26-meter telescope to better define the variability of these active sources in Stokes V. The stability in the sign of the circular polarization has implications for the mechanism believed to be responsible for the emission: specifically tests of the proposed links between the Black Hole - accretion disk and the radio jet. The only source in which we find a stable sign over many years at all three frequencies is OV-236. This polarity is maintained throughout several outbursts in both linear and circular polarization. In other sources we typically find evidence for a preferred polarity for an extended period intermixed with well-defined flips in sign for durations of months to a few years. A good example of this behavior is exhibited by 3C 279. In several sources we also observe differences in polarity between the three frequencies at a single epoch. This work is supported by NSF grant AST-0607523. 142.48 SPH Simulations of Spherical Bondi Accretion: First Step of Implementing AGN Feedback in Galaxy Formation Paramita Barai1, D. Proga1, K. Nagamine1 1University of Nevada, Las Vegas. Exhibit Hall Our motivation is to numerically test the assumption of Black Hole (BH) accretion (that the central massive BH of a galaxy accretes mass at the Bondi-Hoyle accretion rate, with ad-hoc choice of parameters), made in many previous galaxy formation studies including AGN feedback. We perform simulations of a spherical distribution of gas, within the radius range 0.1 - 200 pc, accreting onto a central supermassive black hole (the Bondi problem), using the 3D Smoothed Particle Hydrodynamics code Gadget. In our simulations we study the radial distribution of various gas properties (density, velocity, temperature, Mach number). We compute the central mass inflow rate at the inner boundary (0.1 pc), and investigate how different gas properties (initial density and velocity profiles) and computational parameters (simulation outer boundary, particle number) affect the central inflow. Radiative processes (namely heating by a central X-ray corona and gas cooling) have been included in our simulations. We study the thermal history of accreting gas, and identify the contribution of radiative and adiabatic terms in shaping the gas properties. We find that the current implementation of artificial viscosity in the Gadget code causes unwanted extra heating near the inner radius. 142.49 Comparing The Temporal Evolution Of NIR And Fermi/LAT Observations Of Blazars Ori D. Fox1, A. S. Kutyrev2, J. T. Bonnell2, J. P. Norris3, C. R. Klein4, J. S. Bloom5 1NASA/GSFC/ORAU, 2NASA Goddard Space Flight Center, 3University of Denver, 4University of California, 5University of California, Berkeley. Exhibit Hall Over the past year, the Wyoming Infrared Observatory (WIRO) near-infrared (NIR) camera observed 50 blazars with known flaring states out to a redshift z=2. Data were obtained in conjunction with previously scheduled Fermi/LAT observations over daily, weekly, and monthly time-scales. The Peters Automated Infraed Imaging Telescope (PAIRITEL) provided additional NIR observations. Here, we present a comparison of the fluxes and search for a correlation, or lack thereof, between the different wavelengths. We expect these results to have an impact on our understanding of the relationship between the temporal-spectral behavior of blazar physical states and the black hole evolutionary time scale. 142.50 Seeing Through the Clouds: AGN Geometry with the Swift BAT Sample Eilat Glikman1, M. Urry1, K. Schawinski1, M. J. Koss2, L. M. Winter3, M. Elitzur4, W. H. Wilkin1 1Yale University, 2University of Maryland, 3University of Colorado, 4University of Kentucky. Exhibit Hall We investigate the intrinsic structure of the clouds surrounding AGN which give rise to their X-ray and optical emission properties. Using a complete sample of Swift BAT AGN selected in hard X-rays (14-195 keV), which is unbiased with respect to obscuration and extinction, we compute the reddening in the broad line region along the line of sight to the nucleus of each source using Balmer decrement from the ratio of the broad components of H-alpha/H-beta. We compare reddening from dust in the broad line clouds to the hydrogen column density (NH) obtained from their X-ray spectra. The distribution of the gas-to-dust ratios over many lines of sight allow us to test models of AGN structure and probe the immediate environment of the accreting supermassive black holes. 142.51 Expanding a Monte Carlo Radiation Transfer Scheme to include Anisotropic Magnetic Fields and Bulk Velocities, and Applications to AGN's Guy L. Hilburn1, E. Liang1 1Rice University. Exhibit Hall To extend its usefulness to applications for AGN's, astrophysical jets, and other myriad sources, our Monte Carlo radiation transport has been modified in several important ways. Previously, magnetic fields were considered as having no angle dependence or "structure". Changes have made it possible to consider fields which point in any direction in each simulation cell, which will be vital for properly modelling AGN's, whose fields are strongly anisotropic. Similarly, other modifications have added the capability of treating the simulation plasma as having macroscopic flow. That is, the emission, scattering, and transport of photons in the volume is now dependent on the bulk motion of the plasma. This will be especially important when simulating jets, where speeds may be a considerable fraction of the speed of light. 142.52 Indecent Exposure in Seyfert 2 Galaxies: A Deeper Look Hien D. Tran1 1W.M. Keck Observatory. Exhibit Hall NGC 3147, NGC 4698 and 1ES 1927+654 are three Seyfert 2 galaxies with an unusual combination of properties: X-ray spectra show variability and little absorption indicative of a type-1 (direct) view, but optical spectra show only narrow emission lines, typical of a type-2 (obscured) view of the nucleus. A deep search for hidden broad-line regions (BLR) using Keck LRIS spectropolarimetry and direct near-IR spectroscopy with NIRSPEC does not reveal any broad emission lines, hidden or direct. If typical broad lines were present, the BLR non-detections would indicate an extinction of ~ 11 - 26 mag, inconsistent with their ``naked'' nature. While the obscuration may be due to different material for X-ray and optical light, it appears that the BLRs in these objects are anemically small or nonexistent, due to the weakness of their active central engines. 142.53 Relativistic Hotspots in FR II Radio Sources Alex M. Chartrand1, B. P. Miller2, W. N. Brandt3, M. P. Gawronski4, S. E. Cederbloom1 1University of Mount Union, 2University of Michigan, 3Pennsylvania State University, 4Nicolaus Copernicus University, Poland. Exhibit Hall We present a list of six FR II radio sources that are candidates to possess hotspots with modestly relativistic (v/c > 0.2) bulk velocities, in contrast to the vast majority of FR II radio sources that possess non-relativistic hotspot bulk velocities (e.g., v/c = 0.03+/- 0.02 from Scheuer 1995). These objects display arm- length and flux-ratio asymmetries between lobes that self-consistently indicate relativistic motion. The candidates are selected from the FIRST 1.4 GHz survey (including but not limited to the catalog of FR II quasars of de Vries et al. 2006) with the requirement that the radio core have a spectroscopic SDSS counterpart. We find no significant difference in the number of neighboring sources within 300 projected kpc of the candidate sources and randomly selected nearby regions. The deprojected and light travel-time corrected lobe distances are not abnormal for FR II sources, and neither are the core-to-lobe flux ratios after correcting for lobe beaming. We briefly consider four possibilities for these type of objects: (i) environmental interactions randomly mimicking relativistic effects, (ii) a restarted jet causing the near hotspot to brighten while the far hotspot still appears faint, (iii) observation during a short interval common to FR II lifetimes during which the hotspot decelerates from relativistic to non-relativistic velocities, and (iv) innately unusual characteristics (e.g., a mass-loaded jet) driving relativistic bulk velocities in the hotspots of a small fraction (< 1%) of FR II objects. We favor the last interpretation but cannot rule out the alternatives. We also comment on the useful external constraints such objects provide to the evaluation of hotspot X-ray emission mechanisms. 142.54 Broad Absorption Line Variability in Radio-Loud Quasars Christine Welling1, B. P. Miller2, W. N. Brandt3, R. R. Gibson4, M. C. Eracleous3, K. T. Lewis5 1Dickinson College, 2University of Michigan, 3Pennsylvania State University, 4University of Washington, 5College of Wooster. Exhibit Hall We investigate broad absorption line (BAL) variability within a sample of 20 radio-loud quasars (RLQs) using Sloan Digital Sky Survey (SDSS) spectra along with new Hobby-Eberly Telescope (HET) observations. By comparison to BAL variability in radio-quiet quasars (RQQs), we aim to assess whether BAL outflows in RLQs have a similar physical origin to those in RQQs. The BAL RLQs were selected from SDSS/FIRST data and include both core-dominated (17) and lobe-dominated (3) objects; their radio luminosities and radio-loudness values span 2.5 and 3 orders of magnitude, respectively, and a substantial fraction have large BAL velocities (8/20 exceed 10000 km/s) and equivalent widths (6/20 exceed rest-frame 4000 km/s). Only modest BAL variability is detected on rest-frame timescales of 300-1000 days: the median fractional change in equivalent width is 0.07, exceeds 0.2 for only 3/20 objects, and in no cases is greater than 0.30. We do not find any correlation between the fractional change in equivalent width and radio luminosity. There is a possible tendency for lobe-dominated objects to display greater variability, but a larger sample is required for confirmation. Comparison to variability in BAL RQQs does not reveal significant differences in the distribution of fractional change in equivalent width. This suggests that the mechanism of BAL production within this sample of RLQs may be similar to that of the comparison BAL RQQs. We extend this comparison to shorter timescales (30-300 rest-frame days) through the additional inclusion of BAL RLQs with multiple SDSS spectra, and discuss the results. Additional coverage at longer timescales would be helpful to investigate whether the variability amplitude increases for BAL RLQs, as it apparently does for BAL RQQs. 142.55 Multiwavelength Study of Gamma-Ray Bright Blazars Daria Morozova1, V. M. Larionov1, V. A. Hagen-Thorn1, S. G. Jorstad2, A. P. Marscher2, I. S. Troitskii1 1St.Petersburg State Univ., Russian Federation, 2IAR, Boston Univ.. Exhibit Hall We investigate total intensity radio images of 6 gamma-ray bright blazars (BL Lac, 3C 279, 3C 273, W Com, PKS 1510-089, and 3C 66A) and their optical and gamma-ray light curves to study connections between gamma-ray and optical brightness variations and changes in the parsec-scale radio structure. We use high-resolution maps obtained by the BU group at 43 GHz with the VLBA, optical light curves constructed by the St.Petersburg State U. (Russia) team using measurements with the 0.4 m telescope of St.Petersburg State U. (LX200) and the 0.7 m telescope of the Crimean Astrophysical Observatory (AZT-8), and gamma-ray light curves, which we have constructed with data provided by the Fermi Large Area Telescope. Over the period from August 2008 to November 2009, superluminal motion is found in all 6 objects with apparent speed ranging from 2c to 40c. The blazars with faster apparent speeds, 3C 273, 3C 279, PKS 1510-089, and 3C 66A, exhibit stronger variability of the gamma-ray emission. There is a tendency for sources with sharply peaked gamma-ray flares to have faster jet speed than sources with gamma-ray light curves with no sharp peaks. Gamma-ray light curves with sharply peaked gamma-ray flares possess a stronger gamma-ray/optical correlations. The research at St.Petersburg State U. was funded by the Minister of Education and Science of the Russian Federation (state contract N#P123). The research at BU was funded in part by NASA Fermi Guest Investigator grant NNX08AV65G and by NSF grant AST-0907893. The VLBA is an instrument of the National Radio Astronomy Observatory, a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. 142.56 Starburst and AGN Indicators in Optically Faint X-ray Sources in the Cosmic Evolution Survey Derek Robins1, M. Elvis2, F. Civano2 1Harvard College, 2Harvard-Smithsonian Center for Astrophysics. Exhibit Hall A sample of 55 faint, X-ray selected objects were chosen for analysis from the COSMOS survey with high quality Keck DEIMOS data. The average redshift of the sample was 1.36, consistent with the average redshift of type 1 AGN in COSMOS of 1.4. Emission lines, NeV - an indicator of AGN luminosity - and OII - an indicator of star formation rate, were measured for a subset of 34 objects. Line properties for these objects were measured. The combination of the two lines is evidence for significant star formation in these obscured AGN. Differences between OII and NeV redshifts were measured carefully. Significant differences between OII and NeV redshifts were found in 10-14 objects, implying OII outflows. The results are consistent with current models of galaxy evolution that invoke an interplay between AGN activity and star formation. 142.57 VLBI Images of Water Maser Galaxies Caterina Impellizzeri1, J. Braatz1, C. Kuo1, J. Condon1, C. Henkel2, M. Reid3, F. Lo1 1NRAO, 2MPIfR, Germany, 3CfA. Exhibit Hall The goal of the Megamaser Cosmology Project (MCP) is to determine a precise value of the Hubble Constant by measuring angular diameter distances to galaxies in the Hubble flow using the megamaser technique. We search for new megamasers and monitor the most promising ones with the Green Bank Telescope. The best candidates are then followed up with high-resolution VLBI observations to map the maser distribution. These observations provide direct geometrical distances to the galaxies, precise black-hole masses, and offer the opportunity to study their physical properties on sub-parsec scales. We present here an atlas of all VLBI maps of megamaser galaxies observed to date by the MCP. The maser distribution in these galaxies is consistent with emission from edge-on accretion disks in the AGN. The variety of properties gives insight into the different physical conditions associated with accretion onto a black hole, and we discuss those implications here. 142.58 Double-peaked Narrow Emission Lines In AGN: Jets, Spins Or Twins? Krista Smith1, G. A. Shields1, S. Salviander1, D. J. Rosario2 1University of Texas at Austin, 2Max Planck Inst., Germany. Exhibit Hall AGN with double-peaked narrow lines have attracted recent attention as candidates for binary AGN in galaxy mergers. However, double-peaked lines can also result from bipolar jets or rotating disks. We examine tests of these possibilities involving the properties of the emission lines. Indicators based on the velocity separation of the components suggest that objects with equal intensity peaks may be rotating disks. 142.59 Properties Of Seyfert 2 Galaxies: Divergence From Unified Model? Kazuyuki Tamura1, H. Kim1, M. J. Rutkowski1, R. A. Windhorst1 1Arizona State Univ.. Exhibit Hall At the nucleus of the Seyfert galaxies, broad-line region (BLR) is surrounded by the dust torus. According to the unified model of active galactic nucleus (AGN), different types of Seyfert galaxies are classified based on viewing angle of the AGN: signature of BLR is missing in Seyfert 2s due to obscuration by dust torus. However, recent studies find some differences between the properties of the two types of Seyferts that are inconsistent with simple unified model. Simulations show that BLR features can also disappear at very low accretion rates onto the central black hole. Such low accretion rates may be accompanied by declining star formation rates in the host galaxy. We investigated this possibility through a multi-wavelength study of 44 nearby Seyfert galaxies selected from the Palomar spectral survey, using data/images observed by Chandra, GALEX, XMM-Optical Monitor (XMM-OM), HST, 2MASS, and Spitzer (IRAC and MIPS). We compare the global star formation rates measured from the near ultraviolet (GALEX and/or XMM-OM) and Spitzer 24 micron images, and quantify the galaxies' structure in each band using variety of methods such as 2-D decomposition, CAS (Concentration, Asymmetry, and Clumpiness) and Gini parameters. Correlations between these different parameters, including the nuclear accretion rates, therefore, reveal whether Seyfert 2 galaxies are the results of the viewing angle (following unified model) of AGN, or whether some Seyfert 2 galaxies have mechanically different properties from the others. Funding for this project is provided through NASA/ADP grant NNX10AD77G. 142.60 Observations of Markarian 421 with the WIYN Telescope for a Multiwavelength Blazar Campaign David F. Fierroz1, T. Montaruli2 1Columbia University, 2University of Wisconsin-Madison. Exhibit Hall This is a report on the recent work of a long term multimessenger and multiwavelength campaign on blazars. We show how we have set up the tools to analyze the data of the WIYN 0.9m optical telescope during two periods in 2008-2009 and 2009-2010. We present the optical data we collected here as well as a preliminary correlation study. We are mostly interested in the variability in time of the optical emission in order to correlate to other wavelengths. The Whipple public data for the same periods are shown as an example of correlation studies in the TeV band and in the optical. This work was supported by the National Science Foundation's REU program through NSF Award AST-1004881 142.61 A New Analytical Model for Trans-Relativistic Particle Acceleration Peter A. Becker1 1George Mason University. Exhibit Hall Most existing analytical models describing the second-order Fermi acceleration of relativistic particles due to collisions with MHD waves assume that the injected seed particles are already highly relativistic, despite the fact that the most prevalent source of particles is usually the local thermal background, which is typically a non-relativistic gas. This presents a problem because the momentum dependence of the momentum diffusion coefficient describing the interaction between the particles and the MHD waves is qualitatively different in the non-relativistic and highly relativistic limits. Since the existing analytical models are not able to address this situation, workers have had to rely on numerical simulations to obtain particle spectra describing the trans-relativistic case. In this work we present the first analytical solution to the global, trans-relativistic problem, obtained by using a hybrid form for the momentum diffusion coefficient, given by the sum of the two asymptotic forms. The model also incorporates the appropriate momentum dependence for the particle escape timescale, and the effect of synchrotron and inverse-Compton losses, which are critical for establishing the location of the high-energy cutoff in the particle spectrum. The results can be used to model the acceleration of particles in AGN and solar environments, and can also be used to compute the spectra of the associated synchrotron and inverse-Compton emission. Applications of both types are discussed. 142.62 Analysis of GALFACTS Data for the Study of Variable Radio Sources Scott Barenfeld1, T. Ghosh2, C. Salter2 1NAIC/University of Rochester, 2NAIC. Exhibit Hall The G-ALFA Continuum Transit Survey (GALFACTS) is a spectro-polarimetric survey of Arecibo Observatory’s visible sky from 1225-1525 MHz, using the Arecibo L-band Feed Array (ALFA). Among the survey’s many scientific goals is a large-scale statistical study on the short-term variability of the flux density and polarization of radio sources. Every point in the sky is observed twice, with less than a month between observations, making this the largest systematic search for variability ever conducted. In this poster, we present the development of computer code to aid in this search, and some preliminary results from this code. The code takes GALFACTS data in the form of time series for 2048 individual spectral channels, containing positions and full-stokes antenna temperatures, and turns these into a list of individual radio sources with their positions and Stokes-I temperatures. We first ran the code for the field surrounding the radio source S0206+330, of known flux density, as a test. Once a working code was completed, it was run on the field of another radio source, S0311+307. 142.63 A Difference-Imaging Survey for AGN in Stripe 82 Yumi Choi1, R. R. Gibson1, A. Becker1, Z. Ivezic1, A. J. Connolly1 1University of Washington. Exhibit Hall With upcoming surveys such as LSST poised to generate a deep movie of the optical/UV sky, variability-based selection promises to generate highly-complete AGN catalogs while minimizing contamination. To prepare for large time-domain surveys, photometric analyses are currently focusing on SDSS Stripe 82 because it covers a large area of sky (about 300 square degrees) with ~70 epochs of observations in each of five (ugriz) filters. We are exploring an alternate approach to variability-based selection in Stripe 82 data, using difference-imaging code developed for the LSST survey. Difference imaging analyses do not need to assume or fit a source model, so they excel at identifying variable sources embedded in complex or blended emission regions. Our initial goal in this project is to identify AGN that are surrounded by host-galaxy emission, including lower-luminosity AGN that may be omitted from photometric or spectroscopic catalogs. We describe algorithmic and computational challenges faced by such an analysis and compare our results to existing catalogs of Stripe 82 sources in order to determine the best strategies for distinguishing AGN from star-forming galaxies, quiescent galaxies, and other types of sources that can contaminate AGN catalogs. 142.64 Multi-waveband Variations of Blazars from Turbulent Plasmas Crossing Shock Waves Alan P. Marscher1 1Boston Univ.. Exhibit Hall The author is developing a model in which much of the optical and high-energy radiation in a blazar is emitted near the 43 GHz core of the jet as seen in VLBA images, parsecs from the central engine. The main physical features are a turbulent ambient jet plasma that passes through either standing or moving shock waves in the jet. The model allows for short time-scales of optical and gamma-ray variability by restricting the highest-energy electrons radiating at these frequencies to a small fraction of the turbulent cells, perhaps those with a particular orientation of the magnetic field relative to the shock front. Because of this, the filling factor at high frequencies is relatively low, while that of the electrons radiating below about 10 THz is near unity. Such a model is consistent with the following observational trends: (1) red-noise power spectra of flux variations in blazars, (2) shorter time-scales of variability of flux and polarization at higher frequencies, (3) mean polarization levels as well as fractional deviations from the mean that are higher at optical than at lower frequencies, (4) apparent rotations in polarization position angle, and (5) breaks in the synchrotron spectrum by more than the radiative loss value of 0.5. The dependence of items 2-4 on frequency is directly related to the change in spectral index beyond the break, according to the model. The model is being expanded to include high-energy radiation from inverse Compton scattering. The numerical calculation takes into account the light-travel times from cell to cell and from each cell to the observer. The presentation will include preliminary results of this added feature. This research is supported in part by NASA through Fermi grants NNX08AV65G and NNX10AO59G, and by NSF grant AST-0907893. 142.65 Magnetic Fields in Blazar Jets: Radio and Optical Polarization over 20-30 Years Caroline Caldwell1, B. Wills1, D. Wills1, H. Aller1, M. Aller1 1University of Texas. Exhibit Hall Blazars are highly active nuclei of distant galaxies. They produce synchrotron-emitting relativistic jets on scales of less than a parsec to many Kpc. When viewed head-on, as opposed to in the plane of the sky, the jet motion appears superluminal, and the emission is Doppler boosted. Blazars show rapid radio and optical variability in flux density and polarization. There are two types of blazars that can have strong synchrotron continua: non-BL Lac blazars with strong broad emission lines (quasars), and BL Lac objects with only weak lines. We have compiled optical linear polarization measurements of 22 blazars, incorporating much archival data from McDonald Observatory. While the optical data are somewhat sparsely sampled, The University of Michigan Radio Astronomical Observatory observed many blazars over 20-30 years, often well-sampled over days to weeks. These data enabled us to compare optical and radio polarization position angles. We constructed histograms of the separation of polarization position angles of the optical and radio. We found that in BL Lac objects, the histogram has a significant peak at zero separation. Since the polarization position angle indicates the direction perpendicular to the magnetic field vector, finding similar polarization position angles indicates a similar magnetic field at the origin of the optical and radio synchrotron radiation. Non-BL Lac blazars show peaks at zero and 90 degree separation of position angle. The 90 degree separation may be caused by optical depth effects within the jet. Although there are a few sources that do not strongly display the characteristics summarized by the histograms, most sources produce optical and radio polarization position angles that nearly coincide or are separated by 90 degrees. Using VLBA and VLA radio maps, we interpret the results in terms of the position angle of the jet in the sky plane. 143 Black Holes Poster Session Exhibit Hall 143.01 Time-Variable Compact Emission Around the Galactic Center Black Hole Vincent L. Fish1, S. S. Doeleman1, EHT Collaboration 1MIT Haystack Observatory. Exhibit Hall The Galactic Center radio source Sagittarius A* is believed to host a massive black hole. The event horizon of Sgr A* subtends a larger angle than any other known black hole candidate. The resolution of millimeter-wavelength very long baseline interferometry (VLBI) is perfectly suited to studying Sagittarius A*. In prior observations, our collaboration detected Sagittarius A* at 1.3 mm wavelength on a baseline between the James Clerk Maxwell Telescope (JCMT) in Hawaii and the Submillimeter Telescope (SMT) in Arizona, demonstrating the existence of structure on the scale of a few Schwarzschild radii. We report on new 1.3 mm VLBI observations of Sagittarius A* using an array consisting of the JCMT, the SMT, and two telescopes of the Combined Array for Research in Millimeter-wave Astronomy (CARMA) in California. For the first time, we detect Sgr A* on JCMT-CARMA baselines. The data indicate that Sagittarius A* is composed of both a 43 microarcsecond (4.3 Schwarzschild radii) compact component as well as a large-scale component (> 300 microarcseconds) that is resolved out on VLBI baselines. The flux density of the compact component is seen to increase on one day, but the implied size of the emission region remains constant. These result place strong constraints on the quiescent and flaring emission mechanisms of Sgr A*. High-frequency VLBI work is supported by grants from the National Science Foundation. 143.02 Ultraluminous X-ray sources in Interacting Arp Galaxies Douglas A. Swartz1, A. F. Tennant2, R. Soria3 1USRA/MSFC, 2NASA/MSFC, 3MSSL/UCL, United Kingdom. Exhibit Hall Chandra X-ray Observatory spectrophotometric images of interacting galaxies in Arp's Atlas of Peculiar Galaxies are used in a search for Ultraluminous X-ray sources (ULXs). The resulting population census is compared to that of spiral and elliptical galaxies in order to test the hypothesis that ULXs occur more frequently in interacting and in starburst galaxies compared to the normal galaxy population. An interesting number of ULXs are found along tidal tails and bridges suggesting X-ray binary formation is somehow especially favored in these environments. 143.03 Fingerprints of Intermediate Mass Black Holes in Globular Clusters Michele Trenti1 1University of Colorado. Exhibit Hall Globular clusters seem to be the best place to search for Intermediate Mass Black Holes (IMBHs) in the local universe, but so far no definitive observational evidence for their existence has been found. Here we evaluate the uniqueness of classical signatures from stellar dynamics that are typically associated to the presence of a central IMBH (shallow cusp in the surface brightness profile and central rise in the velocity dispersion). We also present a novel technique to identify likely IMBH hosts, based on the measurement of mass segregation in collisionally relaxed globular clusters. 143.04 A Refined Black Hole Mass for the X-ray Transient GRS 1009-45 Phillip Macias1, J. A. Orosz2, C. D. Bailyn3, M. M. Buxton3, P. L. Schechter4, R. A. Remillard4, J. E. McClintock5, J. F. Steiner5 1University of California, Santa Barbara, 2San Diego State University, 3Yale University, 4Massachusetts Institute of Technology, 5Harvard/Smithsonian Center for Astrophysics. Exhibit Hall We have acquired new spectroscopic and photometric observations of the black hole binary GRS 1009-45. The source was observed using the MagE spectrograph on the 6.5m Magellan Clay Telescope at Las Campanas Observatory in February, 2008. A total of 11 useful spectra with a resolving power of 4000 were obtained. The source was monitored by the 1.3m SMARTS telescope at Cerro Tololo Observatory between December, 2007 and June, 2010. In total we obtained 342 useful images in R and 119 images in J. Additional J- and Ks-band images were obtained using the PANIC camera on the Magellan Baade Telescope April, 2008. From the spectra we were able to measure (for the first time) the rotational velocity of the K-star companion. The projected rotational velocity of 86.8 +\- 5.2 km/sec implies a mass ratio of M/M2 of about 17. The spectra also imply an R-band disk fraction of about 30%. The SMARTS light curves show evidence for a strong asymmetry that changes slowly with time. Previously published light curves obtained in runs of a few nights also show an asymmetry. This feature was modeled using a bright spot on the accretion disk. Using all of the available light curves we find an inclination near 50 degrees, and component masses of about 8.5 and 0.5 solar masses for the black hole and companion star, respectively. P. M. acknowledges support from the NSF REU program at San Diego State University that is supported by grant AST-0850564. 144 Binary Stellar Systems, X-ray Binaries Poster Session Exhibit Hall 144.01 Get a Clue with ZZ Boo Brian Kirk1, A. Prsa1, S. Engle1, J. Robertson1 1Villanova University. Exhibit Hall ZZ Bootis is a detached eclipsing binary that has been the subject of spectroscopic analysis before, yet these data were acquired in 1950s and the early 1960s, which prompted us to further study this system. Earlier this year, we acquired spectroscopic data from a 2.1m telescope at Kitt Peak National Optical Astronomy Observatory of ZZ Boo at eighteen different phases. The parameters deduced from eclipsing binaries are used to calibrate our current evolutionary models. These observations give physical confirmation of our theories and allow us to calibrate the mass-luminosity relationship from which the masses of single stars can be estimated. Because a large proportion of stars exists in binary systems, binaries are particularly important to our understanding of the processes by which stars form. Furthermore it has been demonstrated that eclipsing binaries are excellent distance indicators, permitting the calibration of the cosmic distance scale essentially free from assumptions. We prepare the data for study by performing cosmic ray removal, wavelength calibration, and flux normalization for cross-correlations to extract radial velocities. After the reduction process, we use PHOEBE to simultaneously model light curves, radial velocity curves, and spectra of ZZ Boo. We present our current findings on our poster. We gratefully acknowledge grant NSF/RUI grant AST-05-07542. 144.02 The Spectroscopic and Photometric Analysis of the Eclipsing Binary System DN UMa Jordan Robertson1, A. Prsa1, B. Kirk1, S. Engle1 1Villanova University. Exhibit Hall The eclipsing binary system DN UMa (HD 103483) is a likely triple system with a possible pulsating component that has been studied extensively. The period of ~1.7-d has been determined by Gimenez and Queseda (1982). Wilson (1953) reported a systemic radial velocity of -8 km/s, based on a limited data-set. To investigate this interesting object further, we initiated a photometric campaign in April 2009 on the Automatic Photoelectric Telescope in Patagonia, AZ. In January 2010 we followed up DN UMa spectroscopically at the 2.1 m telescope at Kitt Peak National Observatory. The high-resolution echelle spectra have been processed in IRAF. The exposures have been cleaned of cosmic rays, and the extracted spectra have been wavelength-calibrated and flux-normalized. In conjunction with photometry, the spectroscopic data were used to determine fundamental parameters (radii, masses, and temperatures) of the binary star components. We present the results of the modeling based on archival and newly acquired data. 144.03 Solving the Mysteries of Potential Eclipsing Binaries NSV 860 and V795 Cas Emily Rosche1, A. Prsa1, J. Robertson1, B. Kirk1 1Villanova University. Exhibit Hall NSV 860 was classified as an eclipsing binary in 1936 by Zinner but has been neglected since. V795 Cas has also been classified as an eclipsing binary system in the SIMBAD database, however no definitive studies have been done on either one in order to confirm this, so they both seemed objects worthy of further study. Consequently, we have obtained 18 spectra of NSV 860 and 14 spectra of V795 Cas in order to determine the true nature of these systems. Using IRAF software we removed the systematic artifacts and cosmic rays from the data and then proceeded to wavelength-calibrate the spectra. From here we analyzed the spectra in order to accurately and scientifically classify the star systems. We gratefully acknowledge NSF/RUI grant AST-05-07542 and the VURF grant given by Villanova University. 144.04 Analysis and Modeling of Eclipsing Binary AI Hydrae Cindy Villamil1, A. Prsa1, S. G. Engle1, B. M. Kirk1, J. A. Robertson1 1Villanova University. Exhibit Hall AI Hydrae is an F-type detached eclipsing binary that we know a considerable amount about. In 1988, Popper analyzed light curves and spectra of AI Hydrae to determine parameters such as the spectral type, period, orbital eccentricity, systemic velocity, and argument of periastron. We have retaken photometry of the system using the Four College Automated Photoelectric Telescope and acquired echelle spectra with the 2.1 and 4 meter telescopes at Kitt Peak National Observatory, both located in Arizona. We reduced the echelle spectra using IRAF to remove the cosmic rays in the data, perform wavelength calibration, and measure the Doppler shifts of the spectral lines to obtain radial velocity curves. After reducing the spectroscopic data we simultaneously analyzed the radial velocities with the light curves for AI Hydrae to compare those results with the previous values from the literature. With this analysis, we aim to reduce the error margin of the system’s physical parameters such as masses, luminosities, radii, and velocities, and consequently, further calibrate the mass-luminosity relationship. This poster presents preliminary results of our analysis and modeling based on our acquired data. We gratefully acknowledge NSF/RUI grant AST-05-07542. 144.05 Spectral Analysis of the Mass Flow in Binary System U Cephei Peter R. Tupa1, G. G. DeLeo1, G. E. McCluskey, Jr.1 1Lehigh University. Exhibit Hall Data from the International Ultraviolet Explorer (IUE) archive was utilized in the analysis of the Algol type eclipsing binary star system U Cephei (HD 5679). The U Cep system consists of a B7V primary star and G8IV secondary that is actively transferring mass to the primary. A total of 115 spectral images from the IUE archive were analyzed, with special attention given to the 29 images taken during a complete period of 2.5 days. Synthetic spectra generated via TLUSTY and SYNSPEC were used, along with comparison spectra from the standard star Regulus, to determine continuum flux levels, light curves, and radial velocities for the system. Observations of non-photospheric absorption features suggest a transient outward matter flow present in the early observed phases of 0.48 to 0.69, but the same features are significantly reduced in the same phases one period later. Additionally, simulated spectra suggest absorption features previously thought to be high energy Si IV and C IV lines may in fact be anomalous convolutions of different ionic species at lower temperatures. 144.06 CCD Photometric Study of a Rare Algol Dwarf Binary System, V1001 Cassiopeiae Heather Chamberlain1, R. G. Samec1, D. Faulkner2, W. VanHamme3 1Bob Jones University, 2University of South Carolina, Lancaster, 3Florida International University. Exhibit Hall We present a photometric study of detached Algol system, V1001 Cas [RA(J2000) = 23h 50m 17.12 s, Dec(J2000)= +51° 11' 29”, MisV1222, GSC 3651-00655, USNO-A2.0 1350.18742581] with 0.43 days period. It was discovered 2005 and reported in IBVS 5600 (Nakajima, Yoshida, and Ohkura 2005). Their report characterizes it as EB system. Its short period, similar to W UMa’s and its distinct EA light curve (large eclipse depths difference, shallow amplitude secondary, long stretches of low variation outside eclipses) make it rare and interesting for photometric investigation. Our images were taken 26,27, September, 2009, at Lowell Observatory (NURO) and 28 September 2009 via remote observing from Kitt Peak with SARA. UBVRI CCD photometry shows V1001 Cas has a V=1.2 mag primary eclipse and a 0.1 mag secondary amplitude. Our period study yielded 5 times of minimum light. These include JD Hel Min I = 2455100.8306 ± 0.0036, 2455101.6888 ± 0.0002, 2455103.83367 ± 0.00028 , JD Hel Min II = 2455100.6160 ± 0.0005, 2455103.61961 ± 0.0005. Using CCD minima, we calculated the first precision ephemeris, HJD Min I = 2455101.6890 ± 0.0008 + 0. 4287188 ±0.0000002d*E. We first manually fit BVRI Johnson-Cousin’s Photometry with Binary Maker. This revealed V1001 Cas is a well detached binary with spot activity. Next, we performed BVRI simultaneous WD synthetic light curve analysis. With its deeper secondary, the I curve, although of good quality, would not fit with the others. So, we did a BVR solution. Our first solution gives a mass ratio of nearly 1.0, a temperature difference of 850 K, with fill-outs of 71% and 78% of the primary and secondary stars’ respective lobes. We only needed one 22o radius cool spot with a temperature of 0.72 times that of the photosphere. The stars appear to be of mid K and early M main sequence-type. 144.07 The Overcontact Binary V535 Aurigae: Well On Its Way to Coalescing? David H. Bradstreet1, S. J. Sanders1, B. Hiebert-Crape1 1Eastern Univ.. Exhibit Hall V535 Aurigae is a faint (12.8 mag) short period (9.23 hours) overcontact binary which has only one published light curve and no published analysis. 811 digital images in the V filter and 845 in R were obtained over seven nights in the winter of 2008 at the Bradstreet Observatory at Eastern University. The data were obtained using the Observatory’s 41-cm telescope coupled with an SBIG ST-10XME CCD camera. Six new timings of minimum light were measured in order to analyze whether or not the system’s period has changed since its discovery. Preliminary results tentatively indicated that the period had been decreasing linearly over the previous nine years since it was discovered. In order to confirm the large change in period the binary was observed in 2009 and 2010 resulting in complete V and R light curves in both seasons and an additional nine timings of minimum light. These timings confirm that V535 Aur has a dP/dt = -0.208 sec/yr, some twenty times greater than the average period change for overcontact systems. V535 Aur thus displays the largest decrease in period for any known overcontact system. The light curves were compiled into phased normal points and analyzed using the Binary Maker 3.0 light curve analysis software. These preliminary results were then fine tuned using the benchmark Wilson-Devinney code as implemented in Andrej Prsa’s PHOEBE software suite. The analysis shows that the system is totally-eclipsing with a fillout of 85% and equal component temperatures. The extraordinarily large fillout (average for overcontacts ~ 28%), equal stellar temperatures and very large period decrease may indicate that V535 Aur is well on its way to coalescing into a single star. The methods and results of the data acquisition, period study and light curve analysis will be presented in this poster. 144.08 Very Wide Binaries Robert Olling1, E. Shaya1 1Univ. Of Maryland. Exhibit Hall We develop Bayesian statistical methods for discovering and assigning probabilities to physical stellar companions. The probabilities depend on similarities in "corrected" proper motion, parallax, and the phase-space density of field stars. Very wide binaries with separations over 10,000 AU have recently been predicted to form during the dissolution process of low-mass star clusters. In this case, these wide systems would still carry information about the density and size of the star cluster in which they formed. Alternatively, Galactic tides and weak interactions with passing stars peel off stars from such very wide binaries in less than 1/2 of a Hubble time. In the past, these systems have been used to rule in/out MACHOs or less compact dark (matter) objects. Ours is the first all-sky survey to locate escaped companions that are still drifting along with each other, long after their binary bond has been broken. We test stars for companionship up to an apparent separation of ~8 parsec: 10 to 100 times wider than previous searches. Among Hipparcos stars within 100 pc, we find about 260 systems with separations between 0.01 and 1 pc, and another 190 with separation from 1 to 8 parsec. We find a number of previously unnoticed naked-eye companions, among which: Capella & 50 Per; Alioth, Megrez & Alcor; gamma & tau Cen; phi Eri & eta Hor; 62 & 63 Cnc; gamma & tau Per; zeta & delta Hya; beta01, beta02 & beta03 Tuc; 44 & 58 Oph and pi & rho Cep. At least 15 of our candidates are exoplanet host stars. 144.09 Standardization of Comparison Stars in the Fields of 10 High Mass X-ray Binaries Eric G. Hintz1, M. D. Joner1 1Brigham Young Univ.. Exhibit Hall To support our current observing program to monitor High Mass X-ray Binary (HMXB) systems for optical variability, we calibrated a large sample of comparison stars in the fields of ten HMXB systems. This was done using the new BYU West Mountain 0.9-m telescope. Calibrations were done in the B, V, and I filter with Landolt standard fields. Two of our systems, 4U 1907+09 and KS 1947+300, had previously published magnitudes for the optical counterpart of each x-ray system. The eight remaining systems had no identified optical counterparts. These systems include: AXJ1844.8-0258, 4U 1850-03, 4U 1901+03, 4U 1908+075, XTE J1906+090, XTE J1908+094, IGR J19140+0951, and IGR 18410-0535. We will report on the calibrations for each field and an attempt to identify each optical counterpart. This work is supported by NSF grants AST-0618209. We also acknowledge support from a BYU ORCA MEG grant. 144.10 Potential Optical Counterparts to High Mass X-Ray and ?-Ray Binaries Carl Mitchell1, M. V. McSwain1 1Lehigh University. Exhibit Hall We seek to identify optical counterparts to several previously discovered high mass X-ray binaries and ?-ray sources from the Liu et al. and Fermi first year catalogues. Observations were taken with the CTIO 0.9-meter telescope, operated by the SMARTS Consortium. Photometric data were taken in the Strömgren b and y filters, as well as a narrow-band H? filter. We present color-color diagrams of y-H? vs. b-y for each field, and candidates for optical counterparts were selected based on their excesses of H? emission. We also present spectral energy distributions for select candidates. This work is supported by the NSF REU site grant PHY-0849416, NASA DPR No. NNX09AT67G, and Lehigh University. We also thank the SMARTS Consortium, Rachael Roettenbacher, Tina Aragona, and Amber Marsh. 144.11 Time-series, Multi-wavelength Monitoring Of The High Mass X-ray Binary 4U 2206+54 Jessica L. Bugno1, E. G. Hintz1, M. D. Joner1, C. D. Laney1 1Brigham Young University. Exhibit Hall The high mass X-ray binary 4U 2206+54 has been a very controversial system. Optical time-series observations of this system from West Mountain Observatory and the Orson Pratt Observatory were analyzed to determine a more accurate orbital period. The summers of 2008 and 2009 provided a total of 55 nights of observations in the Johnson V filter. The summer of 2010 provided 20 nights of observations in Johnson BVRI. We present our preliminary results as of October 1, 2010 as well as the error analysis for the data. We also acknowledge NSF grant AST-0618209 for data collected from the West Mountain 36” telescope. 144.12 Optical Monitoring Of Two High Mass X-ray Binary Systems: 4u 1907+09 And Ks 1947+300 Juan C. Payan1, E. G. Hintz2, M. D. Joner2 1Worcester Polytechnic Institute, 2Brigham Young University. Exhibit Hall Using the BYU West Mountain 0.9-m telescope we monitored two High Mass X-ray Binary systems during the summer of 2010. The optical counterpart for 4U 1907+09 is reported as an O9 Ia star with an orbital period of 8.38 days and a magnitude of V= 16.4. For KS 1947+300 we find a B0 Ve reported as the optical counterpart with an orbital period of 40.4 days and V=14.2. We felt these two targets provided a good test of the new telescope’s capabilities. Each target was observed every clear night from June to September in the broadband B, V, and I filter. We will report on the optical variability seen in both systems and its relation to the published periods. This work is supported by NSF grant AST-0618209. 144.13 Optical Monitoring Of Three High Mass X-ray Binary Systems: BD+53 2262, RX J2030.5+4751, And BD+49 3718 Nathaly Zurita1, E. G. Hintz1, E. Salway1, C. R. Porritt1 1Brigham Young University. Exhibit Hall Over the past four summers we have monitored a number of High Mass X-ray binary systems as part of our undergraduate research program, including our REU program. These systems have been primarily monitored using the 0.4-m telescope of the BYU Orson Pratt Observatory. The data set is a mixture of high density single night observing runs that cover many hours, along with long term night to night monitoring. In this poster we will present preliminary results for three systems we have monitored; BD+53 2262, RX J2030.5+4751, and BD+49 3718. We wish to acknowledge the support of a BYU ORCA MEGs grant which has provided support for this program. 144.14 CCD Photometry Of The Extreme Mass Ratio Binary, TYC 1404-1687-1 Danny R. Faulkner1, Ron Samec, Evan Figg, Bruce Oliver, Astronomy Program, Bob Jones University, Walter VanHamme, Florida Interational University 1University of South Carolina Lancaster. Exhibit Hall We report our photometric analysis of the variable, TYC 1404-1687-1 (GSC 1404 1687, Cancer). The images were taken in December, 2008, March 2009 with NURO and 16 January 2009 via remote observing with SARA North. The UBVRI CCD photometry shows that TYC 1404-1687-1 has a totally eclipsing W UMa light curve, yet it has a shallow amplitude (AV~0.4 mag.). We studied the possibility the low amplitude was due to the presence of a third component: we began our analysis with ~30% third light as determined from Binary Maker. Next, we performed a BVRI simultaneous WD synthetic light curve analysis. Surprisingly, we obtained two nearly identical sums of square solutions, one with a measurable but small third light component (0-2%) and another with no third light. We conclude that the solution does not require a third light. Our period study yielded 9 new times of minimum light, two from ROTSEI curves, JD Hel Min= 2452721.4226 and 2452728.3972, and the others from our observations: HJD Min I = 2454848.8844 ±0.0014, 2454901.8924 ±0.0006, 2454902.6903 ±0.0014, 2454904.6790 ±0.0058, HJD Min II = 2454823.9678 ±0.0017, 2454827.9618 ±0.0005, 2454901.6927 ±0.0005. Using these, we calculated the first precision ephemeris for this system, HJD Min I = 2454902.6912 ±0.0009 + 0.3985874 ±0.0000003 d*E. UBVRCIC standard magnitudes were determined. We find that the comparison star (GSC 1404 0119) is a late G-type dwarf while the check star (GSC 1404 0587) is a mid F-type dwarf. The binary is an F0V contact binary. We also performed a number of solutions (a q-search) which minimized at a mass ratio near 0.2. Our WD solution gave a fill-out of 45%. No spots are needed in the solution. So we find that TYC 1404-1687-1 is among the once rare, but growing number, of low amplitude-extreme mass ratio, totally eclipsing binaries. 144.15 The Mass Transfer Rate Of A Nearly Semi-detached Eccentric Binary Star Systems Colby Haggerty1, J. F. Sepinsky1 1University of Scranton. Exhibit Hall We calculate the instantaneous mass loss rate of a nearly-semi-detached donor star in an eccentric orbit about its companion by taking into account the varying size and shape of the donor’s Roche Lobe throughout the orbit. As in the circular case, we model the density of the stellar atmosphere as a decreasing exponential function of the instantaneous gravitational potential above the photosphere. At each point in the orbit, the equipotential surfaces corresponding to the stellar photosphere and the inner Lagrangian point need to be recalculated due to the changing distance between and relative orbital velocity of the two objects. By analyzing the shape of the potential in the vicinity of the inner Lagrangian point we can determine the effective cross-section of the flow out of the donor star’s effective Roche Lobe. Combining this with mass density and sound speed we determine the instantaneous mass loss rate through the inner Lagrangian point of the donor star at each point in the orbit. We show the functional form of this rate over the course of a single orbit for a wide variety of binary parameters. This orbit variable mass loss rate is vital to proper calculations of orbital evolution of mass transferring eccentric binary system. 144.16 Estimating the Fraction of Binaries Affecting the JMAPS Astrometry Henrique R. Schmitt1, B. F. Lane2, R. B. Hindsley3 1NRL/CPI, 2C. S. Draper Laboratory, 3NRL. Exhibit Hall We estimate the fraction of stars that are binaries and have a large enough motion of the center of light relative to the center of mass of the system, larger than 1 mas, to significantly affect the astrometric accuracy of the Joint Milli-Arcsecond Pathfinder Survey (JMAPS). These calculations were done using information about the observed distribution of spectral types, the frequency of binary systems as a function of spectral type, their mass ratios and period distributions. We find that, for systems with periods smaller than 10 years, approximately 12 percent of the stars with I=2 mag will have a motion of the center of light relative to the center of mass larger than 1 mas, decreasing to less than 1 percent for stars with I=14 mag. We explore the effects of reddening, orbital eccentricity, and different distributions of spectral types, to these fractions. These results are compared with the fraction of binary stars detected by the Hipparcos satellite. 144.17 Exploring Possible Origins of an Improbable Binary Star in the Open Cluster NGC 6819 Through Dynamical Exchange Simulations Thomas Finzell1, A. Geller2, N. Gosnell1, R. Mathieu1 1UW Madison, 2Northwestern University. Exhibit Hall We model the origin of the binary star system, NGC 6819-3002-a highly improbable star system that is likely the remnant of a dynamical encounter. The horizontal-branch primary star would have had a large enough radius while in it's giant phase to engulf the orbit of the secondary star, making it very unlikely that these two stars were born together. In order to explore the likelihood that the binary was created via a dynamical exchange interaction we use a scattering experiment algorithm to simulate encounters between a single star and binary system. We use this to investigate the possible initial parameters that could produce the currently observed properties of the system. We incorporate the scattering experiments within a genetic algorithm, which searches over the large parameter space and iteratively selects initial parameters that yield the observed binary. The genetic algorithm gives us the ability to confine the potential parameter space into one of a computationally manageable size. We then perform a more systematic search of the identified region of parameter space in order to determine the multi-dimensional probability distribution of parameters that can produce NGC 6819-3002. We then correlate that probability distribution with the distribution of binary and stellar parameters of NGC 6819 in order to determine the likelihood that such a dynamical interaction could have occurred. The result of this process shows that NGC 6819-3002 may indeed have originated through a dynamical exchange interaction. Applying this technique to additional stars and star systems in other clusters will allow us to constrain the impact of dynamical encounters on the formation of anomalous objects like NGC 6819-3002. We gratefully acknowledge funding from the National Science Foundation under grant AST-0908082. 144.18 Comparisons Between SPH and Grid-Based Simulations of the Common Envelope Phase Jean-Claude Passy1, C. L. Fryer2, S. Diehl2, O. De Marco3, M. Mac Low4, F. Herwig5, J. S. Oishi6 1American Museum of Natural History and University of Victoria, 2Los Alamos National Laboratory, 3Macquarie University, Australia, 4American Museum of Natural History, 5University of Victoria, Canada, 6Kavli Institute for Particle Astrophysics and Cosmology. Exhibit Hall The common envelope (CE) interaction between a giant star and a lower-mass companion provides a formation channel leading eventually to Type Ia supernovae, sdB stars and bipolar PNe. More broadly, it is an essential ingredient for any population synthesis study including binaries, e.g. cataclysmic variables. Occurring on a short time scale - typically between one and ten years, the CE interaction itself has so far never been observed with certainty but the existence of companions in close orbits around evolved stars, whose precursor's radius was larger than today's orbital separation, vouches for such interaction taking place frequently. Via a detailed study of the energetics and the use of stellar evolution models, we derived in our previous paper the efficiency ? of the CE interaction from a carefully selected and statistically analyzed sample of systems thought to be outcomes of a CE interaction. We deduced the initial configuration of those systems using stellar models, and derived a possible inverse dependence of ? with the companion to primary mass ratio. Here, we compare these predictions to numerical simulations with two different codes. Enzo is a 3D adaptive mesh refinement grid-based code. For our stellar problem we have modified the way gravity and boundary conditions are treated in this code. The SNSPH code is a 3D hydrodynamics SPH code using tree gravity. The results from both codes for different companion masses and different types of primary stars are consistent with each other. Those results include a resolution study of a 0.88 M? red giant interacting with a 0.9, 0.6 and 0.3 M? white dwarf, respectively. Those systems reach a final separation of 25, 18 and 10 R?, respectively. In this contribution, we present and discuss those results and compare them to our predictions. This research was funded by NSF grant 0607111. 144.19 The Colliding Stellar Winds of the Extreme Wolf-Rayet Binary CQ Cephei Rosina Iping1, G. Sonneborn1, J. C. Bouret2 1NASA's GSFC, 2Laboratoire d'Astrophysique de Marseille, France. Exhibit Hall We present time-resolved observations of the Wolf-Rayet + O star Binary CQ Cephei using the FUSE satellite. We acquired a series of observations of CQ Cephei and determined the structure of the bow shock zone formed when the winds of the two hot stars collide. CQ Cephei has the shortest period of all the known W-R+O binaries. The W-R star is classified as a nitrogen-rich WN6 star and the companion as an O9 II-Ib star. The observations cover a significant part of the 1.64-day orbital period. We were able to study the wind interaction zone from phase-dependent spectral variations. Of particular importance in the FUSE wavelength range is the large number of emission lines of abundant elements with different ionization potentials, ranging from O VI, S IV, P V, C III, to N II. The S and P lines are important because these elements are produced only in SN explosions and are not enhanced by nuclear processes in the binary stars themselves. We present improved constraints on orbital parameters and on characteristics of the W-R star itself (wind momentum, mass-loss rate, and abundances). 144.20 Mass of the Black Hole in V4641 Sgr Rachel K. D. MacDonald1, C. D. Bailyn1, A. G. Cantrell1 1Yale University. Exhibit Hall V4641 Sgr is a galactic microquasar, or x-ray binary, with a B9III star as secondary and an orbital period of 2.82 days. Although the secondary star is very bright (13th mag.), it is clear that the disk around the black hole also contributes to the optical emission. This makes the determination of the orbital inclination, and thus the mass of the compact object, uncertain. We present simultaneous spectroscopy and photometry from 2009 and 2010, taken at the SMARTS telescopes in Cerro Tololo, Chile, which enables us to determine the disk fraction of the optical emission. Once this disk fraction has been determined, a more definitive mass measurement for the black hole in the system will be possible. 144.21 Photometry, Spectroscopy, And Doppler Tomography Of The Eclipsing LMXB EXO 0748-676 = UY Vol Valerie J. Mikles1, R. I. Hynes1, E. D. Jones1 1Louisiana State University. Exhibit Hall We present optical spectra and Doppler tomography of the low-mass X-ray binary EXO 0748-676 = UY Vol. UY Vol is an eclipsing X-ray binary hosting a neutron star. With a total of 65 spectra spread over 4 nights, we have complete phase coverage and construct trailed spectra and Doppler tomograms for thirteen lines and line blends. Although we were not able to detect fluorescent N III/C III emission from the irradiated secondary, we do detect S-wave emission of several He II lines and O II 5289A. Our analysis of the trailed spectra and tomograms allows us to constrain the origin of the line emission. UY Vol has spent the better part of the last two decades in a burst state, but since our spectroscopy, the source has entered a quiescent phase. The optical counterpart, originally ~17th mag has faded substantially to R~22 mag. We present a new light-curve of the source in its quiescent state. This work is partially supported by the National Science Foundation under Grant No. AST-0908789 and by NASA/Louisiana Board of Regents grant NNX07AT62A/LEQSF(2007-10) Phase3-02. 144.22 New Low-Mass PMS Eclipsing Binaries In Orion Maria Morales-Calderon1, J. R. Stauffer1, L. M. Rebull1 1IPAC-CALTECH. Exhibit Hall In Fall 2009, we conducted a large, multi-wavelength time-series photometric monitoring campaign of about a one square degree region of the Orion Nebula cluster (ONC). Our program produced light curves for 2000 Orion young stellar objects (YSOs), with data often in at least four bands (I, J, [3.6] and [4.5]). While our primary goal was to use these data to investigate the structure of the inner disk and time-variable accretion in YSOs with circumstellar disks, these data also provide a treasury of data on all types of pre-main-sequence (PMS) variability. Specifically, we identify nine stars in our FOV whose light curves show eclipse features. Four of these are the previously known ONC eclipsing binaries (EBs) and the other five systems are newly identified ONC PMS EB candidates - more than doubling what was known up to now. Here we present our current work to confirm these candidates. 144.23 Characterizing X-ray Point Source Populations in Nearby Galaxies Tyler D. Desjardins1, R. E. Kilgard1, A. H. Prestwich2 1Wesleyan University, 2Harvard-Smithsonian Center for Astrophysics. Exhibit Hall We present an analysis of Hubble Space Telescope ACS images of the nearby galaxies IC 10 and M 51 in which we determine the characteristics of optical sources that are coincident with X-ray point sources detected with the Chandra X-ray Observatory. For IC 10, we find optical counterparts for six sources consistent with B dwarf stars, with one of the sources likely coincident with an OB association. In M 51, there are twelve X-ray sources that have stellar counterparts with colors and magnitudes indicating O and B dwarfs as well as several early type supergiants. H-alpha images show several supernova remnants in M 51 that are coincident with X-ray point sources. We also present preliminary results on constructing discrete X-ray source luminosity functions segregated by class of optical counterpart. 144.24 The Chandra Galactic Bulge Survey Robert I. Hynes1, P. G. Jonker2, C. G. Bassa3, A. Dieball4, S. Greiss5, T. J. Maccarone4, G. Nelemans6, D. Steeghs5, M. A. P. Torres2, C. T. Britt1, J. L. Clem1, L. Gossen1, J. E. Grindlay7, P. J. Groot6, L. Kuiper2, E. Kuulkers8, M. Mendez9, V. J. Mikles1, E. M. Ratti2, N. Rea10, L. van Haaften6, R. Wijnands11, J. J. M. in't Zand2 1Louisiana State Univ., 2SRON-Netherlands Institute for Space Research, Netherlands, 3University of Manchester, United Kingdom, 4University of Southampton, United Kingdom, 5University of Warwick, United Kingdom, 6Radboud University, Netherlands, 7Harvard-Smithsonian, CfA, 8ESA/ESAC, Spain, 9Groningen University, Netherlands, 10ICE, CSIC-IEEC, Spain, 11University of Amsterdam, Netherlands. Exhibit Hall The Chandra Galactic Bulge Survey (CGBS) is a shallow but wide survey of two approximately 6x1 degree strips of the Galactic Bulge about a degree above and below the plane. The survey by design targets regions where extinction and crowding are manageable and optical counterparts are accessible to detailed follow-up. Our strategy is based on going deep enough to detect quiescent low-mass X-ray binaries (LMXBs), but no deeper in order to avoid an excess of cataclysmic variables (CVs), while covering a large area to maximize the numbers of recovered objects. The primary goals of the CGBS are to test predictions of binary evolutionary models through number counts and period distributions of detected sources, and to greatly expand the sample of LMXBs suitable for detailed optical follow-up including mass determination. We have recovered over a thousand X-ray sources most with optical counterparts, and expect these to be divided evenly between quiescent LMXBs, magnetic CVs, and R CVn stars, with smaller numbers of other source types. We are actively pursuing multiwavelength follow-up including searches for optical, infrared, and ultraviolet counterparts, measurement of variability, and optical spectroscopy. So far we have identified about ten candidate LMXBs and CVs and a few other unusual objects such as X-ray selected sdO and carbon stars, both likely products of binary evolution. This work is supported by the National Science Foundation under Grant No. AST-0908789. 144.25 Chandra And Hst Studies Of The Prototype Ns X-ray Transient, Cen X-4 Samuel Park1, M. R. Garcia1 1Harvard - Smithsonian. Exhibit Hall For nearly a century Black holes have been a hot topic, a physical singularity or simply a flawed, all be it brilliant, mathematical concept? Fundamental proof of the existence of black holes lies in the proof of the existence of their event horizons. One such proof lies in the comparison of the X-ray luminosities of black hole and neutron star X-ray transients however this proof assumes that both NS and BH transients continue to accrete at low Mdot during quiescence. Cen X-4 is the prototype NS X-ray transient, and this work is compared to A06020-00, the prototype BH X-ray Transient. As part of this comparison we obtained the first short-wavelength UV spectrum of Cen X-4 in 2004 with HST STIS and obtained simultaneous X-ray data with Chandra. Interestingly, the X-ray flux was found to decrease by a factor of three, while the UV was down by a factor of two. We report on our search for evidence for a disk in the UV and optical spectra, even at these very low Mdot levels. We have extracted the highest quality spectrum from the HST STIS and Chandra data, and compared Cen X -4 to A0620, searching for hints as to the accretion, emission mechanisms and ultimately the existence of their event horizons. This research as been jointly funded by the University of Southampton and the Harvard-Smithsonian center for astrophysics. 144.26 A Chandra Search for Low-mass Companions of Late B Stars in Tr 16 Nancy Remage Evans1, K. DeGioia-Eastwood2, M. Gagne3, L. Townsley4, S. Wolk1, Y. Naze5, P. Broos4, M. Corcoran6, L. Oskinova7, A. F. J. Moffat8, J. Wang1, N. Walborn9 1SAO, 2Northern Arizona University, 3West Chester University, 4Pennsylvania State University, 5Universite de Liege, Belgium, 6NASA's Goddard Space Flight Center, 7University of Potsdam, Germany, 8Universite de Montreal, Canada, 9Space Telescope Science Institute. Exhibit Hall The cluster Tr 16 is included within the area of the large survey of the Carina region with Chandra (PI: Townsley). Stars later than B3 are not known to produce X-rays. On the other hand, low mass stars (later than mid-F spectral type) produce copious X-rays when they are young. We have developed a list of B3 to A0 stars in the young cluster Tr 16 which: 1.) are within 3' of Eta Car, 2.) have an appropriate V and B-V combination (including a range of +/- 0.1 in E(B-V), and 3.) have proper motions consistent with cluster membership. We have identified stars from this list which are X-ray sources on a 90 ksec Chandra image of Tr 16. Presumably the X-rays are produced by a low mass companion, at least in nearly all cases. This attribution is reinforced by the fact that the X-ray sources have higher median temperatures than O and early B sources. In addition, the spectral fits to 4 strongest sources produce temperatures typical of low-mass coronal sources. On this basis, 39% of the late B stars have low mass companions. Interpretation of this number depends on the completeness of the X-ray detections, however discussion of the low mass stars in Tr 16 indicates that stars which will be M stars on the main sequence are detected. N. Evans acknowledges support from the Chandra X-ray Center NASA Contract NAS8-03060 144.27 LSI +61 303 And LS5039: More Mysteries Uncovered By Fermi Richard Dubois1, Fermi LAT Collaboration 1SLAC National Accelerator Laboratory. Exhibit Hall Results from the first two year of Fermi LAT (Large Area Telescope) observations of the bright sources LS I +61 303 and LS 5039, well observed binary systems at X-ray and TeV energies, have yielded new questions at GeV energies about their nature. These sources are proving to be surprising in terms of spectral behaviour and variability. The exponential cutoff seen in both sources is very reminiscent of the many pulsars Fermi has found, yet the orbital variability is not expected in that interpretation. In addition, LS I +61 303 has shown remarkable, abrupt changes in its flux levels and orbital modulation. In survey mode the LAT observes every point in the sky every 3 hours making it an ideal monitor for these systems. 144.28 Gamma-Ray Emission from Variable Galactic Radio Sources Chris R. Shrader1, D. J. Macomb2 1NASA's GSFC, 2Boise State University. Exhibit Hall We describe our ongoing program using data obtained with the Swift/BAT and the Fermi Large Area Telescope to search for hard-X-ray and gamma-ray emission from recently published surveys of galactic radio sources. Radio emission was established as a ubiquitous property of gamma ray sources prior to the launch of Fermi and subsequent examination of the composition of the 1451 source catalog of that mission further supports this idea. Known classes of galactic variable radio sources include high-mass X-ray binaries such as Cyg X-3 and LSI +61 303 which are already established gamma-ray emitters. Those objects are often transient in nature and they are often revealed through survey observations in the hard-X-ray band. Additional objects among this class may be revealed and establishing them as gamma-ray emitters would be of great interest. Other possible source classes include magnetars, RRATs (Rotating Radio Transients) and flare stars. Most interestingly, totally unexpected phenomena could also be revealed. We will describe our sample selection, data extraction and analysis methods and present results obtained to date. 144.29 Gamma-ray/x-ray Observations Of The Be-pulsar Binary 1a0535+262 During A Major Outburst Angelo Varlotta1, G. Maier2, VERITAS 1Purdue University, 2Deutsches Elektronensynchrotron (DESY), Germany. Exhibit Hall The detection of Cyg X-1, PSR B1259-63, LS 5039 and LS I +61 303 at TeV energies have established X-ray binaries as a new class of VHE gamma-ray emitters. In this work, we report results from gamma-ray and X-ray observations of 1A035+262 during a major outburst in December 2009. The TeV gamma-ray data were obtained with VERITAS (0.1-30 TeV). We also used public Fermi/LAT data to cover the GeV band (0.1-300 GeV). The X-ray data were obtained with the RXTE/PCA (2-60 keV) and Swift/XRT (0.3-10 keV). The observations provided a good coverage of the X-ray outburst, as well as the binary orbit. 1A0535+262 was not detected at TeV or GeV energies. This is consistent with the fact that the observed X-ray continuum can be described as the combination of blackbody and Comptonized emission from thermal electrons (presumably in the accretion disk and "corona") and that the source radiates little at radio wavelengths. The lack of non-thermal electrons distinguishes the source from those Be X-ray binaries (such as PSR B1259-63 and LS I +61 303) that have been detected at GeV-TeV energies. We discuss the implications of the results on theoretical models. 145 Career Paths, Professional Development, and STEM Diversity Poster Session Exhibit Hall 145.01 The Astronomer's H-R diagram Alberto Conti1, S. Lowe2, A. Accomazzi3, G. DiMilia3 1STScI, 2LCOGT, 3ADS. Exhibit Hall Most people who've taken an astronomy course are familiar with the Hertzsprung-Russell diagram. It was developed to show the relationships between the temperature (or colour) of a star and its luminosity. Following this premise and an original idea by Stuart Lowe, we asked ourselves if american astronomer as a group have a "Main Career Sequence" in the space of Peer Reviewed papers and "absolute" Google index. Here we expand on Stuart's original idea examining several cuts in publication and Google parameter space with the help of proper ADS data 145.02 Career Outcomes for Astronomy Ph.D. Graduates of the University of Texas at Austin: The Next Generation Harriet L. Dinerstein1 1Univ. of Texas, Austin. Exhibit Hall Sixteen years ago I conducted a survey of the career trajectories and outcomes of 78 individuals who earned Ph.D.s from the Department of Astronomy at the University of Texas at Austin during the period 1984-1995 (Dinerstein, H. 1996, AAS, 189.0501). In the current poster I extend these statistics up to the present, adding 68 Ph.D. recipients from 1996-2010. This is a sufficiently large sample to search for secular trends such as possible changes in duration of the postdoctoral stage, redistribution of demographics among different kinds of long-term positions, and the emergence of new categories of astronomy-related employment. The picture is less discouraging than one might expect. As of 2010, about 75% of the Texas graduates 7 - 14 years past the Ph.D. are still doing astronomy, and most of those in non-astronomical careers left the field by choice (and often have had considerable success in their alternate careers). Of those 6 years or less past the Ph.D., 50% were in postdoctoral positions and less than 10% had left astronomy. Recent reconsiderations of the employment market (Metcalfe, T.S. 2008, PASP, 120, 229; Seth, A. 2009, Astro2010: The Astronomy and Astrophysics Decadal Survey, Position Paper No. 51) make the point that a typical astronomer who ultimately achieves a permanent position will have held two or three prior temporary positions; this was equally true three decades ago. There has been notable growth nationwide in the number of astronomers employed as faculty at small liberal arts colleges and other undergraduate-centered institutions, a trend that to some degree was anticipated by the University of Texas cohort, which included a number of students for whom this was their personal goal. In a world where job certainty is no longer so prevalent, motivated and resourceful astronomers are finding ways to remain active members of our community. 145.03 AstroBetter: A Blog and Wiki for Professional Astronomers Kelle L. Cruz1, J. Lu2, J. Rigby3, E. Bressert4, T. Robitaille5, M. Huerta6, S. Dhital7 1Hunter College/CUNY & AMNH, 2Caltech, 3Greenbelt, MD, 4University of Exeter, United Kingdom, 5Harvard/CfA, 6Gentleman Scholar, 7Vanderbilt. Exhibit Hall AstroBetter.com is a multi-contributor blog and wiki website designed for information sharing among professional astronomers. The goal of the site is to increase the productivity of astronomers by creating a centralized location for tips and tools of our multifaceted trade. Our content includes topics related to data reduction and analysis, general computing, writing papers and proposals, giving talks, teaching, career planning, productivity, organization, and diversity and equity in science and education. While we have several contributors, the site is intended to be community driven and we encourage everyone to publish to the wiki, submit guest posts, suggest post ideas, and to comment on blog entries. One of our primary goals is to consolidate and reduce the transient nature of the astronomy community's collective knowledge base by having an active wiki. Currently, the most common way to share astro-centric tools and tips that are not appropriate for a published paper, is to put them on an individual's website. However, the average astronomer's website will have at least four different addresses over the course of their career and only the site owner can edit the content. As a result, information on personal websites goes stale very quickly and dead links to such sites abound. It is our hope that community maintained wikis, such as the one hosted on AstroBetter, will gradually replace the personal website. In this poster we introduce the contributors to AstroBetter, show statistics about our current readership, give excerpts of some of our most popular posts and wiki entries, and show how anyone can add or edit content on the wiki. The goal of this poster is to spread the word about AstroBetter and increase our community of readers and wiki editors, because together, we can AstroBetter. 145.04 LGBT Workplace Issues for Astronomers Laura E. Kay1, R. Danner2, K. Sellgren3, V. Dixon4, GLBTQastro 1Barnard College, 2Northrup Grumman Aerospace Systems, 3Ohio State University, 4Johns Hopkins Univ.. Exhibit Hall Federal Equal Employment Opportunity laws and regulations do not provide protection from discrimination on the basis of sexual orientation or gender identity or gender expression. Sexual minority astronomers (including lesbian, gay, bisexual and transgender people; LGBT) can face additional challenges at school and work. Studies show that LGBT students on many campuses report experiences of harassment. Cities, counties, and states may or may not have statutes to protect against such discrimination. There is wide variation in how states and insurance plans handle legal and medical issues for transgender people. Federal law does not acknowledge same-sex partners, including those legally married in the U.S. or in other countries. Immigration rules in the U.S. (and many other, but not all) countries do not recognize same-sex partners for visas, employment, etc. State `defense of marriage act' laws have been used to remove existing domestic partner benefits at some institutions, or benefits can disappear with a change in governor. LGBT astronomers who change schools, institutions, or countries during their career may experience significant differences in their legal, medical, and marital status. 145.05 Commitment to Broadening Participation at NOAO Catharine D. Garmany1, D. Norman1 1National Optical Astronomy Observatory. Exhibit Hall AURA and NOAO take seriously the importance of Broadening Participation in Astronomy. At the request of the AURA President, each of the AURA centers (NOAO, NSO, STSCI, Gemini) appointed a Diversity Advocates (DA). At NOAO this job is shared by Dara Norman and Katy Garmany, who were appointed by Dave Silva in Jan 2009. The DA’s are members of the AURA Committee on Workforce and Diversity (WDC), a designated subcommittee of the AURA Board of Directors. The role of this committee includes reviewing activities and plans on an AURA wide basis aimed at broadening the participation within AURA, and reviewing AURA wide policies on the workforce. At NOAO, the role of the DAs spans a number of departments and activities. They serve on observatory search committees, and offer suggestions on how NOAO job searches can reach the most diverse audience. The DA’s job is to insure that NOAO actively pursues every opportunity to increase diversity: to this end they are involved in outreach and educational activities that focus on workplace development and encourage inclusion of woman, minorities and persons with disabilities. 145.06 Current Results and Future Directions of the Pulsar Search Collaboratory Sue Ann Heatherly1, R. Rosen1, M. McLaughlin2, D. Lorimer2 1NRAO, 2West Virginia University. Exhibit Hall The Pulsar Search Collaboratory (PSC) is a joint partnership between the National Radio Astronomy Observatory (NRAO) and West Virginia University (WVU.  The ultimate goal of the PSC is to interest students in science, technology, engineering, mathematics (STEM) fields by engaging them in conducting authentic scientific research—specifically the search for new pulsars.  Of the 33 schools in the original PSC program, 13 come from rural school districts; one third of these are from schools where over 50% participate in the Free/Reduced School Lunch program.  We are reaching first generation college-goers.  For students, the program succeeds in building confidence in students, rapport with the scientists involved in the project, and greater comfort with team-work.  We see additional gains in girls, as they see themselves more as scientists after participating in the PSC program, which is an important predictor of success in STEM fields. The PSC has had several scientific successes as well.  To date, PSC students have made two astronomical discoveries: a 4.8-s pulsar and bright radio burst of astrophysical origin, most likely from a sporadic neutron star.   We will report on the status of the project including new evaluation data. We will also describe PSC-West, an experiment to involve schools in Illinois and Wisconsin using primarily online tools for professional development of teachers and coaching of students. Knowledge gained through our efforts with PSC-West will assist the PSC team in scaling up the project. 145.07 The California-Arizona Minority Partnership for Astronomy Research and Education (CAMPARE): an Educational Experience for Undergraduates at the University of Arizona Alumni Association's Astronomy Camp. Courtney Lemon1, D. McCarthy2, A. Rudolph1 1California State Polytechnic University, Pomona, 2University of Arizona. Exhibit Hall The California-Arizona Minority Partnership for Astronomy Research and Education (CAMPARE) is an NSF-funded partnership between the Astronomy Program at Cal Poly Pomona (CPP) and the University of Arizona Steward Observatory designed to promote participation of underrepresented minorities (including women) in astronomy research and education. As part of the education component of the program, CPP undergraduate physics majors and minors are eligible to work as a counselor at the University of Arizona's Astronomy Camp, one of the premier astronomy outreach opportunities in the world. CAMPARE students have the opportunity to work in this learn-by-doing environment with a wide range of students to gain first hand experience of teaching astronomy to students of a wide variety of ages in highly structured educational setting. Cal Poly Pomona students who are interested in education, both formal and informal, work in a variety of camps, from Girl Scout camps to camps for advanced high school students, to further their understanding of what it means to be a professional in the field of education. The CAMPARE student who participated in this program during summer 2010 had the opportunity to work under Dr. Don McCarthy, camp director of University of Arizona's Astronomy Camps for 20 years, and observe the interpersonal relations between campers and staff that is so vital to the learning the students receive. Through these observations, the CAMPARE student was able to learn to gauge students' interest in the material, and experience real life teaching and learning scenarios in the informal education realm. 145.09 The Lowell Observatory Predoctoral Scholar Program Lisa A. Prato1 1Lowell Observatory. Exhibit Hall Lowell Observatory is pleased to solicit applications for our Predoctoral Scholar Fellowship Program. Now beginning its fourth year, this program is designed to provide unique research opportunities to graduate students in good standing, currently enrolled at Ph.D. granting institutions. Lowell staff research spans a wide range of topics, from astronomical instrumentation, to icy bodies in our solar system, to exoplanet science, to stellar populations and dwarf irregular galaxies. First light with the observatory's new 4.2 meter Discovery Channel Telescope is expected in 2011, making this a particularly exciting time in our history. Student research is expected to lead to a thesis dissertation appropriate for graduation at the doctoral level at the student's home institution. Currently, five students are enrolled in our program; our first graduate completed the program in August, 2009. The Observatory provides competitive compensation and full benefits to student scholars. For more information, see http://www.lowell.edu/rsch/predoc.php and links therein. Applications for Fall 2011 are due by May 1, 2011. 145.10 POCA Update: An NSF PAARE Project Donald K. Walter1, S. D. Brittain2, J. L. Cash1, D. H. Hartmann2, S. B. Howell3, J. R. King2, M. D. Leising2, E. A. Mayo1, K. J. Mighell3, D. M. Smith, Jr.1 1South Carolina State Univ., 2Clemson University, 3National Optical Astronomy Observatory. Exhibit Hall We report on the status of “A Partnership in Observational and Computational Astronomy (POCA)” under the NSF's "Partnerships in Astronomy and Astrophysics Research and Education (PAARE)" program. This partnership includes South Carolina State University (a Historically Black College/University), Clemson University (a Ph.D. granting institution) and the National Optical Astronomy Observatory. We have reached the midpoint of this 5-year award and discuss the successes, challenges and obstacles encountered to date. Included is a summary of our summer REU program, the POCA graduate fellowship program, faculty research capacity building, outreach activities, increased use of NSF facilities and shared resources. Additional POCA research presentations by the authors are described elsewhere in these proceedings. Support for this work was provided by the NSF PAARE program to South Carolina State University under award AST-0750814 as well as resources and support provided by Clemson University and the National Optical Astronomy Observatory. 146 HAD III History Poster Papers Poster Session Exhibit Hall 146.01 Al-Sufi’s Investigation of Stars, Star Clusters and Nebulae Ihsan Hafez1, F. R. Stephenson1, W. Orchiston1 1James Cook University, Australia. Exhibit Hall The distinguished Arabic astronomer, Al-Sufi (AD 903-986) is justly famous for his Book of the Fixed Stars, an outstanding Medieval treatise on astronomy that was assembled in 964. Developed from Ptolemy’s Algamest, but based upon al-Sufi’s own stellar observations, the Book of the Fixed Stars has been copied down through the ages, and currently 35 copies are known to exist in various archival repositories around the world. Among other things, this major work contains 55 astronomical tables, plus star charts for 48 constellations. For the first time a long-overdue English translation of this important early work is in active preparation. In this paper we provide biographical material about Al-Sufi and the contents of his Book of the Fixed Stars, before examining his novel stellar magnitude system, and his listing of star clusters and nebulae (including the first-ever mention of the Great Nebula in Andromeda). 146.02 Kepler's “War on Mars” William Dorsey1, W. Orchiston1, F. R. Stephenson1 1James Cook University, Australia. Exhibit Hall This paper presents an interpretation of how Johannes Kepler changed the study of astronomy. We propose that in his metaphorical “War on Mars,” the Astronomia Nova, Kepler used a revolutionary rhetoric to bring about the usurpation of seventeenth-century astronomy. We discuss how Kepler approached the well-established conceptual framework within which the hypotheses of Ptolemy, Copernicus and Tycho Brahe functioned, and how he sought comprehensive physical principles that could determine the true cause and form of the known Universe. We examine Kepler’s need to redefine reality and his use of rhetoric in shaping his astronomical argument for a new astronomy, and we show that his new ‘laws’ represent a fusion of physics and geometry based upon astronomical observations. We suggest that although Kepler may have believed in and defended some Copernican ideas, his innovative Astronomia Nova opened up a whole new vista for international astronomy. 146.03 The First Three Catalogues of Southern Star Clusters and Nebulae Glen Cozens1, W. Orchiston1, A. Walsh1 1James Cook University, Australia. Exhibit Hall Nicolas de la Caille, James Dunlop and John Herschel compiled the first three catalogues of southern star clusters and nebulae. Lacaille catalogued 42 objects from Cape Town, South Africa, in 1751 and 1752. Dunlop catalogued 629 objects from Parramatta, Australia, in 1826 and Herschel catalogued 1708 objects between 1834 and 1838 from Cape Town. Many of these objects had not been seen before; In this paper we discuss the new discoveries and the accuracy of the positions supplied by Lacaille, Dunlop and Herschel. Half of Dunlop’s 629 objects turned out to be asterisms and faint double stars. 146.04 Early Scientific Astronomy on the American Northwest Coast: Captain Cook’s Sojourn at Nootka Sound in 1778 William Wells1, W. Orchiston2 1Retired Engineer, 2James Cook University, Australia. Exhibit Hall Between 1768 and 1778 England’s premier maritime explorer, James Cook, made three much-published and very successful expeditions to the Pacific, when important contributions were made to anthropology, botany and zoology, not to mention maritime astronomy. Astronomy played a vital role in navigation and coastal cartography, and consequently there were astronomers on all three Pacific expeditions. On the final voyage Cook would lose his life in Hawaii, but not before exploring the northwest coast of the American continent. Three astronomers, Bayly, King and Cook himself, formed part of retinue of this two-vessel expedition, and during the sojourn of the Resolution and Discovery at Nootka Sound they set up their observatories and used a variety of instruments to carry out important astronomical observations. In this paper we review the rationale for Cook’s third voyage, discuss the Nootka Sound stop-over, provide biographical information about Bayly, Cook and King, examine their scientific instruments and review their astronomical observations. 146.05 Williamstown Observatory and the Development of Professional Astronomy in Australia Jenny Andropoulos1, W. Orchiston1, B. Clark1 1James Cook University, Australia. Exhibit Hall During the early 1850s the colony of Victoria was enjoying a succession of gold rushes, and as the population of the fledgling settlement of Melbourne rapidly grew, an urgent need arose for an accurate local time service. Thus, Williamstown Observatory was founded at the port of Williamstown in 1853. Under the dynamic direction of Robert Ellery, the Williamstown Observatory quickly added meteorological and tidal observations, geodetic surveying and non-meridian astronomical observations to its portfolio, and by the time it closed in 1863 it had already played a key role in the early development of professional astronomy in Australia. Ellery went on to direct Melbourne Observatory_Williamstown’s successor_and in the process build an international reputation in astronomy, meteorology and scientific entrepeneurship. In this paper we will discuss the founding and chequered history of the Williamstown Observatory, its scientific instruments and the ways in which they were used to contribute to Australian and international astronomy. 146.06 The USNO 26'' Clark Refractor; From Visual Observations to Speckle Interferometry Jennifer L. Bartlett1, B. D. Mason1, W. I. Hartkopf1 1US Naval Observatory. Exhibit Hall Before addressing queries about how and what to preserve among astronomical devices, the question of what constitutes a historic instrument must be considered. Certainly, the lenses are the defining feature of a Clark refractor. Since 1867, when Newcomb inquired about the possibility of obtaining a great glass from Alvan Clark & Sons, the U.S. Naval Observatory 26-in (66-cm) equatorial has evolved in response to improvements in technology and changes in its observing program. After two major overhauls, only the objective remains of the equipment originally installed by the Clarks in 1873 at the old Observatory site in Foggy Bottom. However, the telescope retains its reputation as a historic Clark refractor. The USNO telescope was briefly renowned as the largest refractor in the world; the second of five such achievements by the Clarks. Through it, Hall first detected the moons of Mars in 1877. However, by that time, the Clarks had already refigured the flint glass. Hall and Gardiner had also altered the drive mechanism. When the USNO moved to its present Georgetown Heights location in 1893, the great equatorial was refurbished with its original Clark optics installed on a more robust Warner & Swasey mount. Peters eventually incorporated discarded parts from the original mounting into his photographic telescopes during the first half of the 20th century. The 26'' refractor underwent further modernization in the early 1960s to facilitate the xy-slide of a Hertzsprung-style photographic double star camera. In 1965, the objective was disassembled for cleaning and reassembled with new spacers. The most recent maintenance included re-wiring and replacing several motors and the hand paddles. Originally designed as a visual instrument, the USNO 26'' Clark refractor now hosts a speckle interferometer for its current double star program. Despite continuing modifications, this telescope remains a fine example of the optician's art. 146.07 The 1882 Transit of Venus and the Popularisation of Astronomy through the Pages of the New York Times Stella Cottam1, W. Orchiston1, F. R. Stephenson1 1James Cook University, Australia. Exhibit Hall After the disappointments of the 1761 and 1769 transits of Venus, the nineteenth century pair, in 1874 and 1882, offered astronomers the next opportunity to use these rare events in a bid to pin down a value for the solar parallax and hence that fundamental yardstick of Solar System astronomy, the astronomical unit. Only the 1882 transit was visible from the USA, and on the fateful day amateur and professional observers were scattered across the nation. While the value for the solar parallax derived from their combined observations was a significant improvement on the range of values obtained in the eighteenth century, there was considerable disquiet about the logic of using transits of Venus in this way when alternative approaches were available. In this paper we discuss some of the observers who observed the 1882 transit from American soil, summarise the scientific results from the overall American endeavour and examine ways in which reports on the transit in the pages of the New York Times helped generate a heightened public awareness of astronomy. 146.08 The IAU Early French Radio Astronomy Project Wayne Orchiston1, A. Boischot2, J. Delannoy2, M. Kundu3, J. Lequeux2, M. Pick2, J. Steinberg2 1James Cook University, Australia, 2Paris Observatory, France, 3University of Maryland. Exhibit Hall In 2006 an ambitious project was launched under the auspices of the IAU Working Group on Historic Radio Astronomy to document important developments in French radio astronomy from 1901 through to the 1960s, in a series of papers published, in English, in the Journal of Astronomical History and Heritage. This successful project has now come to an end with the sixth and final paper in the series about to be published (and a new WG project, on the history of early Japanese radio astronomy, has just been launched). In this paper we discuss Nordmann’s abortive attempt to detect solar radio emission in 1901, and the important roles played by staff from the École Normale Supérieure and the Institut d’Astrophysique in Paris during the 1940s through 60s in developing new radio astronomy instrumentation and pursuing a range of solar and non-solar research projects in Paris itself and at field stations established at Marcoussis, Nançay and the Haute Provence Observatory. 146.09 Van Vleck Observatory and the Role of the Large Refractor in Parallax Studies Ian Glass1, J. Griese, III1, W. Orchiston1 1James Cook University, Australia. Exhibit Hall The second half of the nineteenth century was the era par excellence of the ‘large refractor’ as the aperture of the world’s largest refractor quickly rose to 40 inches, thanks in no small part to the critical role played by the firm of Alvan Clark & Sons. One of the research projects these long focal length telescopes were especially suited to was the determination of stellar parallaxes, and this research focus continued into the twentieth century. In 1922 a 20-inch f/16.5 Clark refractor was installed at the Van Vleck Observatory at Wesleyan University in Middletown, Connecticut, and this telescope was used to determine stellar parallaxes that were subsequently published by van Altena, Lee, and Hoffleit in The General Catalogue of Trigonometric Stellar Parallaxes, Fourth Edition (1995). After providing background information on refractor construction and parallax studies during the nineteenth century this paper focuses on the Van Vleck Observatory parallax program, which continued through into the 1990s, by which time HIPPARCHOS had been launched. 146.10 The Contribution of an Experimental WWII Radar Antenna to Australian Radio Astronomy Wayne Orchiston1, H. Wendt1 1James Cook University, Australia. Exhibit Hall During the late 1940s and throughout the1950s Australia was one of the world’s foremost astronomical nations owing primarily to the dynamic Radio Astronomy Group within the Commonwealth Scientific and Industrial Organisation’s Division of Radiophysics. The earliest celestial observations were made with former WWII radar antennas and simple Yagi aerials, before more sophisticated purpose-built radio telescopes of various types were designed and developed. One of the recycled WWII antennas that was used extensively for pioneering radio astronomical research was an experimental radar antenna that initially was located at the Division’s short-lived Georges Heights field station but in 1948 was relocated to the new Potts Hill field station in suburban Sydney. In this paper we describe this unique antenna, and discuss the wide-ranging solar, Galactic and extragalactic research programs that it was used for. 146.11 History of Astronomy at James Cook University, Australia Wayne Orchiston1, H. Duerbeck1, I. Glass1, K. Malville1, B. Marsden1, I. Simonia1, B. Slee1, F. R. Stephenson1, R. Strom1, I. Whittingham1, R. Wielebinski1 1James Cook University, Australia. Exhibit Hall The Centre for Astronomy at James Cook University (JCU) in Australia has been offering totally internet-delivered Master of Astronomy degrees since 2003 and Doctor of Astronomy and Ph.D. degrees since 2004. In 2005 a new dimension was added with unique offerings in the history of astronomy at both Masters and Doctoral levels. With the aid of 1 full-time staff member and 10 adjunct staff, 4 students have now graduated with Ph.D. degrees, 1 student died from cancer after completing the first draft of his thesis, and 14 students are currently enrolled in Ph.D. degrees. In addition 12 students have completed Master of Astronomy degrees in history of astronomy, and there are 3 students who are currently enrolled for Masters degrees. As part of its commitment to the international development of history of astronomy, the Centre for Astronomy also arranges boutique ‘invitation only’ history of astronomy conferences in March each year, and produces the Journal of Astronomical History and Heritage. 146.12 Filling a Void: The Life and Times of the Journal of Astronomical History and Heritage Wayne Orchiston1, H. Duerbeck1, J. S. Tenn2 1James Cook University, Australia, 2Sonoma State University. Exhibit Hall In 1998 the Journal of Astronomical History and Heritage (JAH2) was launched as a new outlet for those wishing to publish papers on the history of astronomy. The journal has since developed rapidly and become an important publication venue for those conducting research in all fields of historical astronomy, including aspects of Asian and Oriental astronomical history. With support from a distinguished international Editorial Board, the journal has grown from two issues per year to three, and now features increasing numbers of colour pages. In this paper we review the founding and development history of the journal, examine the range of research and review papers that have been published since 1998, and discuss some of the possible future directions that we are currently exploring. 147 Dwarf Galaxies Poster Session Exhibit Hall 147.01 Simulating Cosmic Rays in the Large Magellanic Cloud Paul M. Ricker1, Y. Chu1, B. D. Fields1, R. Gruendl1 1Univ. of Illinois. Exhibit Hall Fermi observations of the Large Magellanic Cloud (LMC) strongly support the idea that cosmic-ray acceleration is associated with regions of ongoing massive star formation. Because it is so close, the LMC is well-resolved in a variety of wavebands, and existing observations place good constraints on its gas distribution and recent star formation history. These facts make the LMC an excellent validation case for the numerical models of cosmic rays used in galaxy cluster simulations. We present preliminary results from a project to incorporate cosmic-ray acceleration and transport into the FLASH adaptive mesh refinement (AMR) simulation code, with particular emphasis on the use of LMC observations to constrain the acceleration efficiency and diffusive length scales of cosmic rays. This research is supported by NASA under Fermi Guest Investigator grant NNX10AO78G. 147.02 Molecular Hydrogen Images of Star Forming Regions in the Magellanic Clouds Ronald G. Probst1, R. Barba2, A. Bolatto3, Y. Chu4, S. Points5, M. Rubio6, C. Smith5 1NOAO, 2Universidad de La Serena, Chile, 3University of Maryland, 4University of Illinois, 5NOAO, Chile, 6Universidad de Chile, Chile. Exhibit Hall The Large and Small Magellanic Clouds exhibit a variety of star formation physics with multiple phase components in low metallicity, gas rich environments. The ~10 K, ~100 K, and ~104 K regimes are well explored. We are imaging LMC and SMC star forming regions in 2.12 micron H2 emission which arises in the ~1000 K transition zone of molecular clouds. This is an NOAO Survey program using the widefield IR camera NEWFIRM on the CTIO 4-m Blanco telescope during its limited southern deployment. The data set will have immediate morphological applications and will provide target selection for followup infrared spectroscopy. We will provide a public archive of fully calibrated images with no proprietary period. NOAO is operated by the Association of Universities for Research in Astronomy, under cooperative agreement with the National Science Foundation. 147.03 The Large Magellanic Cloud In The Sdss And Lcdm: Is There A "Found Satellites Problem"? Erik J. Tollerud1, E. J. Barton1, J. S. Bullock1, C. Trinh2, M. Boylan-Kolchin1 1University of California Irvine, 2University of Sydney, Australia. Exhibit Hall Substructure in LCDM provides a number of interesting puzzles. While the missing satellites problem is well-studied, there are suggestions of an opposite problem on the bright end. Subhalos large enough to host luminous satellites are uncommon, so we investigate whether the existence of the Large Magellanic Cloud (LMC) orbiting the Galaxy is a challenge for LCDM. We construct a volume limited sample of isolated galaxies in the Sloan Digital Sky Survey (SDSS) within which all LMC analogs would be visible. We search this sample for analogs to an isolated galaxy pair like the Milky Way/LMC system and interpret these results with cosmological simulations. We find that a significant fraction of Milky Way-like hosts host LMC-like satellites, closely matching the predictions of n-body simulations. However, we find that the LMC is remarkably blue for such satellites. This could imply that the LMC is on first infall as recent proper motions suggest. 147.04 The Chemical Composition Of Ultra-faint Dwarf Galaxies Anna Frebel1, J. D. Simon2, E. N. Kirby3 1Harvard-Smithsonian Center for Astrophysics, 2Carnegie Observatory, 3Caltech. Exhibit Hall We present recent high-resolution spectroscopic observations of extremely metal-poor stars located in the ultra-faint dwarf galaxies Ursa Major II, Coma Berenices, Leo IV, Segue 1 and Bootes II. Their chemical abundance patterns resemble those found in halo stars of comparable metallicty, suggesting that chemical evolution was universal, at least in the very low-metallicity regime, before the onset of SN Ia. This chemical similarity lends support to the idea that systems like the surviving dwarfs played a significant role in the assembly of (at least) the metal-poor outer halo of the Galaxy. 147.05 Observations of Dwarf Galaxies in Several Photometric Systems Joanne D. Hughes1, R. Leaman2, K. McCormick1, A. Hankins1 1Seattle Univ., 2University of Victoria, Canada. Exhibit Hall Using the SPIcam imager at the Apache Point 3.5-m telescope, we have observed the ultra-faint dSph, UMa II (d~30 kpc), and the WLM dIrr galaxy (d~ 930 kpc) in Washington and Strömgren filters. UMa II is a nearby metal-poor system ([Fe/H]~-2.5), within the dark matter halo of the Milky Way, with few red giant branch stars above the horizontal branch. Previous spectroscopic studies have confirmed that UMa II is old (~12 Gyr), contains some stars more metal-poor than [Fe/H]=-3.0, and has a ~1.0 dex metallicity spread. The WLM Galaxy is more metal rich (mean [Fe/H]~ -1.3) than UMa II, with the bright RGB population being dominated by young and relatively more metal-rich stars. There is a metallicity gradient within the WLM dIrr, with the inner-galaxy population being at least 0.3 dex more metal rich ([Fe/H]~ -1.1) than the outer halo ([Fe/H]~ -1.4). We present our new imaging data and compare the stellar population color-magnitude diagrams with theoretical models to determine the best photometric methods of quantifying metallicity spreads in these diverse populations. We show that photometric metallicities can be determined to ~0.2 dex for bright RGB stars and to ~0.15 dex for well-defined giant branches. We acknowledge support from NSERC Discovery Grants and the M.J. Murdock Charitable Trust. 147.06 Clustering of Milky Way Dwarf Galaxies Brandon Bozek1, R. F. G. Wyse1, G. F. Gilmore2 1Johns Hopkins University, 2Institute of Astronomy, University of Cambridge, United Kingdom. Exhibit Hall The distribution of Milky Way Dwarf Galaxies has been suggested to contain anisotropic subsets of 'ghostly streams' and groups or even to be distributed in a flattened 'Disk of Satellites'. Recent surveys have facilitated the discovery of larger numbers of satellites and we investigated their distribution using a suite of clustering estimators. We also applied the same analysis to the Via Lactea II dark matter simulation and several subsamples selected following recent suggestions. We consider both all dwarf galaxies within 260 kpc and a subset of only those found within the northern contiguous portion of the SDSS DR7 Legacy Footprint. We will present our results and discuss their interpretation. 147.07 The Dwarf Galaxy Population of the M81 Group Kristin Chiboucas1, B. A. Jacobs2, I. D. Karachentsev3, R. B. Tully2 1Gemini Observatory, 2University of Hawaii, 3Special Astrophysical Observatory, Russian Federation. Exhibit Hall In a CFHT/Megacam imaging survey of the M81 Group to search for the smallest dwarf galaxies, we identified 22 new candidate dwarf galaxies. Follow-up HST ACS and WFPC2 imaging in F814W and F606W bands was used to produce color-magnitude diagrams down to 1.5-3 mag below the tip of the red giant branch. From tip of the red giant branch distances, we establish 14 out of the 22 candidates as bona-fide group members, including 3 blue compact dwarfs, 1 likely tidal dwarf, and a dwarf spheroidal galaxy as faint as MR = -6.9. The latter is within the domain of the ultra-faint dwarf galaxies recently discovered in the Local Group. As the original survey extended out to the group second turnaround radius, and based on detection limits determined from simulations, we believe our sample of M81 group galaxy members is largely complete down to MR = -9.5. We discuss the properties of the M81 Group dwarf galaxy population. 147.08 Nearby Dwarf Galaxies in VLA-ANGST: an Exploration of HI Velocity Dispersion Adrienne Stilp1, J. Dalcanton1, J. Ott2, S. Warren3, D. Weisz1 1University of Washington, 2National Radio Astronomy Observatory, 3University of Minnesota. Exhibit Hall The interplay between star formation and the interstellar medium (ISM) is critical for shaping the baryonic component of galaxies. We probe the present-day structure of the ISM through neutral hydrogen (HI) observations of nearby dwarf galaxies from the Very Large Array ACS Nearby Galaxy Survey Treasury (VLA-ANGST) Project, complemented by extensive HST imaging from ANGST that allows us to accurately constrain the recent star formation histories of these galaxies on spatial scales of ~100 pc. We find a clear lower limit to the HI velocity dispersion in every sample galaxy. We explore the possible causes of this limit by examining its properties at varying surface densities as well as any potential correlation with star formation in the last 500 Myr. 147.09 Connecting HI Kinematics and Physical Processes in Dwarf Galaxies' ISM Sean Markert1, A. Stilp1, J. Dalcanton1, T. Quinn1, F. Governato1 1University of Washington. Exhibit Hall We present a comparison of the HI velocity dispersion in cosmological simulations of dwarf galaxies to the VLA-ANGST sample of observed dwarfs. The observations show a clear lower limit to the velocity dispersion in these galaxies. Using state-of-the-art simulations we explore the physical processes that could cause this limit, such as feedback from star formation and effects of gas temperature. We then use the simulations to show the impact these processes have on the interstellar medium in our sample of observed dwarfs. 147.10 The Cold ISM of Low Metallicity Galaxies Steven R. Warren1, E. Skillman1, A. Stilp2, J. Ott3, J. Dalcanton2, F. Walter4 1University of Minnesota, 2University of Washington, 3NRAO, 4Max Planck Institut für Astronomie, Germany. Exhibit Hall Star formation occurs primarily within molecular clouds, and the raw material for molecular cloud formation is the reservoir of neutral hydrogen (HI) gas present in star forming galaxies. Thus, understanding how and where the HI is converted into molecular gas is a key step in our understanding of the star formation process. At low metallicities, the key tracer of molecular gas, CO, is not detected. Identifying narrow line HI emission (e.g., Young et al. 1996, 1997) provides a potential tracer of the molecular phase by tracing the cold HI gas . The cold HI is believed to be a necessary phase in converting the ubiquitous warm HI gas into cold molecular gas. In the current study, we have characterized the locations of narrow HI emission through ine-of-sight spectra of HI line maps taken from the Very Large Array - ACS Nearby Galaxy Survey Treasury (VLA-ANGST) and The HI Nearby Galaxy Survey (THINGS) projects. We detect narrow HI emission in every galaxy surveyed where the signal to noise in a given spectrum is high enough (~15-20) to provide statistically viable fits. The detected narrow HI emission constitutes ~1-20% of the total surveyed HI in a given galaxy. The locations of the cold HI gas can be compared with tracers of recent star formation to better understand the star formation process. 147.11 Star Formation and Integrated Optical Colors from the Local Volume Legacy Survey Cody Minns1, B. R. Shackleford1, L. van Zee1, S. Friberg2, K. L. Barnes1, S. Sakai3, LVL Team 1Indiana University, 2University of Massachusetts, 3University of California. Exhibit Hall We present results of an optical imaging study of 73 galaxies from the Spitzer Local Volume Legacy (LVL) survey. The broadband and narrowband optical images were analyzed in order to determine information about global star formation rates, histories, and evolution of these nearby galaxies. The observed UBVR colors are consistent with the expected colors of star forming galaxies, with B-R colors ranging from 0.4 to 1.4. The blue, low mass galaxies appear to have a wider dispersion of current-to-past star formation rates than the more massive spiral galaxies in the sample. These results are discussed in the context of possible star formation histories for galaxies in the Local Volume. 147.12 Optical Color and Equivalent Width Gradients in the Local Volume Legacy Survey Bryce Shackleford1, C. R. Minns1, L. van Zee1, S. Friberg2, K. L. Barnes1, S. Sakai3, LVL Team 1Indiana University, 2University of Massachusetts, 3University of California. Exhibit Hall We present the results of B, R, and H alpha optical imaging of a subsample of galaxies from the Spitzer Local Volume Legacy Survey. The images were analyzed using a set of concentric, co-eccentric ellipses to measure surface brightness profiles and color gradients. While most of the galaxies in this sample have modest to negligible color gradients, some of the galaxies have B-R color gradients greater than 0.4 mag/kpc. Furthermore, the range of values measured for the B-R color gradient is larger for galaxies with absolute magnitudes fainter than -16. Likewise, the scatter in the observed equivalent width gradient is larger for the low mass irregular galaxies. The increased range of observed color gradients in the low mass galaxies may be related to a transition in the dominant mechanisms that regulate star formation in dwarf irregular and spiral galaxies. 147.13 Stellar Mass Distributions in Dwarf Irregular Galaxies Hongxin Zhang1, D. Hunter1, LITTLE THINGS Team 1Lowell Observatory. Exhibit Hall We present the radial distributions of the stellar mass and the star formation histories for a large sample of dwarf irregular galaxies assembled by the LITTLE THINGS project (Local Irregulars That Trace Luminosity Extremes The HI Nearby Galaxy Survey, http://www.lowell.edu/users/dah/littlethings/index.html). Specifically, utilizing the multi-band data including FUV/NUV/UBV/H?/3.6?m, and with the CB07 stellar population synthesis models, we analyze the variations of the SEDs as a function of radius. By studying the relationship between the stellar mass, star formation histories, star formation and HI gas, we will discuss the possible star formation modes and the roles played by the stellar mass and gas in determining the star formation in dwarf irregular galaxies in general. We gratefully acknowledge funding for this research from the National Science Foundation (AST-0707563). 147.14 Gas, Stars, and Star Formation in Extreme Outer Disks of Dwarf Galaxies Deidre Ann Hunter1, S. Oh2, B. Elmegreen3 1Lowell Obs., 2University of Cape Town, South Africa, 3IBM T.J. Watson Research Center. Exhibit Hall We compare deep optical images, deep ultraviolet images obtained with GALEX, and HI interferometric maps of five dwarf irregular galaxies in order to examine star formation in their outer disks. The V-band surface photometry, which extends to 29-30 mag/arcsec-squared, averages the star formation activity over the past Gyr for on-going star formation. The GALEX ultraviolet data provides information on star formation over the past 200 Myrs. The HI maps and cubes yield information on the gas surface densities and kinematics. We deconvolve the ordered rotation from non-ordered motions of the gas and compare with the stellar populations. This research has been funded by the Lowell Research Fund and by NASA/GALEX grant NNX08AL66G. 147.15 Broken Surface Brightness Profiles in Dwarf Galaxies Kimberly A. Herrmann1, D. A. Hunter1, H. X. Zhang1, LITTLE THINGS Team 1Lowell Observatory. Exhibit Hall Recently it has been well shown that there are three different surface brightness profile types in spiral galaxies: (I) the minority, where the light falls off with a single exponential; (II) truncated, the majority, where the light falls off with one exponential to a break radius and then falls off more steeply; and (III) anti-truncated, where the light falls off with a more shallow exponential beyond the break radius. Additionally, Bakos, Trujillo, & Pohlen (2008) showed that each type has a characteristic color trend with respect to the break location. In dwarf disk galaxies, however, there is a fourth type which is perhaps a special Type II case: the light profile is flat on the inside and then falls off exponentially beyond the break radius. We will show the different color trends for these four profile types from a large photometric study of dwarf disk galaxies and explore the ramifications of the differences between spirals and dwarfs. We gratefully acknowledge funding for this research from the National Science Foundation (AST-0707563). 147.16 Spectroscopic Properties of Newly Discovered H? Dots Jesse Feddersen1, J. J. Salzer1, A. Williams1, C. Gronwall2 1Indiana University, 2Pennsylvania State University. Exhibit Hall We present newly discovered faint point sources of emission - called H? dots - found in narrow-band images taken for the ALFALFA H? project. These images target ALFALFA survey galaxies for the purpose of measuring their star-formation characteristics. Our image analysis turns up a large population of serendipitously discovered emission-line sources that are not associated with the target ALFALFA galaxy. In addition to presenting several dozen new objects, we have acquired and reduced spectral data for nearly all of the sample. These spectra reveal a mix of isolated extragalactic HII regions, ultra-low luminosity dwarf galaxies, background (higher redshift) galaxies, and QSOs. We present examples of several H? dots along with their follow-up spectroscopy, and give a summary of the properties of the full sample of H? dots discovered to date. We also illustrate why these objects are of astrophysical interest. For example, this selection method appears to provide a rich sample of nearby, very low metallicity dwarf systems, as well as luminous [O III]-detected star-forming galaxies at z ~ 0.32 with unusually low abundances. 147.17 The Detectability of Stealth Galaxies Maya Barlev1, B. Willman1, R. Fadely1 1Haverford College. Exhibit Hall The 2008 discovery of dwarf galaxy And XIX (MV = -9.3, rh ~ 1.7 kpc) around M31 raised the question of whether such large scale size systems could exist around the Milky Way but have evaded previous searches. Since then, the existence of yet-unseen "stealth" galaxies around the Milky Way - dwarfs with larger scale sizes and lower surface brightnesses than those currently known - has independently been predicted as a way to understand the apparent common mass scale of dwarf galaxies. To quantify the unexplored stealth galaxy parameter space around the Milky Way, we investigate the detectability of large scale length (rh > 1 kpc) dwarf galaxies in the Sloan Digital Sky Survey dataset. We do this by i) simulating dwarf galaxies based on a Dotter isochrone of an old, metal-poor stellar population, ii) inserting simulated galaxies into the SDSS point source catalog, and iii) applying a standard search algorithm to the resulting catalog. 148 Elliptical Galaxies Poster Session Exhibit Hall 148.01 The Dynamical State of the Telescopium Galaxy Group - Deep Chandra Observations of NGC 6868 and NGC 6861 Kimberly Ward-Duong1, S. W. Randall2, M. E. Machacek2 1Northern Arizona University, 2Harvard-Smithsonian Center for Astrophysics. Exhibit Hall We present results from deep Chandra observations of NGC 6868 and NGC 6861, the two dominant elliptical galaxies in the Telescopium galaxy group (Abell S0851). We examine the diffuse gas in and around these galaxies to establish the possible interactions occurring within the group. Surface brightness images exhibit bright edges and tails, which indicate that the galaxy group is not dynamically relaxed. Spectral analysis reveals a spiral of cool gas with an associated cold front edge in NGC 6868, indicative of gas sloshing initiated by a passing galaxy or subgroup. NGC 6861 shows bright, swept back arms and a broad tail of emission, both to the northwest, suggesting that it is being ram pressure stripped due to interactions with a diffuse intracluster medium as it moves to the southeast. We find evidence that the arms are composed of cool gas originating from the galaxy core, and propose that, as seen in other systems, they may be filaments that have been buoyantly lifted by putative radio lobes inflated by the central AGN. Our results are consistent with previous suggestions that NGC 6868 and NGC 6861 are the central dominant members of two distinct subgroups, which are currently merging to form the Telescopium galaxy group. This work is supported in part by the NSF REU and DOD ASSURE programs under NSF grant no. 0754568, by Chandra grant GO0-1009X issued under NASA contract NAS8-03060, and by the Smithsonian Institution. 148.02 Hi Content Of X-ray Faint Early Type Galaxies And Its Influence On Abundance Yuanyuan Su1, J. Irwin1 1University of Alabama. Exhibit Hall There is a growing body of evidence suggesting that field elliptical galaxies have larger HI halos around them, while elliptical galaxies near the centers of clusters have had their HI haloes destroyed. We compared galaxies with comparable low X-ray gas luminosity, some with HI haloes and some lacking HI haloes with Chandra, XMM and Suzaku archived observations. We found that galaxies with HI haloes (e.g. NGC 4278) has a low abundance for hot gas, while galaxies lacking HI haloes (e.g. NGC 4382) have high abundance for hot gas. We therefore interpret the measured very low abundance of X-ray faint galaxies as a result from the dilution of the remaining hot gas by this pristine HI gas.  148.03 Ionized Gas in E/S0 Galaxies with Dust Lanes Jose G. Funes, S.J.1, I. Finkelman2, N. Borsch2, P. Vaisanen3, A. Kniazev3 1Specola Vaticana, Italy, 2The Wise Observatory and the School of Physics and Astronomy, Israel, 3South African Astronomical Observatory, South Africa. Exhibit Hall We present results from an ongoing program to study the properties of dust and ionized gas in E/S0 galaxies with dust lanes. Our observational program comprises of H-alpha and broad-band images obtained with the SAAO 1.9m, the VATT 1.8m and the 1m telescope on WO. A detailed analysis of 30 galaxies shows the presence of a diffusely distributed ionized gas component in most objects. The extended gas morphology is typically smooth and closely follows the dust structure, with a clear correlation between the mass of both components. The dust content in each galaxy is estimated by measuring the extinction by the extragalactic dust in the dark lanes. The derived extinction law is used to correct the measured colors for intrinsic dust extinction and the data are fitted with a stellar population synthesis model. We find that the line-emission and colors of most objects are consistent with the presence of an “old” stellar population (~10 Gyr) and a small fraction of a “young” population (~10? 100 Myr). The younger stellar population may have formed at a later stage of the evolution of the galaxy through either a merger event or a secondary star-formation burst. Strong evidence for the external origin of the ISM is provided by the apparent inclination of the dust and ionized gas disks with respect to the galactic plane in a large fraction of our sample galaxies. Further spectroscopic observations will be obtained to study the gaseous disks dynamics and to characterize the underlying stellar populations for evidence of multiple phases of star formation and assembly history. 148.04 Gas Accretion in the M32 Nucleus: Past & Present Anil Seth1 1Harvard-Smithsonian CfA. Exhibit Hall Using adaptive optics assisted Gemini/NIFS data, I study the present and past gas accretion in the central 3" of the M32 nucleus. From changes in the spectral slope and CO line depths near the center, I find evidence for unresolved dust emission resulting from BH accretion. With a luminosity of 2e38 ergs/s, this dust emission is the most luminous tracer of current BH accretion. These observations suggest that using high resolution infrared data to search for dust emission may be an effective way to detect other nearby, low luminosity BHs, such as those in globular clusters. I also examine the fossil evidence of gas accretion contained in the kinematics of the stars in the nucleus. The higher-order moments (h3 and h4) of the line-of-sight velocity distribution show patterns that are remarkably similar to those seen on larger scales in elliptical galaxies and in gas-rich merger simulations. The kinematics suggests the presence of two components in the M32 nucleus, a dominant disk overlying a pressure supported component. I suggest a scenario, in which the nuclear disk formed gradually from the stellar winds of stars in the bulge of M32, that may provide a good explanation of the observed kinematics, stellar populations and abundance gradients seen in the nucleus. The kinematic measurements presented here are the highest quality available for the nucleus of M32, and may be useful for any future dynamical models of this benchmark system. 148.05 Supermassive Black Hole Activity Within Local Early-type Galaxies Brendan P. Miller1, E. Gallo1, T. Treu2 1University of Michigan, 2University of California, Santa Barbara. Exhibit Hall We report preliminary results from an ongoing Chandra survey of 100 field early-type galaxies. This project investigates the influence of environment upon supermassive black hole (SMBH) accretion within formally inactive galaxies. The volume-limited sample has been selected to be well-matched to the recently conducted AMUSE-Virgo survey, which studied SMBHs within cluster early-type galaxies. That work resulted in the detection of nuclear X-ray sources in 32/100 objects, establishing a firm lower limit of 24-34% to the SMBH occupation fraction of normal galaxies, and found the average Eddington-scaled X-ray luminosity to be a decreasing function of SMBH mass, evidence for accretion "downsizing" (Gallo et al. 2008, 2010). Galaxies in more isolated environments have distinct properties that might influence the rate of SMBH fueling. Relative to cluster sources, field early-type galaxies have a lower probability of mergers; they also likely retain a larger fraction of hot gas (due to reduced ram-pressure stripping) and apparently contain more cold gas and tend to have younger stellar populations. The X-ray detection fraction of the field early-type galaxies is found to be comparable to that of the AMUSE-Virgo survey. We correlate the average Eddington-scaled X-ray luminosity with SMBH mass for the observed objects and compare the relation to that found for cluster galaxies. We also calculate the rate of off-nuclear X-ray sources and discuss implications for X-ray binary populations within field early-type galaxies. 148.06 Components of GALEX-Detected Star Formation in and around E and S0 Galaxies Lea Zernow1, J. Ryon2, B. F. Madore1, M. Seibert1, D. Neill3 1Carnegie Observatories, 2University of Wisconsin - Madison, 3California Institute of Technology. Exhibit Hall We present the first results of an investigation into ongoing star formation within E and S0 galaxies, selected from optical catalogs to be on the red sequence. Star formation in these spheroidal systems is traced using ultraviolet imaging from GALEX. We have identified a wide variety of unanticipated sites of apparent star formation in this sample, which include clumps, rings, and other structures. In order to quantify the contributions of these structures to the total UV flux, we have fit Sersic and/or exponential disk profiles to a subsample of 500 galaxies with high S/N, and compared the residuals of these smooth component fits to the original galaxy. 148.07 Star Formation in Brightest Cluster Galaxies Aaron Scott Hoffer1, M. Donahue1, A. Hicks1, R. Barthelemy1 1Michigan State University. Exhibit Hall We present Spitzer and GALEX spectral energy distributions (SEDs) for a sample of brightest cluster galaxies (BCGs). The BCG sample was selected from the Chandra archive, to have uniformly and well-measured X-ray cluster gas profiles for temperature, density, and entropy (Cavagnolo et al. 2009). The galaxy SEDs include data from GALEX [124 galaxies] , 2MASS [202 galaxies], and Spitzer IRAC [108 galaxies] and MIPS [83 galaxies]. These spectral energy distributions are fit to Siebenmorgen and Krügel (2006) starburst galaxy models in the IR and Groves et al. (2008) star formation models which span the IR through the UV, as well as an SED for an old stellar population. This sample provides a good baseline for the colors to expect from a quiescent BCG, since this sample includes BCGs that do not inhabit cool core clusters. We confirm the trend for BCGs in systems with low central hot gas entropy to have UV and mid-IR emission in excess over that expected from a quiescent BCG. We compare the star formation signatures in the BCGs with those from star-forming and starburst galaxies and find that their IR/UV ratios are similar to other star-forming galaxies, while their FUV-NUV colors might be somewhat bluer. 148.08 An Integral Field View of Early-Type Galaxies in the Coma Cluster Nicholas Scott1, R. Houghton1, R. L. Davies1, N. Thatte1, M. Cappellari1, F. Clarke1, L. Fogarty1, M. Tecza1 1University of Oxford, United Kingdom. Exhibit Hall We present Integral Field Unit (IFU) observations of a sample of 14 early-type galaxies (ETGs) in the Coma Cluster with Oxford's Short Wavelength Integral Field specTrograph (SWIFT) on the 200" Hale Telescope at Palomar. SWIFT is an i- and z-band IFU with R ~2 Å (? ~ 35kms-1). Our sample was selected to evenly sample the full range in velocity dispersions of giant ETGs in the cluster (90km/s to 400km/s). The observations were taken using the 0.235" scale giving a field of view of 11" x 22", covering most galaxies out to one Re. We extract stellar kinematics from the Calcium Triplet (CaT, observed at ~8800 Å) using pPXF (Cappellari & Emsellem, 2004) and present velocity and velocity dispersion maps for each of the galaxies in the sample. Using our IFU observations combined with SDSS and, where available, HST photometry we derive: Re, Ie, and ?e and from these determine the Fundamental Plane of Coma ETGs. In the near future, we plan to study the fast rotator/slow rotator ratio in Coma, one of the densest and richest local environments for ETGs, to compare with the latest results from the volume limited ALTAS3D survey which lacks such high densities. 149 Galaxy Clusters Poster Session Exhibit Hall 149.01 Population Analysis of Seyfert Galaxies in the Coma-Abell 1367 Supercluster Megan Jones1, E. Wilcots1 1University of Wisconsin-Madison. Exhibit Hall We study the population galaxies in groups along the Coma- Abell 1367 supercluster to study the occurrence of Seyfert galaxies. Within this population, we identified ~5% of the galaxies as Seyferts and found that ~40% of the groups contain at least one Seyfert. Only a small fraction of groups contain more than one Seyfert. We report on the distribution of Seyfert galaxies as a function of environment across the supercluster and probe the characteristics of the population of groups that currently host at least one Seyfert. In particular we correlate the properties of the population of Seyferts galaxies with the HI content of groups as derived in the ALFALFA survey. 149.02 The Galaxy Alignment Effect in Abell 1689 Li-wei Hung1, E. Bañados2, R. De Propris3, M. J. West4 1The Ohio State University, 2P. Universidad Católica de Chile, Chile, 3Cerro Tololo Inter-American Observatory, Chile, 4European Southern Observatory, Chile. Exhibit Hall We examined alignments for galaxies in the galaxy cluster Abell 1689 (z = 0.18) based on archival Hubble Space Telescope WFPC2 F606W and F814W images. The sources were extracted using SExtractor. We used distance from the color-magnitud relation (defined by the bright galaxies) as a proxy to select likely cluster members. We carried out a series of simulations with artificial galaxies in order to understand the limit of our position angle measurement. Based on the cluster member selection and the result of our simulations, we isolated a sample of galaxies lying on the red sequence with I < 24 and e > 0.2 to study the alignment effect. By applying the Kuiper test, we find evidence of alignment among faint galaxies and galaxies in the inner 500 kpc of the cluster. The best mechanism to produce this alignment result is tidal torquing. Akin to the Earth-Moon system, tidal effects would (re)create alignments between galaxies. Under the presence of the tidal field, fainter galaxies, especially in the center, will align themselves more rapidly than brighter galaxies. 149.03 Galaxy Alignment In Low-Redshift Abell Clusters Wayne Barkhouse1, M. Byrd1, O. Lopez-Cruz2 1Univ. of North Dakota, 2INAOE, Mexico. Exhibit Hall We present an analysis of the alignment effect of galaxies extracted from a sample of 57 low-redshift (0.04 < z < 0.20) Abell clusters. Galaxies have been selected with respect to their color, luminosity, and distance from the cluster center. We investigate possible correlations between the orientation of cluster galaxies and various properties of the host cluster (e.g., optical richness, BM-type, and X-ray luminosity). Understanding the relationship between cluster galaxies and their local environment, will help to uncover details about galaxy formation and evolution in these dense systems. 149.04 Power Spectrum Analysis of Faraday Rotation Measure in the Intracluster Medium Gary Foreman1, P. Ricker1 1University of Illinois, Urbana-Champaign. Exhibit Hall For conduction to be an efficient method for heating the cores of galaxy clusters, magnetic fields must be randomized within the central region of the intracluster medium (ICM). The heat-flux-driven buoyancy instability (HBI) tends to align magnetic fields azimuthally and shut off conduction; however, turbulence from mergers and galactic wakes may be enough to restore random orientations. One method for quantifying such randomness is through Faraday rotation measure mapping, which may be achieved using high resolution polarization measurements of the cosmic microwave background (CMB). In anticipation of such measurements, we present a statistical analysis of power spectra from numerically modeled rotation measure maps. We initialize a spherically symmetric galaxy cluster in hydrostatic equilibrium based on observed parameters of Abell 1060, and we generate rotation measure maps from randomly oriented, flux-frozen, divergence-free magnetic fields. 149.05 Evolution of the ICM Magnetic Fields from AGNs Hao Xu1, H. Li1 1Los Alamos National Lab. Exhibit Hall Radio observations suggested micro Gauss magnetic fields permeating the Intra Cluster Medium (ICM) in the galaxy clusters. Theory and simulations suggest that magnetic fields from Active Galactic Nucleus (AGNs) powered by their central super massive black holes can be an important source of these magnetic fields in the ICM. We present cosmological Adaptive Mesh Refinement (AMR) magnetohydrodynamic (MHD) simulations following the cluster formation and evolution of magnetic fields originally injected by AGN. We have performed simulations of a suite of galaxy clusters with virial masses ranging from 1 × 1014 to 2 × 1015 M?. In most clusters, the injected magnetic fields can be transported throughout the whole cluster and be further amplified by the ICM turbulence to micro Gauss level. The magnetic field strength and total energy are dependent on the sizes of the clusters, while the amplification processes of the magnetic fields are determined by the cluster merger history. We will demonstrate how the ICM MHD turbulence is excited and sustained by the frequent mergers during the cluster formation. We will discuss the small-scale dynamo processes and their relations to the ICM turbulence in different clusters. We will also present the distributions of magnetic fields and Synthetic Faraday rotation measurement (FRM) of our simulated clusters. This work was supported by the DOE/OFES via the Center for Magnetic Self-Organization and the LDRD program at LANL. 149.06 Mid Infrared Selected AGN in Galaxy Clusters From 0 < z < 1.2 Adam Tomczak1, K. Vy-Tran1, A. Saintonge2 1Texas A&M University, 2University of Zurich, Switzerland. Exhibit Hall We conduct a mid-infrared census of nine galaxy clusters with a total of 1517 spectroscopically confirmed member galaxies. Mid-IR color selection techniques were applied to identify active galactic nuclei (AGN) using Spitzer IRAC photometry. We find 12 candidate IR-AGN from a total of 712 cluster galaxies that have ?3? detections in all IRAC channels. To compare AGN activity across our redshift range we select three types of complete samples of galaxies: (1) galaxies with rest-frame [3.6]?m luminosity >1.3 × 1044 erg s-1, (2) a sample of the 100 brightest [3.6]?m galaxies and (3) galaxies with absolute VAB magnitude <-21.5. For all three samples we observe a tendency for the fraction of IR-AGN in cluster galaxies (fAGN) to increase with redshift. We observe the most rapid change between z ? 1.2 and 0.8 where fAGN drops from ~15±8% to ~3±2%, a time-span of ~1.5 Gyr. In general we find fAGN ? 1±1% at z < 0.7 but at z > 0.7 we calculate fAGN ? 5±2%. The mid infrared AGN fraction for field galaxies in the Spitzer Extragalactic First Look Survey(XFLS) is ~7±1% at z < 0.7 for galaxies with [3.6]?m ? 100 ?Jy. In agreement with recent studies, we find that IR-AGN are predominantly hosted by late-type galaxies that preferentially occupy the blue-cloud. We further observe that the most luminous IR-AGN from our sample (a) are accompanied by X-ray emission, (b) are located ?0.5 Mpc from the cluster center and (c) appear highly morphologically disturbed. These results support a scenario where X-ray-luminous AGN likely result from interactions/mergers of galaxies during infall into the cluster potential, simultaneously boosting the mid-IR signature. 149.07 Measuring the Effects of AGN Activity on the Intergalactic Medium Hanna Herbst1, K. Hess1, E. Wilcots1 1UW Madison Astronomy Dept.. Exhibit Hall Our current understanding of the formation and evolution of galaxy groups and clusters is impeded by a major problem. Models of gravitational collapse predict that the cores of galaxy groups should have had sufficient time to cool, but no observations have shown evidence of the cool gas that should reside in the cores. This means there must be some source of non-gravitational energy that is heating the intergalactic medium (IGM) and hindering the cooling flows. The two most likely sources are starburst driven galactic outflows or galactic outflows from active galactic nuclei (AGN). Here, we study AGN powered galactic outflows in NGC 1052 and NGC 741 as a possible source of the excess non-gravitational heating seen in x-ray observations. VLA data is used to estimate the total output of the radio jets, which is then compared the observed x-ray luminosity of the IGM, in order to determine to what extent AGN outflows could be responsible for the heating of the IGM. 149.08 Brightest Cluster Galaxy Identification Luke Leisman1, D. B. Haarsma1, D. A. Sebald1, ACCEPT team 1Calvin College. Exhibit Hall Brightest cluster galaxies (BCGs) play an important role in several fields of astronomical research. The literature includes many different methods and criteria for identifying the BCG in the cluster, such as choosing the brightest galaxy, the galaxy nearest the X-ray peak, or the galaxy with the most extended profile. Here we examine a sample of 75 clusters from the Archive of Chandra Cluster Entropy Profile Tables (ACCEPT) and the Sloan Digital Sky Survey (SDSS), measuring masked magnitudes and profiles for BCG candidates in each cluster. We first identified galaxies by hand; in 15% of clusters at least one team member selected a different galaxy than the others.We also applied 6 other identification methods to the ACCEPT sample; in 30% of clusters at least one of these methods selected a different galaxy than the other methods. We then developed an algorithm that weighs brightness, profile, and proximity to the X-ray peak and centroid. This algorithm incorporates the advantages of by-hand identification (weighing multiple properties) and automated selection (repeatable and consistent). The BCG population chosen by the algorithm is more uniform in its properties than populations selected by other methods, particularly in the relation between absolute magnitude (a proxy for galaxy mass) and average gas temperature (a proxy for cluster mass). This work supported by a Barry M. Goldwater Scholarship and a Sid Jansma Summer Research Fellowship. 149.09 The Hoag’s Object, UGC 4599 and NGC 6028: Other Examples of Star Forming Rings Shannon MacKenzie1, A. Pipino2, R. Rich2, C. Martin3, GALEX Team 1University of Louisville, 2University of California Los Angeles, 3California Institute of Technology. Exhibit Hall We study a sub-sample of Brightest Cluster Galaxies (BCGs) drawn from the Szabo et al. SDSS cluster catalogue, by selecting those in the richest clusters which also have a Galex counterpart and are at redshifts 0.1-0.4. Our multiwavelength approach allows us to study recent episodes of star formation witnessed by the UV-optical colours, as a function of the host cluster properties. In particular, we present a sample of blue BCGs in likely cool-core clusters that deserve X-ray follow-up. The properties of these galaxies have been carefully compared to our control sample of blue BCGs which have a known X-ray counterpart. Finally, we highlight the presence of interacting blue central early-type BCGs as interesting evidence of the creation of the dominat galaxy. In the course of the survey of BCG star formation, we serendipitously discovered a new example of a UV ring galaxy, UGC 4599. We compare the UV properties of this new UV ring galaxy with the well studied elliptical NGC 404, and with Hoag's Object, for which we report the first GALEX photometry. 149.10 Uncovering The Nature Of Optically-faint Chandra X-ray Clusters Stephanie Corbett1, W. Barkhouse1, P. Green2, M. Smith3, A. Vikhlinin2, D. Kim2 1University of North Dakota, 2Harvard-Smithsonian Center for Astrophysics, 3Cerro Tololo Inter-American Observatory, Chile. Exhibit Hall We present analysis of infrared observations of eight extended Chandra X-ray sources that were serendipitously discovered as part of the Chandra Multiwavelength Project (ChaMP). These X-ray sources were selected as having no optical counterparts in NOAO 4-meter observations in gri passbands (limiting depth i~23.5). Since these ``X-ray only" clusters are likely to be at high redshift, we have acquired J- and Ks-band imaging of these objects using PANIC on the Magellan telescope. Our Magellan/PANIC data allows us to confirm the high redshift nature of our sample by measuring the cluster red sequence, and ascertaining the properties of galaxies in these distant systems. 149.11 Evolution Or Selection: The X-ray Properties Of Moderate-redshift Optically-selected Clusters Of Galaxies Amalia K. Hicks1 1Michigan State University. Exhibit Hall By virtue of their size, galaxy clusters can be used to place important constraints on cosmological parameters. In particular, charting the evolution of the cluster mass function provides us with vital information on the progression of large-scale structure formation over time. The masses of clusters, however, are often inferred from observables such as gas temperature or X-ray luminosity, which can be influenced by non-gravitational processes that affect cluster baryons, such as energy injection (heating) and radiative cooling. In addition, many high-redshift cluster surveys select samples based on baryon observables such as gas density. Recent correlations between temperature, luminosity, and total cluster mass indicate significant discrepancies between observations and the theoretical expectations of self-similarity. Therefore understanding changes in cluster properties with redshift is of crucial importance to surveys that intend to use the evolution of the cluster population as a proxy for cosmic evolution, and ultimately for the determination of cosmological parameters. The results of our X-ray investigation of 13 high-redshift (0.6 < z < 1.1) optically-selected clusters suggest that the central entropy of these objects has been elevated by processes such as pre-heating, mergers, and episodic AGN outbursts, and that their ratio of gas mass to total gravitating mass is systematically lower than that found in lower-redshift X-ray selected clusters. To determine whether these effects are primarily associated with selection or evolution, we have designed a comparison sample of 10 moderate-z (0.2 < z < 0.6) optically-selected clusters, all of which have recently been observed by Chandra, Suzaku, or XMM. Here we present our final results from these observations, and discuss their relevance to cluster surveys which rely on the assumption of constant gas mass fraction to detect clusters and/or determine their masses. 149.12 Optical Scaling Relations of X-ray Selected Clusters at Moderate Redshift Dylan Kloster1, K. Rines1, B. E. Svoboda1, R. L. Arnold1, T. J. Welch2, R. A. Finn3, A. Vikhlinin4 1Western Washington University, 2McGill, Canada, 3Siena, 4CfA/IKI. Exhibit Hall The relation between dark matter and galaxies is a fundamental problem in astrophysics. Here, we study this relation using optical observations of an X-ray-selected sample of clusters at moderate redshift (z=0.35-0.90). We collected griz images of 30 clusters with WIYN/OPTIC to measure the bright end of the luminosity function. Our imaging extends approximately 2 magnitudes fainter than M*, thus including most of the total cluster light. We use the red sequence and statistical background subtraction to estimate the richnesses and stellar luminosities of the clusters. We measure scaling relations by comparing the optical properties to X-ray mass estimates derived from Chandra observations. At low redshift, some studies indicate that total stellar luminosity is a better predictor of cluster mass than X-ray luminosity. We test whether a similar result holds at moderate redshift. In the future, we will compare the optical and X-ray properties to virial mass estimates from optical spectroscopy and to Sunyaev-Zeldovich Effect observations. If photometric properties of clusters are good predictors of cluster mass, these relations could be applied to large surveys like SPT, Planck, DES, eROSITA, and LSST to improve constraints on the properties of dark energy. 149.13 A Systematic Search For X-ray Cavities In Galaxy Clusters Haik Manukian1, R. Dong2, J. Mulchaey3, J. Rasmussen4 1UC Santa Cruz, 2Princeton, 3Carnegie, 4DARK Cosmology Centre, Denmark. Exhibit Hall We have performed a systematic search for X-ray cavities in the hot gas of 280 galaxy clusters using Chandra archival data. The cavities are identified by subtracting an elliptical beta-model fitted to the X-ray surface brightness. Standard data reduction and calibration was performed to the cluster data using the most recent version of CALDB. Exposure maps were computed for the clusters assuming a mono-energetic distribution of source photons at the peak flux energy (usually around 1keV). The source images were then normalized by the exposure map, correcting for the effect of strongly variable exposure near the detector edges. A beta-model was then fitted and a residual image was obtained. The residual images were then visually inspected for cavities. Finally, we modeled the cavities as ellipses. We find tight correlations between the radial and tangential radii of the cavities, and between their size and projected distance from the cluster center, in quantitative agreement with the case for groups. This suggests that similar physical processes are responsible for cavity evolution and disruption in systems covering a large range in total mass. 149.14 Shocks in Galaxy Cluster X-ray Temperature Images Greg Salvesen1, J. W. Henning1, S. W. Skillman1, J. O. Burns1 1University of Colorado. Exhibit Hall We present adaptively binned X-ray temperature maps for a sample of galaxy clusters created from joint spectral fitting to XMM-Newton and Chandra archival data. The overall distribution of temperature in a cluster is more tightly constrained for maps produced by joint fitting than from fits to individual spectra alone. Mach number distributions are generated from temperature gradients, providing insight into the magnitude of shocks within the cluster. Major mergers are expected to produce shock structure, tracing the formation history of galaxy clusters. Applying our shock finding method to simulated temperature maps created with the Enzo N-body + hydrodynamic adaptive mesh refinement cosmological code, we find that the underlying Mach number distribution is recovered from the temperature structure after applying our binning scheme. While the quality of temperature maps generated from joint spectral fitting strongly depends on reliable calibration between the different instruments, we find our method to be a promising probe of the temperature structure in cluster environments and potentially the merger history. 149.15 Measurement of the Temperature Distributions of Galaxy Clusters Kari A. Frank1, J. R. Peterson1, K. Andersson2, J. S. Sanders3, A. C. Fabian3 1Purdue University, 2MIT, 3Univ. of Cambridge, United Kingdom. Exhibit Hall We utilize a Markov Chain Monte Carlo analysis to measure a new galaxy cluster parameter, the width of the ICM temperature distribution (?_logkT), as well median temperature, emission measure, cluster size, and abundance.  Critical to measuring ?_logkT, the MCMC avoids typical assumptions such as spherical symmetry and isothermality by modeling the ICM as a collection of X-ray emitting, smoothed particles of plasma, each with its own set of parameters including temperature, emission measure, position, and abundance.  The resulting distribution of particle temperatures is then representative of the ICM temperature distribution, and similarly for the other parameters.  The cluster temperature and ?_logkT are defined as the median and standard deviation of the temperature distribution, respectively.  The cluster emission measure is simply the sum of the particle emission measures, and the characteristic cluster size is determined from the particle spatial positions.  We have so far performed this analysis on XMM-Newton observations of 20 clusters with temperatures of 1keV-13keV in order to search for correlations between the temperature width and other cluster parameters.  149.16 Caustic Mass Estimate of Abell 370 Melodie Kao1, C. Harrison2 1Massachusetts Institute of Technology, 2University of Michigan. Exhibit Hall As the largest virialised structures in the Universe, galaxy clusters are important tools for constraining cosmological models. In particular, cluster masses can be used to estimate the M/L of the Universe and from that the matter energy density, Omegam. The most frequently used methods for estimating cluster masses are limited in their applicability. We present here a method of cluster mass estimation that is relatively free from these limitations. Originally proposed by Diaferio and Geller (1997), this method uses the amplitude of the caustics formed by galaxies in redshift space to estimate the escape velocity of the cluster gravitational potential and therefore the cluster mass. We estimate the mass within ~2Rvir of the rich cluster A370 (at z=0.3745) using this method. We thank the CTIO 2010 REU Program for supporting this work. 149.17 The Faint End of the Galaxy Luminosity Function in A1689: A Steep Red Faint End Upturn at z = 0.18 Eduardo Banados1, L. Hung2, R. De Propris3, M. West4 1Pontificia Universidad Catolica de Chile, Chile, 2Ohio State University, 3Cerro Tololo Inter-American Observatory, Chile, 4European Southern Observatory, Chile. Exhibit Hall We present a deep and wide I Luminosity Function (LF) for galaxies in Abell 1689 (z=0.183) from HST WFPC2 mosaic images covering 10' on the side. The main result of this work is the detection of a steep upturn in the dwarf galaxy LF, with a faint-end slope ? -2. We show that the faint end upturn is dominated by red quiescent galaxies. Evidence of luminosity segregation is presented: the dwarf-to-giant ratio appears to increase outward, but this is because giant galaxies are missing in the cluster outskirts. It seems likely therefore that the fainter galaxies have not been accreted from the field at recent times. 149.18 Galaxy Evolution in Ten Nearby Clusters Through XMM-OM Ultraviolet Photometry Neal A. Miller1, S. Yen1 1University of Maryland. Exhibit Hall We report on a program capitalizing on the availability of XMM Optical Monitor(XMM-OM) ultraviolet (UV) photometry to study galaxy evolution in clusters. We have produced a sample of ten nearby Abell clusters with XMM-OM, SDSS, and GALEX photometry, including nearly 800 objects with SDSS spectra and XMM-OM UV photometry. Of these, over 500 are galaxies belonging to the parent cluster sample. We use this large database to explore color-magnitude relations and identify various classes of objects. We further demonstrate the application of XMM-OM UV photometry to evaluate the star formation histories of galaxies. Support for this work is provided by NASA Award Number NNX09AC76G. 149.19 Clg J0218.3-0510: New Results On The Most Distant Spectroscopically Confirmed Cluster Ivelina G. Momcheva1, C. Papovich2, C. Willmer3, M. Pierre4, N. Clerc4, K. Tran2, J. Lotz5, K. Finkelstein2, S. Finkelstein2, G. Rudnick6, P. McCarthy1 1Carnegie Observatories, 2Texas A&M University, 3University of Arizona, 4Service d Astrophysique du CEA, France, 5STScI, 6University of Kansas. Exhibit Hall ClG J0218.3-0510 at z=1.62 is currently the most distant spectroscopically confirmed cluster. We will present results based on new ground-based spectroscopy of this cluster complemented by Chandra X-ray Observatory observations. We will examine the star formation rates and nuclear activity of the cluster galaxies with a focus on the high concentration of LIRGs and ULIRGs found in the cluster core and discuss their effect on the X-ray emission from the cluster. We will also outline our continuing survey to identify and study other z>1.5 clusters. 149.20 Abundances in Spiral Galaxies of the Pegasus I Cluster Paul Robertson1, G. A. Shields1, G. A. Blanc1 1University of Texas at Austin. Exhibit Hall We present a study of abundances in spiral galaxies of the Pegasus I cluster (cz = 4000 km/s), motivated by evidence for high interstellar abundances in the spirals of the Virgo cluster. Spectra of H II regions in six galaxies with a range of H I deficiency were obtained with the VIRUS-P integral field spectrograph on the 2.7-meter telescope at McDonald Observatory. The results suggest a pattern of higher abundances in more hydrogen deficient galaxies. This resembles the case for Virgo, despite the lower velocity dispersion and higher spiral fraction in the Pegasus cluster. 149.21 Specific Star Formation in the Abell 85 Cluster and its Filament Dario Fadda1, L. O. V. Edwards1, F. Durret2 1Caltech, 2IAP, France. Exhibit Hall We report the first results of the analysis of more than 500 optical spectra and near-infrared photometry targeting the galaxies of the Abell 85 cluster and its filament. Our team discovered the filament initially using X-ray observations. Recently, in order to study the dynamical and star formation properties, we have further supplemented our dataset with more than 500 new spectra covering cluster galaxies down to r'=21. We have also obtained J, H, and K images of approximately one square degree covering the cluster and its Southern filament. We present here a study of how the specific star formation, i.e. the star formation normalized by stellar mass, of the member galaxies varies in the different environments of the cluster: core, filament, and other external regions. 149.22 Gas-rich Optically Inert Galaxies in the Virgo Cluster Brian R. Kent1 1NRAO. Exhibit Hall Aperture synthesis observations of two HI cloud complexes located in the periphery of the Virgo galaxy cluster are presented. These low HI-mass clouds (log(MHI) < 8 at 16.7 Mpc) are seen toward the western M region of Virgo, where the galaxy population is thought to lie behind the main A cluster surrounding M87. The kinematic measurements of both unresolved Arecibo and resolved VLA-C observations are in good agreement. The HI detections cannot be identified with any optical,IR, or UV emission from available archival imaging. They are inert at these wavelengths. The total dynamical mass estimates are several times their HI content. We report the observed parameters derived from the VLA observations. One of these detections appears to be the most isolated optically inert object observed in the outer reaches of Virgo. 149.23 Arecibo Galaxy Environment Survey Observations of the NGC 7448 Region and the HI Mass Function Robert F. Minchin1, J. I. Davies2, Arecibo Galaxy Environment Survey (AGES) 1Arecibo Obs., 2Cardiff Univ., United Kingdom. Exhibit Hall The Arecibo Galaxy Environment Survey (AGES) is the deepest wide-area blind HI survey to date. Each surveyed region is centered on a nearby galaxy, group or cluster: we here report on the observations of the NGC 7448 group. Galaxy interactions in the NGC 7448 group reveal themselves through tidal tails and bridges - we find approximately 2.5 times more atomic gas in the intragroup medium than in the group galaxies. We also identify five new dwarf galaxies, two of which appear to be members of the NGC 7448 group. This is too few dwarf galaxies to reconcile observations with theoretical predictions of galaxy formation models. Combining the data from this group with observations of other AGES regions to derive an HI mass function which is well fit by a Schechter function with a relatively steep faint-end slope of -1.53 ± 0.5. Integrating this mass function gives a cosmic mass density of neutral hydrogen of 8.9 ± 0.8 x 10-4 - twice that found in the ALFALFA survey and almost three times higher than found in HIPASS. 149.24 Globular Cluster Survey in the Shapley Supercluster Regina Barber DeGraaff1, J. P. Blakeslee2, W. E. Harris3 1Washington State University, 2Herzberg Institute of Astrophysics, Canada, 3McMaster University, Canada. Exhibit Hall We present a survey of the globular cluster systems of 11 giant elliptical galaxies in clusters associated with the Shapley Supercluster. The program galaxies were imaged with the ACS/WFC in the F814W bandpass (comparable to I-band) and are in the redshift range z = 0.035-0.046. Radial density plots and the total globular cluster populations of these 11 galaxies are presented. The most massive galaxy in our sample contains the largest globular cluster population studied to date. Another galaxy in our sample, ES0325-G004, is the nearest gravitational lensing galaxy, and STScI obtained multi-band imaging for a press release image. This provides additional color information on its rich GC system. 149.25 Searching for Intragroup Light in Multiple Galaxy Groups John J. Feldmeier1, S. Downing1, J. C. Mihos2, P. Harding2, H. L. Morrison2 1Youngstown State Univ., 2Case Western Reserve University. Exhibit Hall Intracluster stars, stars outside of galaxies, have been shown to be common in galaxy clusters, and contain approximately 20% of the total stellar luminosity. However, the amount of intragroup light in galaxy groups is substantially less certain. Estimates of the intragroup luminosity fraction range from 0% to 46% of the total light. This is extremely unfortunate, since the majority of galaxies are in groups, and theoretical work shows that the group environment can have strong effects on the production of intracluster/intragroup light. Here, we give an update on our efforts to determine the amount and spatial distribution of intragroup light in both normal and compact groups. We will present data from the 0.6m Burrell Schmidt and the KPNO 2.1m of four Hickson and four normal galaxy groups, including the nearby Leo I group that is known to have intergalactic star formation. Using the techniques of deep surface photometry, we can reach faint surface brightnesses of 26-27 magnitudes per square arcsecond. We will show tidal features found in these groups, and provide estimates of the total intragroup fraction. 149.26 Using Networking Algorithms to Assess the Environment of Galaxy Groups Ali Bramson1, E. M. Wilcots1 1University of Wisconsin-Madison. Exhibit Hall Understanding the environment a galaxy resides in is crucial to our understanding of the galaxy’s formation and properties. Most galaxies (~70%) live in groups and it is important to develop a quantitative understanding of how galaxies are distributed within groups and how groups are distributed in the larger scale structure. In addition to the traditional friends-of-friends algorithms we are applying analytical techniques developed for understanding social networks to understand the network of galaxies in the Abell 1367-Coma supercluster. We use data from the SDSS, 2MASS, and ALFALFA to detect substructure within catalog groups and quantitatively measure the degree to which individual groups are connected as a new method of probing the large scale environments of galaxies and groups. 149.27 The Mysterious Cheshire Cat Galaxy System. The First Case of a Collision Between Fossil Groups? Jimmy Irwin1, R. Dupke2 1Univ. Of Alabama, 2Univ. Of Michigan. Exhibit Hall Fossil groups present a puzzle to current theories of structure formation. Despite the low number of bright galaxies, their high velocity dispersions and high gas temperatures seem to indicate cluster-like gravitational potentials. One extreme example of a potential fossil group is the Cheshire Cat gravitational lens group of galaxies. While it contains two bright central galaxies rather than one (surrounded by ~25 galaxies at least two magnitudes fainter), these galaxies are moving at least 1100 km/s relative to one another and likely represent the collision of TWO fossil groups. We analyzed data from a moderately long Chandra observation of the Cheshire Cat and found and found the ICM to have a very hot (~6 keV) core, but a low X-ray luminosity, which places it off the LX/TX relation for groups/clusters. Furthermore, the X-ray emission does not appear to be centered on either bright galaxy, but midway between them. We discuss the implications of the Chandra results and discuss whether this system represents the first example of a fossil-group/fossil group merger. 149.28 SMARTS H? Observations Of ALFALFA Gas-rich Galaxies In NGC 5846 Katelyn M. O'Brien1, R. A. Koopmann1, ALFALFA Team 1Union College. Exhibit Hall The Undergraduate ALFALFA (Arecibo Legacy Fast ALFA) Team Groups Project is a collaborative undertaking of faculty and undergraduates at 11 institutions, aimed at investigating properties of galaxy groups surveyed by the ALFALFA blind HI survey. The Union College team is analyzing the galaxy group NGC 5846 and its environments. Here we present star formation properties of 12 gas-rich galaxies in the group as traced by CCD H? images obtained at the Small and Moderate Aperture Research Telescope System (SMARTS) CTIO 0.9m telescope. This work has been supported by NSF grants AST-0724918, AST-0725267, and AST-0725380. 149.29 HI Deficiency as a Function of Galaxy Type in the MKW11 Group James Turner1, M. Crone-Odekon1, ALFALFA Team 1Skidmore College. Exhibit Hall The Undergraduate ALFALFA (Arecibo Legacy Fast ALFA) Team Groups Project is a collaborative undertaking of faculty and undergraduates at 11 institutions, aimed at investigating properties of galaxy groups surveyed by the ALFALFA blind HI survey. As part of this project we examine a 10x10 degree region around the rich galaxy group MKW 11 in order to study HI deficiency as a function of local density as well as optical galaxy morphology. Our sample includes 496 galaxies in the Sloan Digital Sky Survey, 153 of which are detected in HI. This work has been supported by NSF grants AST-0724918, AST-0725267, and AST-0725380. 149.30 Group Membership and HI Sources in the WBL 368 Galaxy Group Catherine Weigel1, M. Brault1, P. Troischt1, ALFALFA Team 1Hartwick College. Exhibit Hall The Undergraduate ALFALFA (Arecibo Legacy Fast ALFA) Team Groups Project is a collaborative undertaking of faculty and undergraduates at 18 institutions, aimed at investigating properties of galaxy groups surveyed by the ALFALFA blind HI survey. The Hartwick College team is analyzing a 6X6 degree region around the galaxy group WBL 368, which has an average recessional velocity of 4732 km/s. Preliminary analysis using ALFALFA data and the Sloan Digital Sky Survey indicates a significant increase in group membership, with 47% of the member galaxies detected as HI sources. This work has been supported by NSF grants AST-0724918, AST-0725267 and AST-0725380. 149.31 Stellar Populations and Star Formation of ALFALFA Galaxies in Coma-Abel 1367 Cody Gerhartz1, M. Jones1, K. Hess1, E. Wilcots1 1University Of Wisconsin Madison. Exhibit Hall We present GALEX near-ultraviolet (NUV) and far-ultraviolet (FUV) photometry, Sloan Digital Sky Survey r and u-band photometry, as well as archival 2MASS observations for the Coma-Abell 1367 Supercluster. Our aim is to study the stellar populations and star formation history of HI-detected galaxies from the ALFALFA survey. We correct for the effects of interstellar reddening and inclination on the observed uv colors and derive an measure of the rate of recent and current star formation, and how they are linked to the HI content, of galaxies throughout the supercluster. 150 Large Scale Structure, Cosmic Distance Scale Poster Session Exhibit Hall 150.01 RR Lyrae as Structural Tracers for the LMC Katherine Accetta1, A. Kunder2 1Youngstown State University, 2CTIO, Chile. Exhibit Hall RR Lyrae variable stars are key distance indicators because they have a predictable period-luminosity relation. Previous surveys by the OGLE and MACHO collaborations have identified RR Lyrae stars within the Large Magellanic Cloud (LMC), but as the prime directive of these surveys was to search for gravitational lensing effects, precision photometry was not a primary concern. We have obtained accurate V and R photometry of a sub-sample of OGLE RR Lyrae located around the central bar. The results presented here encompass two of the twenty-six surveyed fields, one field on the far east side of the central bar and the other on the far west. Distances and reddening along the line of sight of 50 RR Lyrae can be used to map out the structure of the old stellar populations within the LMC. A comparison on the properties of the RR Lyrae in these two fields allow constraints to be made on the orientation of the LMC, and to place limits on the warping of the LMC disk. 150.02 The Flow-field From Galaxy Groups In 2MASS Aidan Crook1, J. Huchra2, L. Macri3, K. Masters4, T. Jarrett5 1Microsoft, 2Harvard-Smithsonian Center for Astrophysics, 3Texas A&M University, 4University of Portsmouth, United Kingdom, 5California Institute of Technology. Exhibit Hall We present the first model of a flow-field in the nearby Universe (cz < 12,000 km/s) constructed from groups of galaxies identified in an all-sky flux-limited survey. The Two Micron All-Sky Redshift Survey (2MRS), upon which the model is based, represents the most complete survey of its class and, with near-IR fluxes, provides the optimal method for tracing baryonic matter in the nearby Universe. Peculiar velocities are reconstructed self-consistently with a density-field based upon groups identified in the 2MRS Ks<11.75 catalog. The model predicts infall toward Virgo, Perseus-Pisces, Hydra-Centaurus, Norma, Coma, Shapley and Hercules, and most notably predicts backside-infall into the Norma Cluster. We discuss the application of the model as a predictor of galaxy distances using only angular position and redshift measurements. By calibrating the model using measured distances to galaxies inside 3000 km/s, we show that, for a randomly-sampled 2MRS galaxy, improvement in the estimated distance over the application of Hubble's law is expected to be ~30%, and considerably better in the proximity of clusters. We test the model using distance estimates from the SFI++ sample, and find evidence for improvement over the application of Hubble's law to galaxies inside 4000 km/s, although the performance varies depending on the location of the target. This work has been supported by NSF grant AST 0406906 and the Massachusetts Institute of Technology Bruno Rossi and Whiteman Fellowships. 150.03 21 Cm Tomography With the Alfalfa Survey Alexander B. Fry1, C. Boutan1, P. A. Carroll1, B. Hazelton1, M. F. Morales1 1University of Washington. Exhibit Hall Neutral hydrogen (HI) 21cm intensity mapping, or HI tomography is a promising technique being utilized by several upcoming experiments (LOFAR, MWA, SKA). The measurement of volume averaged neutral hydrogen mass density in synoptic sky surveys can be applied to the study of the HI mass function, the distribution of large scale structure, the reionization of the universe, and the expansion history of the universe through such standard rulers as baryonic acoustic oscillations. In order to prepare for future experiments, in particular the Murchison Widefield Array (MWA), we analyze the Arecbo Legacy Fast ALFA (Arecibo L-Band Feed Array) Feed Array (ALFALFA) survey data to probe the spatial density variations of HI in our local universe (z <0.06) where data is currently available. We address challenges unique to data of this kind, such as identifying and subtracting out signal from RFI and local galactic sources, and characterizing the ALFA array beam pattern which dictates sensitivity and resolution. 150.04 Estimating Photometric Redshifts in Non-Representative Galaxy Samples using Boosted Decisions Trees Adam J. Sypniewski1, D. W. Gerdes1 1University of Michigan. Exhibit Hall Future large-scale optical surveys, such as the Dark Energy Survey, will require photometric redshift estimates for hundreds of millions of galaxies. In general, the magnitude and color distributions of these galaxies are expected to differ from those of the spectroscopic sets used for training empirically-based photometric redshift algorithms. In this analysis, we investigate the robustness of the ArborZ boosted decision tree method for estimating photometric redshifts in these non-representative cases. We show that ArborZ performs well in these cases, provided that the training and target sets have sufficient overlap in parameter space. We also compare the results of training ArborZ on magnitudes, colors, and a combination of the two. 150.05 Photometric Redshift Catalog of SDSS DR8 Luminous Red Galaxies Antonio Jose Cuesta-Vazquez1, A. Ross2, S. Ho3, N. Padmanabhan1, F. Prada4, M. White5, D. J. Schlegel3, W. J. Percival2, N. Connolly6, F. de Simoni7, B. Ramos7, N. Ross3, L. A. N. da Costa7 1Yale University, 2Institute of Cosmology and Gravitation, University of Portsmouth, United Kingdom, 3Lawrence Berkeley National Laboratory, 4Instituto de Astrofisica de Andalucia, Spain, 5University of California at Berkeley, 6Hamilton College, 7Observatorio Nacional, Brazil. Exhibit Hall The project focuses on the calibration of photometric redshifts of luminous red galaxies within the DR8 imaging catalog of Sloan Digital Sky Survey. We aim to use the spectroscopic sample of BOSS galaxies and compare their (true) spectroscopic redshifts with photometric redshifts obtained from different techniques. We discuss the performance of photo-z estimation via template fitting of the spectral energy distribution and trained neural networks using ANNz. We also obtain the photometric redshift distributions of luminous red galaxies in different redshift bins and provide an analytical fit to these distributions. In this sense, we comment on the capabilities of ANNz to investigate the systematics involved in galaxy clustering measurements, such as spatial variations of the redshift distributions. The resulting photo-z catalogs are useful for the estimation of cosmological parameters through the evaluation of the power spectrum (Padmanabhan et al. 2007), which will benefit from large sky area covered by SDSS-III imaging sample. 151 Dark Matter & Dark Energy Poster Session Exhibit Hall 151.01 Monte Carlo approach to Dark Matter Mapping Suzanne Lorenz1, J. R. Peterson1 1Purdue University. Exhibit Hall We present an an analysis method of constructing dark matter maps based on weak lensing using a Markov Chain Monte Carlo technique. The dark matter in a cluster can be modeled as a collection of massive blobs that bend light according to gravitational lensing. We move these dark matter blobs in RA, Dec and redshift and as a result perturb the ellipticities of subsequent background galaxies. With this method we have looked at images of Abell 2218 from the Subaru archive, which have been analyzed by our wavelet source detection algorithm and all the ellipticities calculated using second moments. From this we have been able to reconstruct a mass map. With the ability to reconstruct dark matter distributions in redshift as well as projected on the sky, we may be able to more accurately reconstruct the dark matter web. 151.02 Galaxy Kinematics with VIRUS-P: The Dark Matter Halo of M87 Jeremy Murphy1, K. Gebhardt1, J. J. Adams1 1University of Texas, Austin. Exhibit Hall We have conducted axisymmetric, orbit-based dynamical modeling on M87, the second rank galaxy in the Virgo cluster, and find clear evidence for a large dark matter halo. The total enclosed mass within 47 kpc is 6e12 solar masses making M87 one of the most massive dark halos ever measured in the local universe. To construct these dynamical models we fit for the stellar mass-to-light ratio and two dark halo parameters, assuming a cored logarithmic dark halo profile. The dynamical data comes from existing globular cluster data, SAURON stellar kinematics in the center of M87, and new 2-D stellar kinematics taken with VIRUS-P, an integral field unit currently deployed at the McDonald Observatory. These kinematics add significantly to the current data set on M87 and allow for a direct comparison between different dynamical tracers. We find good agreement between the dynamics of the stars and globular cluster data at large radii, indicating these two systems are in equilibrium. However, the enclosed mass we measure is 60% higher than recent mass estimates calculated from X-ray gas measurements. Understanding the systematics present in the various tools used to estimate mass in local galaxies is critical to our understanding of the formation history and the role dark matter plays in the evolution of these galaxies. We also report on the current status of a VIRUS-P survey of the stellar kinematics of local, massive elliptical galaxies. Our data set includes giant field ellipticals, cluster members and brightest cluster galaxies. The goal of this project is to quantify the amount of dark matter in these systems in order to explore how the role of cluster environment influences both the amount and shape of the dark matter profile. 151.03 A Search for Dark Matter Decay Products in Nearby Dwarf Galaxies Bang Nhan1, B. Mason2, K. Spekkens3, J. Aguirre4 1University of Colorado at Boulder, 2National Radio Astronomy Observatory, 3Royal Military College of Canada, Canada, 4University of Pennsylvania. Exhibit Hall According to the current cosmological concordance model, 23% of the universe's denisty is consisted of cold dark matter (CDM). One of the candidates for the CDM is Weakly Interacting Massive Particle (WIMP). Supersymmetric (SUSY) extension of the Standard Model of particle physics has predicted a stable and electrically neutral particle with rest mass between 1 GeV and 1000 GeV. It is known as the neutralino. Colafrancesco et al. (2007) proposes possible indirect detection of the neutralino through decay products of its self annihilation in nearby dwarf spheroidal (dSph) galaxies. We have used Green Bank Telescope (GBT) to search for synchrotron radiation from the self annihilation in four sources: Draco, Ursa Major II, Willman 1, and Coma Berenices. We discuss the analysis of these data, present maps and radial profiles of these four dSph systems, and a comparison with theoretical predictions of the neutralino decay signature. 151.04 A New Assessment of Dark Matter in the Milky Way Galaxy Grant N. Remmen1 1University of Minnesota - Twin Cities. Exhibit Hall Through an examination of recent data on the mass distribution and velocity curve of the Milky Way Galaxy, I produce a new estimate of the dark matter distribution, as well as the overall dark matter content, of our galaxy. Initially, I develop a model of the baryonic mass of the galaxy (i.e. luminous matter and interstellar clouds). This model incorporates three components: an exponential stellar disc and a central stellar bulge, based on the Tuorla-Heidelberg model, and a gaseous layer, fit to the gas density distribution data of Olling & Merrifield (2001). Secondly, incorporating recent data, I calculate an updated rotational velocity curve for the galaxy as a function of galactocentric radius. Using this velocity curve, I determine total galactic mass as a function of radius and compare this with the baryonic mass model to determine the distribution of dark matter in the galaxy, with improved precision and over a greater spatial range than previous estimates. This calculation results in a radial dark matter density distribution that falls off with large distance in a characteristic fashion. Finally, I show that neutrinos, particles that have often been suggested as a component of dark matter, cannot make up more than a negligible fraction of the galactic dark matter content. Funding for this research was provided by the University of Minnesota College of Science & Engineering/Institute of Technology Honors Undergraduate Research Scholarship program. 151.05 Constraining Modified Gravity Theories with Cosmological Data Scott Daniel1, E. V. Linder2 1University of Washington, 2Lawrence Berkeley National Laboratory. Exhibit Hall Cosmic acceleration could be either an effect of dark energy or of a gravity theory other than General Relativity operating on cosmological scales. We constrain these competing possibilities by examining the growth of perturbations in both the Cosmic Microwave Background and large scale structure as measured by weak lensing surveys, galaxy counts, and galaxy-CMB cross-correlations. We consider a model-independent parametrization of departures from General Relativity and find that, while Newton's constant is constrained to be consistent with General Relativity to within a few 10%, a parameter modifying the growth rate of structure is largely unconstrained by present data. We do find evidence for departure from General Relativity at small scales and low redshifts. We believe, however, that this is due primarily to artifacts in the data and uncertainty in the behavior of non-General Relativity gravity theories at non-linear scales. This work was supported by the World Class University grant R32-2009-000-10130-0 through the National Research Foundation, Ministry of Education, Science and Technology of Korea. 151.06 3D Reconstruction of the Density Field: Using Redshift Information in Weak Lensing Analysis Jake Vander Plas1, A. J. Connolly1, B. Jain2, M. Jarvis2 1University of Washington, 2University of Pennsylvania. Exhibit Hall We present a new method for constructing three-dimensional mass maps from gravitational lensing shear data. We solve the lensing inversion problem using truncation of singular values (within the context of generalized least squares estimation) without a priori assumptions about the statistical nature of the signal. This singular value framework allows a quantitative comparison between different filtering methods: we evaluate our method beside the previously explored Wiener filter approaches. Our method yields near-optimal angular resolution of the lensing reconstruction and allows cluster sized halos to be de-blended robustly. It allows for mass reconstructions which are 2-3 orders-of-magnitude faster than the Wiener filter approach, which will become increasingly important for future large surveys, e.g. LSST. Using this SVD framework, we discuss optimal redshift binning for 3D shear mapping, and explore how this informs the choice of binning in measurements of power spectrum evolution. 152 Star Associations, Star Clusters - Galactic & Extra-galactic Poster Session Exhibit Hall 152.01 What Can 100 Million Monte Carlo Simulations Do For You? - Age and Mass for 900 LMC Clusters Margaret M. Hanson1, B. Popescu1 1Univ. of Cincinnati. Exhibit Hall The new version of the MASSCLEANcolors database contains over 100 million cluster models. Presently, current models for stellar populations are available only in the infinite mass limit. But real clusters have a finite mass, and their integrated colors show a large dispersion due to stochastic fluctuations in the stellar mass function. The MASSCLEANcolors database illustrates the extreme and non-Gaussian distribution of integrated colors and magnitudes consistent with theoretical work and integrated photometry of real clusters. The database entries form a consistent set of integrated colors and magnitudes, age and mass and can be used to improve age and mass determinations of moderate mass stellar clusters. Our newest application, MASSCLEANage, uses observed integrated UBVR photometry and a statistical inference code to search the MASSCLEANcolors database to solve simultaneously for the age and mass of a cluster. We demonstrate the power of MASSCLEANage by presenting new values for age and mass for 900 LMC clusters. This material is based upon work supported by the National Science Foundation under Grant No. 0607497 & 1009550. 152.03 Color Selection of Intracluster Globular Clusters in the Next Generation Virgo Survey Patrick R. Durrell1, A. McConnachie2, K. Accetta1, E. W. Peng3, NGVS Team 1Youngstown State Univ., 2HIA, Canada, 3Peking University, China. Exhibit Hall The Next Generation Virgo Survey (NGVS) is a large, 104 square degree deep imaging survey (with CFHT's MegaCam) of the Virgo Cluster. One of the (many) science drivers for the NGVS is to quantify the population of intracluster globular clusters (IGCs) present between the galaxies. The large color baseline of the NGVS ugriz images allows for the effective extraction of candidates IGCs from background galaxies and foreground Milky Way stars. Here we present preliminary results on the definition of the selection of IGCs in color-color space, as well as early results on the surface density of IGCs over a large part the Virgo Cluster. 152.04 Discovery of a Large-Scale Structure of Globular Clusters in the Virgo Cluster Myung Gyoon Lee1, H. Park2, H. Hwang3, S. Lim1 1Seoul National Univ., Korea, Republic of, 2Korea Astronomy and Space Science Institute, Korea, Republic of, 3CEA, France. Exhibit Hall Globular clusters are usually found in galaxies. Decades ago it was suggested that a cluster-wide population of globular clusters may exist in galaxy clusters. Recently we discovered a new type of large-scale structure in the Virgo cluster of galaxies: it is composed of globular clusters. Globular clusters are found wandering between galaxies (intracluster globular clusters) as well as in galaxies. These globular clusters fill a significant fraction in the area of the Virgo cluster. The distribution of the globular clusters is in general similar to that of the X-ray emitting hot gas, but shows some differences as well. The intracluser globular clsuters might have been mostly stripped off from low-mass dwarf galaxies. The nature of the intracluster globular clusters is not yet known. These intracluster globular clusters will be an excellent tool to study various topics on galaxy clusters: the distribution of dark matter, the evolution of galaxy clusters, the first stellar systems in the universe, and the origin of globular clusters. Implications of our results will be discussed. 152.05 Searching for Massive Star Clusters around Luminous Blue Variables Jared Stensland1, M. L. Edwards2, V. J. Mikles3 1Middlebury College, 2Gemini Observatory, Souther Operations Center, Chile, 3Department of Physics and Astronomy, Louisiana State University. Exhibit Hall We present a method to search for the massive birth clusters of Luminous Blue Variables (LBVs). Using theoretical absolute magnitudes of early-type stars, we calculated expected color and magnitude limits for candidate massive stars at the distance and reddening of the Pistol Star and FMM 362 in the Quintuplet. We then applied these cuts to stars found in the 2MASS catalog surrounding the LBVs. By using a well-characterized cluster, we were able to confirm the method's effectiveness and determine the color and magnitude criteria that eliminated the highest number of false candidates while recovering the largest number of known massive cluster members. We then calculated and applied similar cuts to stars within a 1pc radius of WRA 751 to confirm its cluster, Teutsch 143a, discovered by Pasquali et al (2006) and later investigated by Froebrich et al (2008). We used our method to select 22 strong candidate massive cluster stars, 18 medium confidence candidates and 39 weak candidates, categorized based on their colors and magnitudes. These stars are prime candidates for follow-up spectroscopy to determine their spectral types and confirm cluster membership. We plan to apply a similar method to other LBVs without known birth clusters. 152.06 Using H-Alpha Morphology and Surface Brightness Fluctuations to Age-Date Star Clusters in M83 Bradley C. Whitmore1, R. Chandar2, H. Kim3, C. Kaleida3, M. Stankiewicz4, R. O'Connell5, WFC3 SOC 1STScI, 2U. Toledo, 3ASU, 4JHU, 5U. VA. Exhibit Hall We use WFC3 observations of the nearby grand design spiral galaxy M83 to develop two independent methods for estimating the ages of young star clusters. The first method uses the physical extent and morphology of H-alpha emission to estimate the ages of clusters younger than ~10 Myr. It is based on the simple premise that the gas in very young (< few Myr) clusters is largely coincident with the cluster stars, is in a small, ring-like structure surrounding the stars in slightly older clusters (i.e., ~ 5 Myr), and is in larger ring-like bubbles for older clusters (i.e., ~5 - 10 Myr). The second method is based on an observed relation between pixel-to-pixel flux variations within clusters and their ages. This method relies on the fact that the brightest individual stars in a cluster are most prominent at ages around 3 - 10 Myr, and fall below the detection limit (i.e., Mv < -3.5) for ages older than 100 Myr old. The older clusters therefore have a smoother appearance and smaller pixel-to-pixel variations. We compare age estimates of clusters in M83 derived from these two techniques with estimates determined from fitting UBVIHalpha observations with model predictions, and find good agreement at the ~90 % level, with an scatter of ~0.2 dex in log age for young clusters (< 10 Myr) and ~0.5 dex for older (> 10 Myr) clusters. This project is based on Early Release Science observations made by the WFC3 Scientific Oversight Committee. We are grateful to the Director of the Space Telescope Science Institute for awarding Director's Discretionary time for this program. Support for program #11360 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. 152.07 The Star Cluster Populations in the Evolutionary Sequence of Hickson Compact Groups Aparna Maybhate1, K. Fedotov2, I. Konstantopoulos3, J. Charlton3, A. Zabludoff4, R. Chandar5, P. Durrell6, S. Gallagher2, P. Tzanavaris7 1STScI, 2The University of Western Ontario, Canada, 3The Pennsylvania State University, 4Univeristy of Arizona, 5University of Toledo, 6Youngstown State University, 7NASA Goddard Space Flight Center. Exhibit Hall We present a study of the three compact groups HCG 16, HCG 22, and HCG 42 observed using WFPC2 and ACS on the Hubble Space Telescope. These groups span a range of cold gas to total mass ratios defined by log(MHI)/log(Mdyn). Groups with lower gas content have a higher fraction of early type galaxies and thus may be more dynamically evolved. We present a comparative study of the ages and masses of star clusters in these groups based on their color-magnitude and color-color diagrams as well as their spatial distribution within the group. 152.08 Star Clusters in Intermediate-Age Galaxy Merger Remnants Bryan W. Miller1, G. Trancho1, F. Schweizer2 1Gemini Observatory, Chile, 2OCIW. Exhibit Hall Studies of globular cluster systems play a critical role in our understanding of galaxy formation. Star clusters are useful tracers of major star-formation events in galaxies since they are compact, relatively easy to detect, and have properties well described by simple-stellar-population models. Imaging with the Hubble Space Telescope has revealed that young compact star clusters are formed copiously during galaxy mergers, strengthening theories in which giant elliptical galaxies are formed through mergers of spirals. However, the formation and evolution of globular cluster systems is still not well understood. We should be able to observe how cluster systems evolve from the very young systems with power-law luminosity functions to old systems with log-normal luminosity functions like those observed in old elliptical galaxies. Finding intermediate-age cluster systems would constrain theories of cluster formation and destruction (evaporation, shocking, dynamical friction) as well as show the significance of merger events in the histories of galaxies. We present results of combining HST optical photometry with ground-based K-band photometry from NIRI and Flamingos-I on Gemini to study the star cluster systems of five intermediate-age merger remnants. The galaxies were chosen based on blue colors and fine structure such as shells and ripples that are indicative of past interactions. We find evidence for star clusters with ages consistent with the estimated merger ages. The properties of the star clusters systems and implications for galaxy and star cluster formation will be discussed. Based on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the Particle Physics and Astronomy Research Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), CNPq (Brazil), and CONICET (Argentina). 152.09 Observational and Numerical Constraints on Early Star Cluster Evolution Richard de Grijs1, R. J. Allison2, Y. Hu3, L. Deng4, S. P. Goodwin2 1Kavli Institute for Astronomy and Astrophysics, Peking University & The Astrophysical Journal, China, 2Department of Physics & Astronomy, The University of Sheffield, United Kingdom, 3National Astronomical Observatories & Graduate University, Chinese Academy of Sciences, China, 4National Astronomical Observatories, Chinese Academy of Sciences, China. Exhibit Hall Exciting recent developments in theory and observations call for renewed scrutiny of the early evolution of star clusters spanning a large range of parameter space. First, using a large ensemble of N-body simulations of moderately sized (N=1000), cool, fractal clusters, we find that cool, clumpy clusters dynamically mass segregate on a short timescale. This implies that the notion of ‘primordial mass segregation’ may be obsolete. The cluster properties also change rapidly on very short timescales: young clusters may undergo core collapse on timescales of < 1 Myr, when a dense core containing massive stars is hardened because of energy losses to a halo of lower-mass stars. In addition, we use high-resolution Hubble Space Telescope imaging observations of the young (~15-25 Myr-old) star cluster NGC 1818 in the Large Magellanic Cloud to derive an estimate for the binary fraction of F stars (1.3 < m*/M¤< 1.6). Our new study provides the strongest constraints yet on the (close to) initial binary fraction in a low-metallicity environment ([Fe/H] ~ -0.4 dex). We find that our novel artificial-star-test method is sensitive to binaries with mass ratios, q ? 0.4. For binaries with F-star primaries and mass ratios q > 0.4, the binary fraction is ~ 0.35. This suggests a total binary fraction for F stars of 0.55 to unity, depending on assumptions about the form of the mass-ratio distribution at low q, which is consistent with the field and lower-density clusters. This suggests that, at least among intermediate-mass stars, metallicity down to [Fe/H] ~ -0.4 dex does not suppress fragmentation and binary formation, and the binarity of these stars is at least as high as at solar metallicity. We therefore strongly argue for inclusion of realistic binary fractions in simulations aimed at following early star cluster evolution. 152.10 Tides, Rotation Or Anisotropy? Self-consistent Nonspherical Models For Globular Clusters Anna L. Varri1, G. Bertin1 1Universita' degli Studi di Milano, Italy. Exhibit Hall Spherical models of quasi-relaxed stellar systems provide a successful zeroth-order description of globular clusters. Yet, the great progress made in recent years in the acquisition of detailed information of the structure of these stellar systems calls for a renewed effort on the side of modeling. In particular, more general analytical models would allow to address the long-standing issue of the physical origin of the deviations from spherical symmetry of the globular clusters, that now can be properly measured. In fact, it remains to be established which is the cause of the observed flattening, among external tides, internal rotation, and pressure anisotropy. In this paper we focus on the first two physical ingredients. We start by briefly describing a recently studied family of triaxial models that incorporate in a self-consistent way the tidal effects of the host galaxy, as a collisionless analogue of the Roche problem (Varri & Bertin ApJ 2009). We then present two new families of axisymmetric models in which the deviations from spherical symmetry are induced by the presence of internal rotation. The first one is an extension of the well-known family of King models to the case of axisymmetric equilibria flattened by solid-body rotation. The second family is characterized by differential rotation, designed to be rigid in the center and to vanish in the outer parts, where the imposed truncation in phase space becomes effective. For possible application to globular clusters, models of interest should be those, in both families, characterized by low values of the rotation strength parameter and quasi-spherical shape. For general interest in stellar dynamics, we show that, for high values of that parameter, the differentially rotating models may exhibit unexpected morphologies, even with a toroidal core. 152.11 Photometry of the Outer Halo Globular Cluster AM 1 Brian Pohl1, B. W. Carney1 1University of North Carolina, Chapel Hill. Exhibit Hall At a heliocentric distance of ~120 kpc, AM 1 is the most distant Milky Way globular cluster. In an effort to further investigate this cluster, we obtained over 17 hours of data with the SOAR telescope. We present a color magnitude diagram, calibrated to the Johnson BV standard system, with internal errors of 0.025 mag at V = 25. The data were obtained over the course of 10 nights spanning 2007 to 2009 in the hope of detecting variable stars. We present initial results for the search for variable stars as well as revised distance, age and metallicity estimates. 152.12 HST/WFC3 Photometry of NGC 2808 and Its Multiple Main Sequences Elizabeth Jeffery1, T. Brown1, A. Dotter1, I. Hubeny2, W. B. Landsman3, T. Lanz4, A. V. Sweigart5 1STScI, 2University of Arizona, 3Science Systems and Applications, Inc., 4University of Maryland, 5NASA Goddard Space Flight Center. Exhibit Hall Recent high precision photometric observations of several globular clusters have revealed that these simple stellar populations may not be as simple as we once believed. Some globular clusters have shown interesting features in their color-magnitude diagrams indicating the presence of multiple populations. Recent HST observations of the massive globular cluster NGC 2808 have revealed the presence of three main sequences. We present new observations of NGC 2808 using the new WFC3 camera on HST. Observations are in five photometric bands covering a large wavelength range from the UVIS to the IR channels of WFC3. Moreover, these observations extend below the "turn down" in the lower main sequence (as seen in the IR CMD) and therefore reach deeper than past data sets on this cluster. We discuss various model fits and compare with other observed CMDs of other globular clusters to explore the origin of these multiple sequences. 152.13 Luminosity Functions of M15 Diane Feuillet1, B. Borland2, N. Paust1, B. Chaboyer3 1Whitman College, 2University of Wisconsin, 3Dartmouth College. Exhibit Hall We present new BVI observations of the Galactic globular cluster M15 obtained with the 2.4 meter Hilter telescope at the MDM Observatory under good seeing conditions. The observations cover an area 25 arcminutes square centered on the cluster. The observations have been reduced using the DAOPHOT stellar photometry package and extensive artificial star tests to produce detailed color-magnitude diagrams with over 50,000 stars and luminosity functions. The data extends from the tip of the red giant branch to several magnitudes below the main sequence turnoff. We compare the CMDs and luminosity functions to Dartmouth Stellar Evolution Program (DSEP) models. Using a metallicity of [Fe/H] = -2.10 we find an age of 13 Gyr and distance modulus of (m-M)V = 15.55. 152.14 RGB Luminosity Functions for M2, M3, and M14 Nathaniel Paust1, B. Chaboyer2 1Whitman College, 2Dartmouth College. Exhibit Hall We present new BVI wide-field photometry of M2 (NGC 7089), M3 (NGC 5272), and M14 (NGC 6402). After extensive artificial star tests to determine completeness, this photometry is then used to create red giant branch stellar luminosity functions for the clusters. Comparisons of the observed luminosity functions to model functions from the Dartmouth Stellar Evolution Program verify that the stellar evolution models accurately predict the speed of evolution on the red giant branch. Further examination using the Kolmogorov-Smirnoff test, determines the ages and distance moduli of the clusters to be 14.0±1.9 Gyr at (m?M)V =15.3 for M2, 10.3 ± 1.6 Gyr at (m?M)V = 15.2 for M3, and 13.5±1.6 Gyr at (m?M)V = 16.45 for M14. A Monte Carlo investigation of the uncertainties involved in creating and matching theoretical luminosity functions to observations suggests a 1.2 Gyr systematic uncertainty. 152.15 Multiple Stellar Populations in Globular Clusters Enrico Vesperini1, S. L. W. McMillan1, F. D'Antona2, A. D'Ercole3 1Drexel Univ., 2INAF, Osservatorio Astronomico di Roma, Italy, 3INAF, Osservatorio Astronomico di Bologna, Italy. Exhibit Hall A number of spectroscopic and photometric observations have shown that many globular clusters host multiple stellar populations and challenged the common paradigm that globular clusters are 'simple stellar populations' composed of stars of uniform age and chemical composition. We present the results of a survey of simulations exploring the formation and dynamical evolution of multiple populations in globular clusters and the dependence of the amount of second-generation stars formed on a cluster's structural properties. We also present theoretical estimates of the fraction of the Galactic stellar halo composed of second-generation stars that originated in globular clusters. 152.16 Main Sequence Binary Fraction in Globular Cluster NGC 6397 Srikar Srinath1, A. M. Cool1, J. Anderson2 1San Francisco State University, 2Space Telescope Science Institute. Exhibit Hall We report preliminary results from a study of main-sequence binaries (MSBs) in the core-collapsed globular cluster NGC 6397 using the Hubble Space Telescope (HST) Advanced Camera for Surveys. We analyze images of the central regions of the cluster extending out to approximately one half-mass radius (rhm = 2.33') taken with the Wide Field Channel in the F435W and F625W filters. After removing non-members using proper motions, we construct a color-magnitude diagram (CMD) containing 15578 cluster stars. Model cluster CMDs indicate that in the range 16 < R < 22, MSBs with mass ratio (q=M2/M1) >~ 0.6 appear sufficiently far above and redward of the main sequence ridge line to be distinguishable from the single-star sequence. Out of 10835 stars in this magnitude range, we identify an initial set of 137 stars (with primary masses in the range ~0.4-0.7 Msun) whose offset from the single-star sequence is statistically significant. A check of quality of fit to the PSF combined with close visual inspection of the images shows that ~85 of these stars are well measured and unresolved and are thus good MSB candidates. The resulting upper limit on the fraction of MSBs with q >~ 0.6 and primaries in the range 0.4-0.7 Msun is ~0.8%. We compare our measured fraction and the radial distribution of the MSB candidates to earlier findings based on HST/WFPC2 imaging and explore the significance of the results for the total binary population in NGC 6397. Keywords: binaries: general - globular clusters: individual(NGC 6397) - binary fraction - stars: main sequence binary 152.17 The Primordial Binary Fractions for a Sample of 35 Galactic Globular Clusters with HST Observations Jun Ji1, J. N. Bregman1 1University of Michigan. Exhibit Hall Binaries are thought to be the primary heating energy source in globular clusters, since they can convert their binding energy to kinetic energy of the encounter stars through dynamical interactions. Even a small fraction of binaries are sufficient to prevent globular clusters from core collapse for many relaxation times. But the observed global binary fractions in globular clusters are still uncertain. Here we present our preliminary results for the binary fractions of 35 Galactic globular clusters with the HST archival data in the F606W and F814W bands. We use the secondary sequence method on the color-magnitude diagram to statistically account for the main-sequence-main-sequence binaries (primordial binaries). The binary fraction is obtained by fitting the residual color distribution after subtracting the color of the main-sequence ridge line, with properly modeling the photometric errors, field stars, and blending stars. We estimate the binary fractions with 3 different assumed binary mass-ratio distribution functions, and the current data sets are still not good to constrain the binary mass-ratio distributions. In our sample, we obtain a mean binary fraction of (9.1±4.1)% within their half-mass radii assuming a flat binary mass-ratio distribution. There is no clear trend for the binary fractions against the dynamical ages and [Fe/H], but binary fractions tend to increase with the absolute magnitudes of clusters. This is probably because less massive globular clusters consume fewer binaries through dynamical interactions due to their lower stellar density. 152.18 Variable Stars in the Globular Cluster M14 Kyle E. Conroy1, A. N. Darragh2, Z. J. Liu2, B. W. Murphy2 1Villanova University, 2Butler University. Exhibit Hall Using the image subtraction method of Alard & Lupton (1998) we have searched for variable stars in the globular cluster M14 (NGC 6402). Image frames were obtained during June and July 2010 using two different telescopes, the Southeastern Association for Research in Astronomy (SARA) 0.9 meter at Kitt Peak National Observatory and the SARA 0.6 meter located at Cerro Tololo Interamerican Observatory. We confirmed 62 previously known variables catalogued by Wehlau & Froelich (1994). In addition to the previously known variables, we have identified 71 new variables. We have confirmed the periods of most of Wehlau & Froelich’s variables we identified with just a few exceptions. Of the total number of confirmed variables, we found a total of 112 RR Lyrae stars, several of which exhibited the Blazhko Effect. Of the total we classified 55 RR0, 57 RR1, 19 variables with periods greater than 2 days, a W UMa contact binary, and an SX Phe star. We present the periods of previously found variables as well as the periods, classification, and light curves of the newly discovered variables. This project was funded in part by the National Science Foundation Research Experiences for Undergraduates (REU) program through grant NSF AST-1004872 and by a grant from the Butler Institute for Research and Scholarship. 152.19 Interpreting Properties of Partially Resolved Stellar Clusters Lori Beerman1, L. C. Johnson1, J. J. Dalcanton1, B. F. Williams1 1University of Washington. Exhibit Hall Any study of stellar clusters invariably involves deriving the clusters' masses, ages, and metallicities. To determine these parameters, the light from stellar clusters has traditionally been studied in one of two regimes: as a ensemble of individual resolved stars, or as a single integrated value when stars cannot be individually resolved. When studying clusters residing within nearby galaxies with the Hubble Space Telescope, both resolved and unresolved components of the light must be considered. We simulate star clusters with a range of ages, masses, and metallicities, assuming various limiting magnitudes for resolving stars, to investigate properties of the resolved and unresolved flux components. In general, most of the light is resolved in younger clusters, while most is unresolved for older clusters, suggesting that multiple detection and measurement techniques are necessary when analyzing a sample spanning a wide range of cluster ages. We also confirm that significant variations in flux and color due to stochastic effects exist for clusters whose mass is less than 104 solar masses. However, we find that these effects are minimized when the brightest stars in a cluster can be resolved, and the light of the fainter, unresolved stars can be analyzed separately. These simulations can be used to shape survey design and analysis procedures in projects such as the ongoing Panchromatic Hubble Andromeda Treasury. 152.20 Deep HST Imaging in 47 Tuc and NGC 6397: The White Dwarf Cooling Sequence of 47 Tuc Harvey B. Richer1, J. Anderson2, A. Dotter2, G. Fahlman3, R. Goldsbury1, B. Hansen4, J. Hurley5, J. Kalirai2, I. King6, D. Reitzel4, R. Rich4, M. Shara7, P. Stetson3, K. Woodley1, D. Zurek7 1Univ. of British Columbia, Canada, 2STScI, 3HIA, Canada, 4UCLA, 5Swinburne University, Australia, 6University of Washington, 7AMNH. Exhibit Hall In Cycle 17 we were awarded 121 orbits with HST to search for the faintest stellar populations (the coolest white dwarfs, the lowest mass main sequence stars and possibly the brown dwarfs) in 47 Tucanae.  It took 10 months to secure all the data with exquisite care taken to minimize the effects of charge transfer and saturation spikes. The ACS stared at a single field for all 121 orbits but the roll angle of the telescope was varied through 180 degrees for the associated parallel fields observed with WFC3. Archival data were employed to proper motion clean the images allowing virtually complete separation of field stars and those in the background Small Magellanic Cloud from those in the cluster. In this poster, we present the resultant color-magnitude diagram for this important cluster which is a proxy for the Galactic bulge. A rich white dwarf cooling sequence is revealed which will be used to determine a cooling age for the cluster for comparison with the turnoff age (see associated poster by A. Dotter et al.). Multicolor data in other ACS filters as well as four filters with WFC3 are used to examine the spectral energy distributions of the cluster white dwarfs. 152.21 Deep HST Imaging in 47 Tuc and NGC 6397: WFC3 Panchromatic Imaging of 47 Tuc Jason S. Kalirai1, J. Anderson1, A. Dotter1, G. Fahlman2, B. Hansen3, J. Hurley4, I. King5, D. Reitzel3, R. M. Rich3, H. Richer6, M. Shara7, P. Stetson2, K. Woodley6, D. Zurek7 1Space Telescope Science Institute, 2HIA/NRC, Canada, 3UCLA, 4University of Swinburne, Australia, 5University of Washington, 6UBC, Canada, 7AMNH. Exhibit Hall In Cycle 17 our team was allocated 121 HST orbits to dissect the best studied globular cluster in the sky, 47 Tucanae. The HST ACS and WFC3 observations in this study represent one of the deepest images ever obtained for a nearby stellar population. In this poster, we present high-resolution UV and near-infrared imaging of the complete stellar populations of 47 Tuc over a wide field of view spanning a 180 degree azimuthal range and >10 pc radial range in the star cluster. The combined WFC3/UVIS and IR observations in each of these fields extends from well below the hydrogen burning limit in the red, up through the main sequence to the brightest giants in post main-sequence evolution in the visible, and down to the white dwarf cooling sequence in the blue. This complete stellar picture of a globular cluster has revealed several new features of the color-magnitude diagram and represents a comprehensive data base to test stellar evolution models in exquisite detail. In addition to the primary focus of studying 47 Tuc, our imaging penetrates through the star cluster to reveal a rich population of background giants and low mass dwarfs belonging to the distant Small Magellanic Cloud. 152.22 Deep HST Imaging in 47 Tuc and NGC 6397: Main Sequence Turnoff Ages Aaron L. Dotter1, J. Anderson1, G. Fahlman2, B. Hansen3, J. Hurley4, J. Kalirai1, I. King5, D. Reitzel3, R. M. Rich3, H. Richer6, M. Shara7, P. Stetson2, K. Woodley6, D. Zurek7 1Space Telescope Science Institute, 2HIA, Canada, 3UCLA, 4Swinburne University, Australia, 5University of Washington, 6UBC, Canada, 7AMNH. Exhibit Hall The ages of Galactic globular clusters provide insight into the formation history of the Milky Way. Utilizing HST photometry of unprecendented depth and wavelength coverage, we determine the main sequence turnoff ages of the nearby globular clusters NGC 6397 and 47 Tuc. The ages are determined by comparing stellar evolution models to the main sequences with a chi-squared minimization technique. Our analysis of 47 Tuc leverages the pronounced 'kink' or 'knee' feature that appears in the lower main sequence in the near-IR. We present our age estimates as probability distributions and construct confidence intervals over input parameters such as metallicity, distance, and reddening. 152.23 Deep HST Imaging in 47 Tuc and NGC 6397: Variable Stars in 47 Tuc Kristin Woodley1, J. Anderson2, S. Bickerton3, A. Dotter2, G. Fahlman4, B. Hansen5, J. Hurley6, J. Kalirai2, I. King7, R. M. Rich5, H. Richer1, M. M. Shara8, P. Stetson4, D. Zurek8 1University of British Columbia, Canada, 2STScI, 3Princeton University, 4HIA/NRC, Canada, 5UCLA, 6Swinburne University of Technology, Australia, 7University of Washington, 8American Museum of Natural History. Exhibit Hall We have obtained 121 orbits of Hubble Space Telescope imaging observations of the Milky Way globular cluster, 47 Tucanae, from which we can search for stellar variability and transits. Our differential time series photometry covers two fields located outside the cluster core. The first field was observed with the Advanced Camera for Surveys in F606W and F814W covering a 10 month time period and yielding a sample of 20 000 stars. The second field was observed with the Wide Field Camera 3 in F110W and F160W covering 15 days and yielding an approximate sample of 10 000 stars. In this poster, we present the results of our various evaluation methods including phase dispersion minimization and a modified Lomb-Scargle periodogram to identify candidate variables and to determine their periods. 152.24 Deep HST Imaging In 47 Tuc And NGC 6397: Helium-core White Dwarfs In The Core Of NGC 6397 Ryan Goldsbury1, K. Woodley1, J. Anderson2, A. Dotter2, G. Fahlman3, B. Hansen4, J. Hurley5, J. Kalirai2, I. King6, R. M. Rich4, H. Richer1, M. Shara7, P. Stetson3, D. Zurek7 1UBC, Canada, 2STScI, 3HIA/NRC, Canada, 4UCLA, 5U. Swinburne, Australia, 6U. Washington, 7AMNH. Exhibit Hall We present a detailed analysis of a population of helium-core white dwarfs in the core of the Galactic globular cluster NGC 6397. We analyze the radial distribution of these objects compared to the distributions of various other populations of known mass within the this cluster. From this comparison we are able to determine the average mass of the helium-core white dwarfs and their possible binary companions. We find that their distribution is inconsistent with the expected mass range of low-mass white dwarfs, but may be explained by the presence of massive companions to these objects. We also analyze the spectral energy distributions of the He-core white dwarfs to place constraints on the nature of their unresolved partners. 152.25 Deep HST Imaging in 47 Tuc and NGC 6397: Discovery of Dwarf Novae from the Cluster Core Data David Zurek1, J. Anderson2, A. Dotter2, G. Fahlman3, B. Hansen4, J. Hurley5, J. Kalirai2, I. King6, R. M. Rich4, H. Richer7, M. M. Shara1, P. Stetson3, K. Woodley7 1American Museum of Natural History, 2Space Telescope Science Institute, 3HIA/NRC, Canada, 4University of California at Los Angeles, 5Swinburne University of Technology, Australia, 6University of Washington, 7University of British Columbia, Canada. Exhibit Hall We have looked for dwarf novae eruptions in the cluster cores of both 47 Tuc and NGC 6397. The cluster cores were imaged in parallel when the deep white dwarf field was imaged. We have also included archival images of the cluster cores taken with WFPC2, ACS and WFC3. We describe here all the data, our methodology and the total number of dwarf novae discovered. We explore what the number of dwarf novae implies about the total population in the cluster core. 152.26 Deep HST Imaging In 47 Tuc And NGC 6397: Stellar Dynamics On The Outskirts Of NGC 6397 Jeremy S. Heyl1, J. Anderson2, A. Dotter2, G. Fahlman3, B. Hansen4, J. Hurley5, J. Kalirai2, I. King6, R. M. Rich4, H. Richer1, M. Shara7, P. Stetson3, K. Woodley1, D. Zurek7 1UBC, Canada, 2STSci, 3HIA/NRC, Canada, 4UCLA, 5U. Swinburne, Australia, 6U. Wash., 7AMNH. Exhibit Hall Multi-epoch observations with ACS on HST provide a unique and comprehensive probe of stellar dynamics within NGC 6397. We are able to confront analytic, Monte Carlo and nbody models of the globular cluster with the observed stellar proper motions . The observations probe well along the main sequence from 0.5 to below 0.1 solar masses as well as white dwarfs younger than one gigayear. The observed field lies beyond the half-light radius where standard models of globular cluster dynamics (e.g. based on a lowered Maxwellian velocity distribution) make very robust predictions for the stellar proper motions as a function of mass. The observations agree with the models for the main sequence stars; however, the proper motions of the young white dwarfs are somewhat puzzling, and we examine some possible explanations. 152.27 Deep HST Imaging in 47 Tuc and NGC 6397: White Dwarfs and Brown Dwarfs in the Cluster and Field of NGC 6397 Robert Michael Rich1, J. Anderson2, A. Dotter2, B. Hansen1, H. Richer3, G. Fahlman4, J. Hurley5, J. Kalirai2, I. King6, D. Reitzel7, M. Shara8, P. Stetson4 1UCLA, 2STScI, 3UBC, Canada, 4HIA/NRC, Canada, 5Swinburne University, Australia, 6University of Washington, 7UCLA & Griffth Obs, 8AMNH. Exhibit Hall We report analysis of second epoch imaging of the very deep 126 orbit ACS integration in NGC 6397, yielding the deepest proper-motion selected color-magnitude diagram of a globular cluster. We reach past the faint end of the white dwarf cooling sequence and confirm the "blue hook" caused by H2 collision-induced absorption opacity. We also confirm a suspected population of faint red proper-motion members of NGC6397, many of which lie both fainter and redder than the theoretical limit for the hydrogen burning. Other proper motion members of NGC 6397 (with unusual colors) may be white dwarf/red dwarf binaries. Our reduced proper motion plot for the field reveals (for the first time) an extended white dwarf cooling sequence in the thick disk population, along with a well populated sequence of extremely faint red stars, many of which are also fainter and redder than the theoretical hydrogen burning limit. Supported by AURA STScI GO-11633 (R. M. Rich, PI) 152.28 Was the Progenitor of the Sagittarius Stream a Disc Galaxy? Recent Results & Observations. Elaina A. Hyde1, D. B. Zucker1, J. Penarrubia2, M. Irwin2, R. Lane3, G. F. Lewis3, G. Gilmore2, A. Koch4 1Macquarie University, Australia, 2Institute of Astronomy, University of Cambridge, United Kingdom, 3The University of Sydney, Australia, 4University of Leicester, United Kingdom. Exhibit Hall Wrapping around the Milky Way, the Sagittarius (Sgr) stream is one of the most dramatic examples of a stellar tidal stream currently known. Its progenitor, the Sgr dwarf galaxy, has been assumed to be a non-rotating, pressure-supported dwarf spheroidal galaxy. However, to date, no such model for the interaction of Sgr with the Milky Way has been able to reproduce all of the observational features of the stream. Recent theoretical models proposing that the progenitor was a rotating disc galaxy may provide a solution; in particular, the bifurcation of the leading tail of the Sgr stream detected in the SDSS survey naturally arises in models where the Sgr disc is misaligned with respect to the orbital plane. If Sgr was in fact a disc galaxy, these models predict that the core should still show residual internal rotation with a measurable amplitude (~ 20 km/s). We have obtained spectra of over 2000 stars near the core of Sgr with AAOmega on the AAT in order to test the disc-galaxy hypothesis, and we present here our preliminary results, along with a comparison to model predictions. 152.29 The Nearest Old Cluster: Ruprecht 147 Jason L. Curtis1, J. T. Wright1 1The Pennsylvania State University. Exhibit Hall Ruprecht 147 is a hitherto unappreciated open cluster that holds great promise as a standard in fundamental stellar astrophysics. At 200 pc and an age of 2 Gyr, it is the closest old cluster by factor of more than 2 in each dimension. Two previously published member lists in the literature have either completely misidentified, or have only partially identified, the cluster’s stellar population. We are amidst a multi-telescope campaign to characterize R147 and catalog its members and prove its benchmark status. We have identified over 100 members including 5 blue stragglers, obtained first epoch astrometry, and derived four-color optical photometry of the cluster core (CFHT/MegaCam) . The K and M dwarfs of Ruprecht 147 will be the only old, single, cool dwarfs with known ages bright enough to admit close spectroscopic study (so far, Ca II H&K with MMT/Hectochelle). 152.30 Ionizing Sources of Extragalactic HII Regions: Tight Clusters vs. Distributed OB Associations Jessica Marie Evans1, Y. Chu1 1University of Illinois. Exhibit Hall Extragalactic giant HII regions (EGHRs) are sites of active, concentrated star formation, providing ideal labs to analyze starburst phenomenon. The most interesting starburst issue is whether a tight cluster forms and later becomes a globular cluster or distributed OB associations form and later disperse. The two nearest EGHRs serve as standards for each; 30 Dor in the Large Magellanic Cloud hosts a dominant cluster and NGC 604 in M33 hosts multiple OB associations. To investigate the mode of star formation in EGHRs, we have searched the Hubble Legacy Archives (HLA) and identified a sample of >50 EGHRs in galaxies closer than 15 Mpc, limiting our selection by an H-alpha luminosity threshold of 1.5 x 1040 ergs s-1. Binned images of 30 Dor and NGC 604 in continuum bands are used to simulate clusters and distributed OB associations at distances of the EGHRs in our HLA sample. We have analyzed the continuum images of the EGHRs and compared them with the simulated images of 30 Dor and NGC 604 in order to assess whether the ionizing source is dominated by a tight cluster or distributed OB associations. We have also correlated the modes of star formation in EGHRs with the types of their host galaxies and their location within them. Implications of our results on starbursts and formation of EGHRs will be discussed. 152.31 X-Ray Sources in the Rich Open Cluster NGC 6819 Natalie M. Gosnell1, D. Pooley2, J. S. Kalirai3, A. M. Geller4, R. D. Mathieu1, P. Frinchaboy5, E. Ramirez-Ruiz6 1University of Wisconsin-Madison, 2Eureka Scientific Inc., 3Space Telescope Science Institute, 4Northwestern University, 5Texas Christian University, 6University of California. Exhibit Hall We present the first study of the X-ray population of the intermediate-age rich open cluster NGC 6819 using the XMM-Newton Observatory. In the past decade, Chandra X-ray observations have shown a relationship between the X-ray population of globular clusters and their internal dynamics and encounter frequency. We investigate whether a similar link exists in open clusters, utilizing X-ray and UV data from XMM-Newton observations of eight rich open clusters, along with the wealth of photometry and radial velocity data from the WIYN Open Cluster Study (WOCS) and the CFHT Open Cluster Study. These results on NGC 6819 are the first of our investigation. Within the cluster apparent diameter, we detect 11 sources in NGC 6819 down to a luminosity of 1030 ergs/s for cluster members. Sources are classified by taking into account their broadband X-ray/UV/optical spectral properties. We gratefully acknowledge support from XMM grant NNX08AY27G from the National Aeronautics and Space Administration. 152.32 A Closer Look at Cyg OB2 using the HST Fine Guidance Sensors Saida M. Caballero-Nieves1, D. R. Gies1, E. P. Nelan2 1Georgia State University, 2Space Telescope Science Institute. Exhibit Hall We present results of a survey of 58 young OB stars in Cygnus OB2 that we made with the Fine Guidance Sensor 1r (FGS1r) on the Hubble Space Telescope. FGS1r in its high angular resolution TRANS mode is ideal for detecting binaries with angular separations as small as 0.012" with modest magnitude differences. We found that 22.4% of our sample are members of multiple systems (one triple detected). Using adaptive optics imaging in the infrared, we confirm 11 of the 13 multiple systems. 152.33 Measuring Spectra of B-type Stars to Study Young Open Clusters Charisee Chiw1, M. V. McSwain2 1Gettysburg College, 2Lehigh University. Exhibit Hall We used spectra of the open clusters NGC 1960, NGC 1502, NGC 7160, NGC 2384, NGC 2244, NGC 2422, and IC 1590 to analyze their B-type stellar populations. The spectral lines He I ??4388, 4713, 4471, and H? at 4340 Å were analyzed to measure the stars’ projected rotational velocity, temperature, and surface gravity. Then by comparing our measurements to the evolutionary tracks of Schaller et al., we determined the masses of the stars. We determined the ages of the clusters by comparing the luminosity and temperature measurements to isochrones by Lejeune & Schaerer. Finally, we calculate the interstellar reddening and distance to each cluster. This work is supported by the NSF REU site grant PHY-0849416, NASA DPR No. NNX09AP86G, and Lehigh University. 152.34 Two Detached Eclipsing Binaries near the Turnoff of the Open Cluster NGC 6819 Mark Jeffries1, E. L. Sandquist1, R. D. Mathieu2, A. M. Geller2, J. A. Orosz1, M. D. Shetrone3 1San Diego State University, 2University of Wisconsin, 3McDonald Observatory. Exhibit Hall We analyze extensive BVRcI c photometry and radial velocity measurements for Auner 259 and 537, two detached eclipsing binaries (DEBs) that are double-lined members of the moderately old (?2.5 Gyr) cluster NGC 6819. We present results of binary star modeling to measure characteristics of the components, focusing on stellar masses and radii because the binaries reside near the cluster turnoff in a color-magnitude diagram. The masses and radii will provide constraints on the cluster age. We gratefully acknowledge funding from the National Science Foundation under grant AST-0908536 and AST-0908082. 152.35 Testing Star Cluster Disruption Scenarios: Accurate Age Distributions Allison M. Widhalm1, G. Trancho1, N. Bastian2 1Gemini South Observatory, 2IoA/ Cambridge, United Kingdom. Exhibit Hall Due to their intrinsic brightness, star cluster populations hold the potential to accurately probe the SFH of galaxies out to distances of 10 - 100 Mpc. Their diagnostic quality, however, is limited by a poor understanding of the process of cluster disruption. Specifically, two competing empirical scenarios have been proposed, one that proposes a disruption timescale that is dependent on the cluster’s mass (eg., Lamers et al. 2005), and the other which finds no such correlation (e.g., Fall et al. 2005). As Larsen (2009) has recently noted, the two scenarios predict different age-luminosity relationships, and consequently determining the correct scenario is of utmost importance. Here we present preliminary results of the 20 brightest clusters of 3 spiral galaxies to help distinguish between these scenarios. 152.36 An Age-Sensitive Binary Star Near the Turnoff of the Open Cluster M11 Ernest Bavarsad1, E. L. Sandquist1, J. A. Orosz1, M. D. Shetrone2 1San Diego State University, 2McDonald Observatory. Exhibit Hall We present extensive BVRC photometry and radial velocities for the detached eclipsing binary KV29 in the intermediate-age open cluster M11. Spectroscopy shows that the system is double-lined and is a member of the cluster. We will present the results of binary star modeling to measure the characteristics of the components. In particular, we focus in particular on the masses and radii of the components because the binary resides near the cluster turnoff in a color-magnitude diagram, and the size evolution of the brighter component leads to a strong constraint on the cluster age. We gratefully acknowledge funding from the National Science Foundation under grant AST-0908536. 152.37 Detailed Chemical Abundances of NGC 5128 Globular Clusters using High Resolution Spectroscopy Maria Duran1, R. Bernstein1 1University of California Santa Cruz. Exhibit Hall Our current understanding of chemical evolution, nucleosynthesis and galaxy assembly is based largely on stellar abundance studies of old stars in only one galaxy: the Milky Way (MW). Unfortunately, beyond the MW and it's nearest neighbors, old (red giant branch) stars are too faint to observe at the high spectral resolutions(>= 20,000) and high signal-to-noise ratios (SNR >= 60)required for the analysis of individual absorption lines. While young stars can be studied at larger distances, they only record the recent gas-phase abundances. To enable chemical abundance studies of old stars at larger distances, we have developed a method to analyze high resolution (R ~ 20,000) integrated light (IL) spectra of extragalactic Globular Clusters (GCs). GCs are unique tracers of the formation histories of galaxies; they form throughout the lifetimes of galaxies in episodes of rapid star formation (SF) and their properties are known to correlate strongly with the properties of the host galaxy (see Brodie & Strader 2006). We have demonstrated that our GC analysis provides abundances that are as accurate as standard abundance analysis of individual RBG stars, as well as accurate ages for clusters between 0.1 and 13 Gyrs. Here, we present the first detailed chemical abundances (alpha, Fe-peak, and neutron capture elements) and ages for a sample of 5 GCs in NGC 5128, the nearest E/S0 galaxy. 152.38 WIYN Open Cluster Study: Spectroscopic Abundances of M34 from the Oxygen Triplet Region Scott Adams1, R. M. Maderak2, C. P. Deliyannis2 1University of Arizona, 2Indiana University. Exhibit Hall Oxygen has been suggested as a superior chronometer to iron for studying Galactic chemical evolution. Open clusters are an ideal tool for studying abundance-age relationships, given their knowable age and uniform chemical composition. As part of a larger study to investigate the O-age relationship found by King (1993) we obtained high-resolution spectra of the oxygen triplet region for 49 candidate dwarf members in M34, age 225 Myr, using the HYDRA multi-object spectrometer on the WIYN 3.5m. The following results are based on the 38 of these 49 candidate members that turned out to be slowly-rotating single-star radial velocity members. We report weighted cluster average abundances of [Fe/H] = 0.16 ± 0.03, [O/H] = 0.06 ± 0.06, [Al/H] = -0.02 ± 0.02, [Ni/H] = 0.36 ± 0.02, and [Si/H] = -0.01 ± 0.01. Each error includes two components added in quadrature: one component is simply the standard deviation of the mean of all the cluster lines included in the average, and the other component is related to the standard deviation of the mean in the Teff, for each star, that arises from the use of multiple color indices for the derivation of Teff. Our low [O/Fe] is inconsistent with the supersolar [O/Fe] suggested by King for young clusters. 152.39 Open Cluster Neutron Capture Element Abundances and the Chemical Evolution of the Milky Way Disk Heather R. Jacobson1, E. D. Friel2, C. A. Pilachowski3 1Michigan State Univ., 2Boston University, 3Indiana University. Exhibit Hall Open clusters are versatile probes of the chemical abundance distribution of the Milky Way disk. Recent years have seen a steady increase in the number of open clusters subject to high resolution spectroscopic study, including the development of large samples of (10-20) clusters analyzed homogeneously. While abundances of Fe-peak, light and alpha elements in open clusters have been studied in great detail, cluster neutron capture element abundance information is relatively sparse and largely inhomogeneous, save for the barium study of D'Orazi et al. (2009). Neutron capture elements are formed in Type II supernovae and in late stages of evolution in low mass stars, and therefore yield important clues to the chemical enrichment history of the galaxy. We have undertaken a study of Ba, La and Eu abundances in some two dozen open clusters based on KPNO 4m echelle spectra and archival high resolution spectra from Keck and VLT. Our sample has a comparable range in age to the D'Orazi et al. (2009) sample and covers Galactocentric distance Rgc~7 - 22 kpc. Analyses of the first 11 clusters, using a spectrum synthesis technique, confirm the surprising inverse correlation between the abundance of Ba and cluster age in giants first noted by D'Orazi et al. (2009), but full confirmation awaits a larger cluster sample. We also search for similar trends in La and Eu abundances. Here we present the preliminary results of this ongoing analysis. We also search for abundance trends with cluster location in the Galaxy and compare cluster abundance patterns to those of other disk populations, which will yield clues to the formation and evolution of the Milky Way disk. This research is supported by a National Science Foundation Astronomy and Astrophysics Postdoctoral Fellowship to HRJ under award AST-0901919. 152.40 Astrometry with the Hubble Space Telescope: Improved Trigonometric Parallaxes of Selected Hyads G. Fritz Benedict1, B. E. McArthur1, W. F. van Altena2, T. E. Harrison3 1Univ. of Texas, Austin, 2Yale University, 3New Mexico State University. Exhibit Hall We present absolute parallaxes and proper motions for seven members of the Hyades open cluster, pre-selected to lie in the core of the cluster. We obtain Hyad parallaxes with archival astrometric data from Fine Guidance Sensor (FGS) 3, combined with newer data for 3 Hyads from FGS 1R, both white-light interferometers on the Hubble Space Telescope. Proper motions, spectral classifications and VJHK photometry of the stars comprising the astrometric reference frames provide spectrophotometric estimates of reference star absolute parallaxes. Introducing these into our model as observations with error, we determine absolute parallaxes for each Hyad. Compared to our original (van Altena et al. 1997) determinations, our combination of new data and improved analysis lowered the individual parallax errors by an average factor of 2.9. Comparing with the four stars contained in the Hipparcos catalog, we obtain an average factor of seven improvement. Our parallax values now more closely agree with Hipparcos for the four stars in common. Additionally, we measure a perturbation orbit for vA 627, previously identified as a spectroscopic binary. Incorporating a perturbation in the modeling improves the parallax accuracy for this Hyad. We gratefully acknowledge support from NASA, through the Space Telescope Science Institute, grants AR-11746 and GO-11942. 153 Stellar Evolution, Stellar Populations Poster Session Exhibit Hall 153.01 The Quest For The Sun's Siblings: An Exploratory Search In The Hipparcos Catalogue Jennifer Bean1, A. Brown2, S. Portegies Zwart2 1Missouri State University, 2Leiden University, Netherlands. Exhibit Hall We describe the results of a search for the remnants of the Sun's birth cluster among stars in the Hipparcos Catalogue. This search is based on the predicted phase-space distribution of the Sun's siblings from simple simulations of the orbits of the cluster stars in a smooth Galactic potential. For stars within 100 pc, the simulations show that it is interesting to examine those that have small space motions relative to the Sun. From amongst the candidate siblings thus selected, there are six stars with ages consistent with that of the Sun. Considering their radial velocities and abundances only one potential candidate, HIP21158, remains, but essentially the result of the search is negative. This is consistent with predictions by Portegies Zwart on the number of siblings near the Sun. We discuss the steps that should be taken in anticipation of the data from the Gaia mission in order to conduct fruitful searches for the Sun's siblings in the future. 153.02 Expanding our Knowledge of the Chemical Composition of Nearby Stars Michael D. Pagano1, P. Young1, P. Butler2 1Arizona State University, 2Carnegie Institute of Washington. Exhibit Hall I will be presenting abundances of X elements and physical properties for a selection of nearby radial velocity planet search candidates. The abundances are derived from high resolution spectra from MIKE on Magellan. These are the first results of an attempt to create a uniform high resolution chemical abundance database that can be used to understand the chemical evolution of nearby stars, in particular those with potentially habitable worlds. These high resolution spectra are the first from a group of 600 nearby stars, obtained by Paul Butler(Carnigie Institute of Washington). 153.03 A New Digital S Star Atlas and Its Uses Elizabeth Otto1, P. Green2, D. Mink2 1The Ohio State University, 2Harvard-Smithsonian Center for Astrophysics. Exhibit Hall S and carbon (C) stars are traditionally thought to be on the asymptotic giant branch because of their high C/O ratios and enhanced s-process elements. A sample of S stars at high Galactic latitudes would help us understand their formation and evolution in disk to halo populations, at a variety of metallicities and with minimal reddening. Faint S stars would either be at large Galactocentric radii, or dwarfs. S dwarfs are in analogy to dwarf C stars, which are thought to originate from mass transfer in a binary system. Dwarf C stars are now known to be the numerically dominant type of C star in the Galaxy, but no S dwarfs have ever been found. Their discovery and knowledge of their space density could closely constrain some of the many available channels of binary evolution. The Sloan Digital Sky Survey (SDSS) seems an ideal place to find faint S stars, but the colors of these stars are largely unknown, since all known S stars (median V magnitude of ~10.5) are saturated in the SDSS. We use the FAST spectrograph on the Tillinghast reflector on Mt. Hopkins to obtain the spectra of 57 known S stars that appear in the Two-Micron All Sky Survey (2MASS). We flux calibrate these spectra, provide them electronically as a digital atlas, and convolve them with SDSS bandpasses to generate likely colors for S giants and dwarfs. We find that these S star colors are not clearly distinguished from the colors of M giants and C stars. We also present initial results of a cross-correlation with the SDSS spectral database, using the FAST spectra as templates. This work is supported in part by the NSF REU and DOD ASSURE programs under NSF grant no. 0754568 and by the Smithsonian Institution. 153.04 Finding the Odd One Out in Large Spectroscopic Surveys Andrew J. Connolly1, S. Daniel1, L. Xiong2, J. VanderPlas1, J. Schneider2 1Univ. of Washington, 2Carnegie Mellon University. Exhibit Hall Through shear volume of data, next generation surveys will provide us with unprecedented and detailed information about the full distribution of astronomical sources. Anomalous events influenced by the the most extreme and interesting physics will no longer be relegated to the dustbin of "small number statistics." Unfortunately, that same volume of data will render the task of culling these extreme events from the background of ordinary stars and galaxies virtually impossible. Both the number of events and the dimensionality of the data (e.g. a spectral energy distribution measured in 4000 wavelength bins) exist well outside the reasonable limits of human processing In this context, we seek algorithms to project N>>1 dimensional data down to 2 or 3 effective dimensions, preserving the physics of the correlations within the unprojected data. Inspection in these effective dimensions then allows us to identify both objects that resemble one another (classification of objects) and objects that resemble nothing at all (anomaly detection). We consider both Principal Component Analysis, which attempts the projection under the assumption that any given data point can be reconstructed from a linear combination of all other data points, and Local Linear Embedding, which attempts to reconstruct data points only from their nearest neighbors, preserving the non-linear relationships between different neighborhoods. We use stellar spectra from the SDSS to show how these techniques can identify interesting classes of astronomical sources. We acknowledge support from the DOE Applied Mathematics Program DE-FG02-87ER40315 153.05 Stellar Rotation and Activity at 1 Gyr: The Palomar Transient Factory Does NGC 752 Marcel A. Agueros1, P. A. Cargile2, K. R. Covey3, A. L. Kraus4, N. M. Law5, K. G. Stassun2 1Columbia Univ., 2Vanderbilt Univ., 3Cornell Univ., 4Univ. of Hawaii, 5Univ. of Toronto, Canada. Exhibit Hall Large uncertainties remain in our picture of the evolution of stellar rotation and activity in Sun-like stars after they reach the age of the Hyades, roughly 0.5 Gyr. Rotation periods are scarce for stars at these ages, seriously complicating the calibration of an age-rotation-activity relation that could be applied to field stars. The Columbia/Cornell/Caltech Palomar Transient Factory (CCCP) survey of open clusters is an effort to systematically map stellar rotation in nearby open clusters. We present preliminary results from our on-going CCCP campaign on NGC 752, a ~1 Gyr open cluster for which we have several hundred individual R-band observations. At a distance of only ~450 parsecs, and with deep archival X-ray observations, it represents the best opportunity we have to study the age-rotation-activity relation in main sequence stars at an age about a quarter that of the Sun. 153.06 The Columbia/Cornell/Caltech Palomar Transient Factory (CCCP) Praesepe Campaign: Studying the Rotation-Activity Relation in an Intermediate Age Cluster Kevin R. Covey1, J. Lemonias2, M. Agueros2, N. Law3, A. Kraus4, K. Hamren1 1Cornell University, 2Columbia University, 3University of Toronto, 4University of Hawaii, Monoa. Exhibit Hall For several decades, observational surveys have demonstrated a closerelationship between a star’s rotation period, magnetic activity, and age. The age-activity-rotation relation is well documented in clusters younger than 500 Myrs, but its subsequent evolution is less clear. Using wide-field, multi-epoch photometry from the Palomar Transient Factory, we have monitored ~530 members of the Praesepe open cluster, a ~600 Myr nearby Hyades analog. With light curves containing >150 measurements over more than three months, we have measured rotation periods for ~50 K & M-type cluster members. These rotation periods span the gap between the periods measured for solar-type Hyads and the lowest-mass Praesepe members, and indicate that the orderly mass-rotation relation seen for higher mass Praesepe members begins to break down at ~0.6 Msun. Below this critical mass, a range of rotation periods spanning an order of magnitude are observed for stars with similar masses. Combining these rotation measurements with archival X-ray and Halpha observations completes the portrait of the ~600 Myr age-activity-rotation relation, and enables a detailed comparison with Praesepe's sister cluster, the Hyades. 153.07 TripleSpec Observations of Candidate PTF Eclipsing Binaries Katie Hamren1, K. Covey1, N. Law2, M. Agueros3, J. Lemonias3, A. Kraus4 1Cornell University, 2University of Toronto, Canada, 3Columbia University, 4University of Hawaii. Exhibit Hall The Columbia-Cornell-Caltech Palomar Transient Factory (CCCP) survey is designed to obtain stellar rotations in a number of nearby open clusters. Among the interesting objects detected in CCCP fields observed to date are several candidate eclipsing binaries with M star primaries. These systems, whether in the field or in our target clusters, are ideal laboratories for testing models for the masses and temperatures of late-type stars. The challenge is in obtaining and analyzing the high quality follow-up spectroscopy that is required for these tests. Here we report on our use of the near-infrared TripleSpec spectrometer on the 200-inch telescope at Palomar Observatory to follow up on these interesting systems. While these observations are of moderate resolution (R ? 3000), they do provide sufficient traction to constrain the radial velocity separation of the two components of the binary, allowing us to place constraints on the orbits of these systems. 153.08 Chemical Compositions of Field Red Horizontal Branch Stars Melike Afsar1, C. Sneden1, B. For1 1The University of Texas at Austin. Exhibit Hall Field Red Horizontal Branch stars (RHBs) are alleged to be members of the thick disk of our Galaxy and are an important evolutionary link between horizontal and asymptotic giant branch evolution. They are easy to identify in globular clusters through their color-magnitude diagram positions. However, they are harder to identify as single stars in the general field; thus they have received lesser attention to date. In this study, we composed a large catalog of RHB candidates and performed the first large-sample high-resolution spectroscopic survey of these stars. We have obtained high resolution spectra of a number of candidate field RHBs. The high resolution spectra of these stars were taken with the 2.7m Harlan J. Smith Telescope and Tull 2Dcoude (R=60000) spectrometer at McDonald Observatory. We have derived the metallicities and relative abundance ratios for some of the alpha (Ca and Si) and neutron capture (La and Eu) elements along with the fundamental stellar parameters. We have also determined CNO abundances in order to gain insight into the evolutionary states of the candidates. In particular, we have investigated the 12C/13C ratio using the CN features present in the 8000-8040 A region, which we have also used to obtain the N abundances of the candidates. Plausible RHB stars, members of the thick disk, found in our study, can shed light into Galactic evolutionary models. This project has benefitted from the financial support of NSF (AST-0908978), the Rex G. Baker endowment to the University of Texas Astronomy Dept., and The Scientific and Technological Research Council of Turkey (TUBITAK). 153.09 Looking for Metallicity Spread in Clusters Using HST/WFC3 Multiband Photometry Daniel Oravetz1, J. A. Holtzman1 1New Mexico State University. Exhibit Hall We describe efforts to study the internal distribution of metallicites in stellar clusters using multiband HST/WFC3 images that include observations in filters that are designed to be more sensitive to metallicity than standard broadband filters. We analyze observations of NGC 6791, NGC 5927, NGC 104, NGC 6752, and M92, which span a range of metallicities, -2.2 < [Fe/H] < 0.35. We search for metallicity spread by comparing the observed width of the stellar locii in several different color indices to the spread expected from photometric errors. 153.10 Calibrating Measurement of Stellar Metallicities from Multiband HST/WFC3 Photometry Jon A. Holtzman1, B. Anthony-Twarog2, H. Bond3, D. Oravetz1, A. Saha4, B. Twarog2, A. Walker5 1New Mexico State Univ., 2Univ. of Kansas, 3STScI, 4NOAO, 5CTIO. Exhibit Hall We present initial results from a HST/WFC3 calibration project to understand how well stellar metallicities can be determined from multiband photometry that includes filters specifically designed for helping to derive stellar parameters. We report on observations taken in a suite of 11 filters: F336W, F390M, F390W, F395N, F410M, F467M, F547M, F555W, F814W, F110W, and F160W. Data in these filters was obtained in five Milky Way clusters -- M92, NGC6752, NGC104, NGC5927, and NGC6791 -- that span a large range in metallicity. The resulting stellar sequences are compared with model predictions, and results on the most promising metallicity indicators are discussed. 153.11 Chemical Abundances in Carbon-enriched Metal-poor Stars Anna Kwa1, J. Johnson1, T. Masseron2, D. Lai3, M. Bolte3, S. Lucatello4 1Ohio State University, 2Université Libre de Bruxelles, Belgium, 3UCO/Lick Observatory, 4Osservatorio Astronomico di Padova, Italy. Exhibit Hall The metal-poor population II stars in the Galactic halo formed during the first few generations of star formation following the Big Bang, and can thus provide key insights into conditions in the early Universe. Carbon-enriched metal-poor (CEMP) stars, a subset of this population, are of even further interest because of their peculiar chemical abundance patterns. High-resolution spectra of ten known CEMP stars were obtained on the Keck High Resolution Echelle Spectrometer (HIRES) for this study. Stellar parameters for our model atmospheres were determined using Fe I and Fe II equivalent width measurements. We derived chemical abundances from measured equivalent widths whenever possible, or from synthetic spectra in the cases where no equivalent widths could be measured for an element’s spectral lines. Using these methods, we have obtained preliminary abundances for up to 28 elements in our sample. Further work remains in introducing carbon into the model atmospheres and repeating the abundance analysis using these revised models. We can then study the relative abundances of heavy elements in comparison to solar system r-process and s-process abundance patterns in order to infer possible mechanisms by which these stars became carbon-enriched. 153.12 The Chemical Composition of Bulge Stars in Plaut's Window Christian I. Johnson1, R. M. Rich1, J. P. Fulbright2, D. B. Reitzel3 1University of California, Los Angeles, 2Johns Hopkins University, 3Griffith Observatory. Exhibit Hall We present chemical abundances for ~100 red giant branch (RGB) and red clump stars in Plaut's low-extinction window (l,b)=(0°,-8°). The abundances were determined from equivalent width and spectrum synthesis analyses of high resolution (R=22,000), high signal-to-noise (S/N~50-100) spectra obtained with the Blanco 4m telescope and Hydra multifiber spectrograph. We confirm the existence of a vertical metallicity gradient along the Galactic bulge minor axis and that the median metallicity at b=-8° is [Fe/H]~-0.3. However, the red clump stars in this field appear to be both selectively enhanced in metallicity, with a median [Fe/H]~0, and have at least a factor of two smaller radial velocity dispersion than the RGB stars. Interestingly, both the giants and clump stars exhibit similar enhanced [alpha/Fe] ratios compared to the thin and possibly thick disk trends, and the b=-8° [alpha/Fe] ratios are indistinguishable from those at b=-4°. Lastly, we compare the abundances of several additional light and heavy elements in Plaut's Window to those in other bulge fields and stellar populations. 153.13 The Chemical Composition of Globular Cluster M68 Sloane K. Simmons1, C. Sneden1, G. Preston2, I. Thompson2, J. Sobeck3, S. Shectman2 1University of Texas, 2Carnegie Observatories, 3University of Chicago. Exhibit Hall We present a chemical composition study of twenty-five stars in the metal-poor Galactic globular cluser M68. We obtained high-resolution spectra (R ~ 40,000) in the wavelength region 3500-9000 A for the target stars with the the Magellan Inamori Kyocera Echelle (MIKE). The observed stars include 11 red giant branch (RGB) stars, 9 red horizontal branch (RHB) stars, and 5 blue horizontal branch (BHB) stars, which span an effective temperature range of approximately 5000K. The abundances were determined through equivalent width and synthetic spectrum analyses. The computations considered isotropic, coherent scattering in the continuum source functions. Sample stars from each group were analyzed using model atmospheres from the MARCS and ATLAS grids. We find a generally consistent metallicity across all the evolutionary groups: [Fe/H] = -2.4 (RMS deviation = 0.1). However, we note that the mean RHB metallicity is ~0.15 dex less than the overall average. The relative abundance ratios of the alpha elements are typical for low metallicity stars: [Ca/Fe] = [Ti/Fe] ~ +0.35, with only small variations among the RGB, RHB, and BHB stars. Star-to-star variations in proton-capture elements Na, O, and Al are apparent in the spectra. We will present representative abundances from other major element groups in all three stellar evolutionary domains. Acknowledgements: we are grateful to NSF grant AST-0908978, the University of Texas John W. Cox Endowment for Advanced Studies in Astronomy, and the University of Texas Astronomy Department Rex G. Baker, Jr. Endowment for support of this project. 153.14 An Abundance Analysis of Red Giant Stars in the Retrograde Galactic Globular Cluster NGC 3201: Implications for Cluster Formation Scenarios Jennifer A. Simmerer1, I. I. Ivans1 1University of Utah. Exhibit Hall Globular clusters have long been central to the study of Galactic Chemical Evolution. They serve as laboratories for stellar physics, evolution, and nucleosynthesis as well as representing fossil remnants of Galactic assembly processes. Our work addresses two recent areas of interest: globular clusters as accreted objects and globular clusters as hosts for multiple stellar populations. The globular cluster NGC 3201 is a curious object on a retrograde orbit. Some studies suggest that it contains stars of more than one metallicity, a property seen only in the peculiar globular cluster Omega Centauri. Both properties hint at an extra-Galactic origin. We present an elemental abundance pattern for NGC 3201 based on high resolution, high signal-to-noise spectra of red giant stars. We present abundance patterns of similar stars from the globular cluster M5 for comparison. Interpretation of our results is complicated by the discovery that at least two of our giants are variable stars. Though we can derive adequate stellar parameter solutions for both stars in every stage of variability and heavy element abundances do not change with the stellar phase, the abundances of the light elements O, Na, Mg, and Al are extremely unstable and vary greatly. Our inability to correctly model light element line formation in the atmosphere of variable red giant stars has significant implications for studies of star to star abundance variations in exactly these elements in globular clusters, which rely on stars at the same evolutionary stage as the variables in NGC 3201. 153.15 Near Infrared Spectra of SAGE LMC AGB Stars Robert D. Blum1, K. Volk2, S. Srinivasan3 1NOAO, 2STScI, 3IAP, France. Exhibit Hall We present K-band spectra of a sample of Spitzer SAGE LMC sources obtained on the 4-m SOAR telescope in Chile. The near infrared spectral classifications are compared to classifications from Spitzer IRS spectra of the same sources and to the original SAGE IRAC and MIPS photometric classifications. The SOAR Telescope is a joint project of: Conselho Nacional de Pesquisas Cientficas e Tecnolgicas CNPq-Brazil, The University of North Carolina at Chapel Hill, Michigan State University, and NOAO (which is run by the Association of Universities for Research in Astronomy on behalf of the National Science Foundation). 153.16 The O I ?7774 Line as a Luminosity Indicator in M31 Joanna Taylor1, P. Massey1, M. Drout1, S. Tokarz2, N. Caldwell2 1Lowell Observatory, 2Smithsonian Astrophysical Observatory. Exhibit Hall Yellow supergiants are very useful tools in determining the accuracy of current stellar evolutionary models. These stars represent a short phase in a supergiant’s life; typically they will live only thousands of years. Because of this, their positions on the H-R diagram can reveal errors in current models. Identifying stars as yellow supergiants, however, has proved difficult as foreground Milky Way dwarfs can have similar colors and magnitudes. Still, Drout et al. (2009) and Neugent et al. (2010) identified yellow supergiant members from foreground non-members by using stars’ radial velocities. How does one identify yellow supergiants in galaxies without significant rotational velocity, though? In an effort to answer this, we have turned our attention to the O I ?7774 triplet. This line has been known to be a luminosity indicator in F-type supergiants due to Non-Local Thermal Equilibrium (LTE) and sphericity effects (Osmer 1972). We analyzed the spectra of ~900 stars in M31, obtained with the Hectospec multi-fiber spectrometer on the MMT. This sample included 48 rank-1 (nearly certain) M31 members (Drout et al. 2009), looking specifically at the ?7774 line. There was found to be a limit that determines what a ‘significant’ amount of oxygen is, at approximately 1.2 Å. We found that the majority of previously known rank-1’s had a significant amount of oxygen, while ~11% of rank-2’s (probable yellow supergiants) and less than 1% of rank-3’s (foreground dwarfs) had a significant amount. These results imply that the O I ?7774 will indeed work as a luminosity indicator. This work was supported by the National Science Foundation through grants AST-1008020 and AST-1004107. 154 Stellar Atmospheres, Winds Poster Session Exhibit Hall 154.01 Radio And X-ray Emission From Magnetic, Early-type Stars: A Progress Report Stephen Alan Drake1 1USRA/CRESST and NASA/GSFC. Exhibit Hall Radio emission from the classic magnetic early-type stars, the Ap/Bp stars, has been studied since 1985 and its general characteristics and nature seems fairly well understood, e.g., that they can be quite radio-bright and that the dominant emission mechanism is gyrosynchrotron emission. The X-ray emission properties of this stellar class have been harder to pin down, primarily because they are not particularly bright in X-rays, making it difficult to discriminate intrinsic from external emission, e.g., from low-mass coronal companions. With the recent discovery that weaker but still significant magnetic fields are present in many 'normal' early-type stars, it seems timely to re-explore the degree of dependence of the emission in these energy bands on their magnetic fields, as the latter vary over 2-3 orders of magnitude. 154.02 Stellar Spectral Synthesis with OpenGL Nicholas R. Hill1, R. Townsend1 1University of Wisconsin-Madison. Exhibit Hall Given an appropriate model atmosphere, synthesizing the spectrum of a star is a relatively straightforward task -- *if* the star is spherical and homogeneous across its surface. Many astronomically interesting objects do not, however, fall into this category. Examples include single stars that are spotted, rapidly rotating or pulsating, and binary stars in eclipsing or ellipsoidal-variable configurations. To synthesize a spectrum in such cases, it is necessary to construct a 3-D model of the stellar surface; determine which regions of the surface are visible to an external observer; and then calculate the observer-directed radiation from these regions. The Open Graphics Library (OpenGL), a cross-platform application programming interface for creation of 2-D and 3-D graphics, already includes much of the functionality required to implement these steps. We describe a new approach to stellar spectral synthesis that leverages this functionality. A 3-D mesh is constructed to represent the (possibly non-spherical) geometry of the stellar surface (or surfaces, in the case of binary or multiple systems). Textures are laid over this mesh to represent the run of physical attributes such as temperature, gravity, velocity, etc. The textured mesh is then rendered by OpenGL into a framebuffer, a step which naturally takes care of projection and occultation effects. The attributes of each framebuffer pixel are used to look up an appropriate spectrum in pre-calculated tables of specific intensities; and finally, summing the spectra from all pixels gives the disk-integrated synthetic flux spectrum of the star. The advantage of this approach lies in its efficiency (many OpenGL features are hardware-implemented), flexibility and manifest simplicity. Possible applications include binary light-curve modeling, mode identification in pulsating stars, and stellar population synthesis. 154.03 Abundance Results from the Las Campanas Observatory and McDonald Observatory High-Resolution Metal-Poor Star Survey Ian U. Roederer1, G. Preston1, S. Shectman1, I. Thompson1, C. Sneden2 1Carnegie Observatories, 2University of Texas. Exhibit Hall We have undertaken a survey to collect high-resolution and high S/N spectra for more than 300 metal-poor stars. The majority of our sample was selected from the HK Survey of Beers, Preston, and Shectman, and nearly all stars with estimated [Fe/H] < -2.5 have been observed with the MIKE spectrograph on the Magellan-Clay Telescope at Las Campanas Observatory. Additional metal-poor targets were selected based on their kinematic properties and observed with the Tull spectrograph on the Smith Telescope at McDonald Observatory. Previous abundance analyses based on high-resolution and high S/N spectra have been performed for only about 20% of the sample. While this sample naturally allows us to reconfirm and expand upon previously-detected low metallicity abundance trends and identify new stars with unique abundance signatures, its real power is the ability to probe chemical dispersion in abundance ratios. We exploit this attribute by performing line-by-line differential abundance analyses for many elements in large numbers of stars at a single metallicity and evolutionary state. This allows us to assess the evolution of the cosmic scatter of the chemistry of the ISM at very early times in the halo of the Galaxy. Generous funding has been provided by the U.S. National Science Foundation (grant AST 09-08978 to C.S.). 154.04 Asymptotic Giant Branch Stars in the Magellanic Clouds: Dust Production and Mass Return. Martha L. Boyer1, S. Srinivasan2, SAGE-SMC Spitzer Legacy Team 1STScI, 2IAP, France. Exhibit Hall The Small Magellanic Cloud (SMC) was imaged from 3.6 to 160 microns as part of the Legacy program entitled: "Surveying the Agents of Galaxy Evolution in the SMC", or SAGE-SMC. These wavelengths are ideal for studying circumstellar dust, and the full spatial coverage of the SMC (including the bar, wing, and tail) allows for a statistically complete study of its entire dust-producing Asymptotic Giant Branch (AGB) star population. Here, we present the infrared colors and spectral energy distributions of AGB stars, particularly with respect to dust production and mass loss. We also compare the SMC AGB population to those in the higher-metallicity LMC and other metal-poor Local Group dwarf galaxies to assess the influence of metallicity on AGB dust production. This work is supported by Spitzer via JPL contracts 1309827 and 1340964. 154.05 AGB Stars In AKARI And IRAS Two-color Diagrams Kristen Koopman1, L. Sjouwerman2, M. Claussen2 1Sarah Lawrence College and National Radio Astronomy Observatory, 2National Radio Astronomy Observatory. Exhibit Hall Infrared measurements such as from the Infrared Astronomical Satellite (IRAS) all-sky survey and the Midcourse Space Experiment (MSX) Galactic plane survey have been used to statistically distinguish between different types of objects. In particular, two-color diagrams characterize Asymptotic Giant Branch (AGB) stars with different circumstellar shell opacity and thickness, and whether the source is oxygen- or carbon-rich in nature (Van der Veen & Habing 1988, A&A 194, 125; Sjouwerman et al. 2009, ApJ 795, 1554). We present two-color diagrams for AGB stars using infrared data from the AKARI satellite all-sky survey (e.g. Ishihara et al. 2010, A&A 514, A1) and created categories analogous to those for IRAS and MSX two-color diagrams. Our system specifically selects for circumstellar envelopes that are conducive in sustaining SiO maser emission. About 200 new sources were identified in the AKARI data. This research was supported by the Research Experience for Undergraduate Program of the National Science Foundation, and was completed at the National Radio Astronomy Observatory in Socorro, New Mexico. 154.06 ? Vel (K4 Ib-II): Fluorescence on a PAR with Other Luminaries G. M. Wahlgren1, K. G. Carpenter2, T. R. Ayres3, A. Brown3, G. M. Harper4 1CUA/NASA-GSFC, 2NASA-GSFC, 3UCO, 4TCD, Ireland. Exhibit Hall The ultraviolet spectral region of cool, luminous stars contains emission features that originate from fluorescent mechanisms via PAR (photo-excitation by accidental resonance). These mechanisms can account for numerous emission lines, downward transitions from upper energy levels pumped by strong transitions, such as H Ly-?, O I 1302, C II 1335, and Mg II h&k. A new, high S/N observation of the cool giant star ? Vel (K4 Ib-II) was obtained with the HST/COS instrument at a resolving power of R ~ 20000 and covers the wavelength region from 132 nm to 147 nm. High-quality spectra (COS and GHRS) are now available from 128 nm to 147 nm, and at 12 moderate and high resolution observations from the HST/GHRS, the latter covering approximately a third of the wavelength interval from 189 nm to 285 nm. Using these data, together with observations from FUSE and IUE, we investigate PAR processes in the spectra of Cr II and Fe II and make comparisons with other stars. The presence of additional atomic (O I, S I, and Cl I) and molecular (H2, CO) PAR processes in the spectrum of ? Vel is briefly discussed. 154.07 The Chromospheric Structure and Wind of the K-Supergiant Lambda Velorum Kenneth G. Carpenter1, T. R. Ayres2, A. Brown2, G. M. Harper3, G. M. Wahlgren4 1NASA's GSFC, 2University of Colorado, 3Trinity College Dublin, Ireland, 4NASA's GSFC/Catholic Univ. of America. Exhibit Hall Recently, the 1326-1466 Å region of the FUV spectrum of the K4 Ib-II supergiant Lambda Vel was observed with the Cosmic Origins Spectrograph (COS) on HST, as part of the Ayres and Redfield Cycle 17 SNAP program “SNAPing Coronal Iron.” This spectrum covers a region not previously recorded in Lambda Vel at high resolution and, in a mere 20 minutes of exposure, reveals an amazing treasure trove of information. It shows a wide variety of strong atomic and molecular emission lines formed in the chromosphere and multiple atomic absorption lines formed in the stellar wind, both superposed on a bright chromospheric continuum. Further evidence of the stellar wind is seen in the P Cygni profiles presented by the C II (UV 1) lines near 1335 Å. We combine this COS data with archival GHRS spectra of other selected FUV and NUV regions to better characterize the outer atmospheric structure of the star and its massive, outflowing wind. 154.08 Near-Infrared Mass Loss Diagnostics for Massive Stars George Sonneborn1, J. C. Bouret1 1NASA's GSFC. Exhibit Hall Stellar wind mass loss is a key process which modifies surface abundances, luminosities, and other physical properties of hot, massive stars. Furthermore, mass loss has to be understood quantitatively in order to accurately describe and predict massive star evolution. Two urgent problems have been identified that challenge our understanding of line-driven winds, the so-called weak-wind problem and wind clumping. In both cases, mass-loss rates are drastically lower than theoretically expected (up to a factor 100!). Here we study how the expected spectroscopic capabilities of the James Webb Space Telescope (JWST), especially NIRSpec, could be used to significantly improve constraints on wind density structures (clumps) and deep-seated phenomena in stellar winds of massive stars, including OB, Wolf-Rayet and LBV stars. Since the IR continuum of objects with strong winds is formed in the wind, IR lines may sample different depths inside the wind than UV-optical lines and provide new information about the shape of the velocity field and clumping properties. One of the most important applications of IR line diagnostics will be the measurement of mass-loss rates in massive stars with very weak winds by means of the H I Brackett alpha line, which has been identified as one of the most promising diagnostics for this problem. 154.09 OB-wind X-ray/Bolometric Luminosity Proportionality as a Coincidence of the Parameters Kenneth G. Gayley1 1Univ. of Iowa. Exhibit Hall X-ray luminosities of single OB and early-type WN stars show a tendency to scale with the stellar bolometric luminosity. A long-standing question is whether this is essentially a coincidence of the parameters that generate X-ray emission from the generally nonlinear wind strength, or if it is indicative of some X-ray generation process that more directly taps into the bolometric luminosity via some consistent conversion efficiency. Here I explore the former possibility by adopting a novel approach to the general scaling laws for X-ray emission from embedded wind shocks, and find that a coincidental connection between the various nonlinear scalings, resulting in a net response that is broadly proportional to stellar luminosity, is a plausible resolution of this puzzle. This work was supported by a NASA ADP grant. 154.10 Variability in OB Star X-ray Emission Lines: Analysis Techniques Joy S. Nichols1, A. W. Mitschang1, W. Waldron2 1Harvard-Smithsonian, CfA, 2Eureka Scientific, Inc.. Exhibit Hall X-ray emission lines in the spectra of hot stars are expected to vary over short or long periods due to a number of phenomena related to the wind, a companion, or the star itself. Such variations are difficult to quantify due to the comparatively low signal-to-noise in the existing data and the lack of extensive temporal coverage. We utilize several quantitative methods, including a Monte Carlo technique and KS tests, to evaluate emission lines in X-ray spectra for short-term variability based on time-sliced spectra. Our sample of test spectra includes several co-added spectra of multiple observations of a target, as well as four O stars that were serendipitously observed during observations of other targets. We discuss the probability of detecting short-term variations in the He-like emission lines of several hot stars in HETG Chandra data and the need for deeper exposures. 154.11 Long-term Spectroscopic Variability of Luminous Blue Variables Noel Richardson1, D. R. Gies1, N. D. Morrison2 1Georgia State University, 2University of Toledo. Exhibit Hall We report on the preliminary results of a three-year monitoring campaign of southern luminous blue variables with the Cassegrain and Echelle spectrographs at the CTIO 1.5 m telescope. We have collected more than 300 moderate-resolution spectra of 20 stars in the red portion of the optical spectrum, which includes the wind-sensitive transitions of H-alpha and He I 5876 and 6678 Angstroms. We present initial results on the variability of the sample. We find several stars exhibiting observational evidence of changes in the emission line morphology that reflect changes in the wind structure. We also present a detailed study of 15 years of high resolution H-alpha spectroscopy from Ritter Observatory of the prototypical luminous blue variable, P Cygni. We report on the discovery of discrete absorption components in P Cygni's H-alpha profile, and we discuss their relationship to the long-term photometric and emission line variability. 154.12 Tracking Eta Car Through the 2009 Event John C. Martin1, A. Mehner2, K. Davidson2, R. M. Humphreys2, K. Ishibashi3, G. Ferland4 1U of Illinois Springfield, 2U of Minnesota, 3Nagoya University, Japan, 4U of Kentucky. Exhibit Hall Eta Carinae's 2009 spectroscopic event showed significant differences with the two previous well-observed events in 1998.0 and 2003.5. Photometry and spectra gathered with HST and Gemini/GMOS in late 2008 and early 2009 show differences with past events including: 1. a much deeper minimum brightness during the 2009 event and 2. differences in the spatially resolved spectrum during the event that may indicate a significant change in the structure and physical parameters of the wind. Taken together with other data including the early return of X-rays after the event, we believe this represents a critical data point in understanding the nature and continued evolution of Eta Carinae. 155 The Sun Poster Session Exhibit Hall 155.01 Active Region Segmentation Based on Stokes Asymmetries Jieun Choi1, B. Harker-Lundberg2 1UC Berkeley, 2National Solar Observatory. Exhibit Hall During the Stokes inversion process, we would ideally use a distinct model for each structure in an active region which addresses the differences in the physical conditions of these regions. While the Milne-Eddington model of the atmosphere---a frequently-used ideal model that assumes all local thermodynamic equilibrium (LTE) conditions are satisfied---is a sufficient approximation for the description of the solar photosphere, we almost always observe deviations from this model. It is thus of interest to devise a method to systematically and accurately identify the active regions based on their spectra, such that we could use a more sophisticated model catered to each structure in an active region during the actual Stokes inversion process. We present a classification scheme for different active region structures using Stokes asymmetries and line core depths as discriminators. The data used for this investigation were obtained from the Synoptic Optical Long-term Investigations of the Sun (SOLIS) facility using the Vector Spectromagnetograph (VSM), observed in a 3 A bandpass around Fe I 6302.5 A, from March 27, 2008 to March 29, 2008. This work is carried out through the National Solar Observatory Research Experiences for Undergraduate (REU) site program, which is co-funded by the Department of Defense in partnership with the National Science Foundation REU Program. The National Solar Observatory is operated by the Association of Universities for Research in Astronomy, Inc. (AURA) under cooperative agreement with the National Science Foundation. 155.02 Spectroscopic Imaging of the Dynamic Quiet Sun using the Murchison Widefield Array Prototype Interferometer Lynn D. Matthews1, D. Oberoi1, R. Kennedy2, Murchison Widefield Array Team 1MIT Haystack Observatory, 2University of California Berkeley. Exhibit Hall We will present results from recent spectroscopic imaging observations of the solar corona obtained with the Murchison Widefield Array (MWA) Prototype interferometer. The 32-element MWA Prototype operates between 80-300 MHz and is a precursor to the full 512-element MWA that is currently under construction in Western Australia. The combination of high spectral resolution and high dynamic range imaging capabilities afforded by the MWA Prototype are already providing a wealth of new insights into the dynamic nature of the radio Sun. For example, during two separate days in late March 2010 (characterized as "quiet" to "very quiet" by the NOAA Space Weather Prediction Center), we have detected modest level broad-band bursts that are similar to classic Type III bursts in their duration and peak wavelengths. On one of these days, we also detected and imaged numerous short-lived, narrow-band events whose nature is clearly non-thermal, but whose properties, to our knowledge, do not match those of any other previously reported class of radio burst. All of the temporally variable features appear to be linked with x-ray-bright active regions. In some cases, we also observe circularly polarized emission at these locations. Our observations and analysis are ongoing, and we will use these and other new results to illustrate the powerful new capabilities for solar and heliospheric research that will be provided by the full MWA over the next several years. This research was supported by a grant from the National Science Foundation. 155.03 Tracked Motions of G-band Bright Points Olivia Telford1, S. L. Keil2 1University of Pittsburgh, 2National Solar Observatory. Exhibit Hall Abstract Bright points (BPs) are magnetic elements in the photosphere observable in the CN G-band at 4305 Å. High-speed speckle images were taken with the Dunn Solar Telescope in Sunspot, NM with a 80 frame burst every ~32 seconds, achieving a resolution of 0.1422” in the reconstructed images. The BPs were tracked by hand and velocities and curls (vorticity) were derived at each time step. Small-scale motions were also tracked using a FFT local correlation tracking algorithm. The velocities obtained from correlation tracking were generally smaller by factors of 2 to 5 than the hand tracked motion in agreement with previous results, however, the hand-tracked BPs tended to move in the direction of the local correlation tracking velocities. The velocities of the BPs were used to estimate the energy associated with these motions, which was found to vary between 1 to ~3*1017 erg cm-1 based on observed velocities between 2 to 7 km s-1. This amount of energy could provide a source of heat for the corona, which has a minimum energy requirement of 106 erg cm-2 s-1. In some cases, BPs were seen to travel at ~7 km s-1, and changed their direction of motion after collisions with granules. These supersonic speeds could generate shockwaves, which in turn could transfer energy from the BPs to the magnetic field. BPs often spiral around each other, possibly entangling the associated magnetic field providing a mechanism by which energy could be transported to the corona. This research was funded by the National Science Foundation as part of its REU program. 155.04 Effect of Solar Flares on Acoustic Oscillations Within the Sun Kendra Kellogg1, S. Tripathy1, K. Jain1 1National Solar Observatory. Exhibit Hall We investigate the effects that energetic flares have on the acoustic oscillations observed on the surface of the sun. We use the ring-diagram technique, one of the local helio-seismology method, in order to comprehend the role of the flare in exciting the oscillation modes. We analyze these oscillations before, during and after the onset of the flare. The ratio of the mode parameters at different phases of the flare with respect to the pre-flare phase provides us with insight as to how the modes of oscillation are changing with the evolution of the flare. We find that in 32% of the cases studied, the power is absorbed almost completely in the active region. Out of the remaining 68%, a clear enhancement of the power is seen in 23% while a partial enhancement is seen in the other 45%. This work is carried out through the National Solar Observatory Research Experiences for Undergraduate (REU) site program, which is co-funded by the Department of Defense in partnership with the National Science Foundation REU Program. The National Solar Observatory is operated by the Association of Universities for Research in Astronomy, Inc. (AURA) under cooperative agreement with the National Science Foundation. 155.05 Beyond the Limb: A Narrow Band EUV Search for Background Objects with the AIA Sam Schonfeld1, P. Testa2, S. Saar2 1Whitman College, 2Harvard-Smithsonian Center for Astrophysics. Exhibit Hall As the star closest to Earth, the Sun provides us with the opportunity to study up close and test models for X-ray stellar activity. Its close proximity (and consequent brightness), however, makes it challenging to observe the Sun and other celestial objects with the same instrument; thus instrumental cross-calibration difficulties have complicated comparison of the Sun with other stars. The new Solar Dynamics Observatory (SDO) launched in February 2010 may at last allow for direct comparison of the Sun and other stars. The Atmospheric Imaging Assembly (AIA) onboard the SDO, a series of telescopes taking images of the full Sun at high spatial and temporal resolution in seven extreme ultraviolet (EUV) pass bands, can potentially observe background objects passing within the field of view of the telescopes off the limb of the Sun. Young stars, active galactic nuclei and other strong X-ray and EUV emitters may be bright enough to observe after careful background subtraction. Using technical specifications of the telescopes and measured X-ray fluxes of various background sources, we determined that with exposure times of the order of minutes, significantly longer than the standard ~3s exposure, we should be able to observe the brightest background sources when they pass in the AIA field of view. We also determined what kinds of instrumental limitations we need to overcome and how best to make observations of these dim background sources. 155.06 Improved Modeling Of Atmospheric Effects Of The September 1859 Solar Flare. Keith Arkenberg1, B. Thomas1 1Washburn University. Exhibit Hall The atmospheric effects of the 1859 solar flare known as the Carrington event have previously been studied by two different groups. In Thomas et al. 2007, the event was studied with a 2D atmospheric chemistry and dynamics model, using a proton fluence estimate derived from ice core records, and ionization scaled from the 1989 solar proton event. In Rodger et al. 2008, the Carrington event was studied using a 1D model, but with ionization calculated from a likely proton spectrum and time variation, based again on the 1989 event, as well as two other events. In this study we improve upon past work by combining the proton spectrum and time variation used in Rodger et al. 2008 with our 2D atmospheric model. This combination allows for a more accurate estimate of global, long-term atmospheric effects than either approach by itself. Here we report on our computation methods and results, including atmospheric ionization, production of odd nitrogen compounds and subsequent reduction in ozone. Finally, we compare these results to those of past studies. 155.07 The Heliophysics Event Knowledgebase in Action Neal E. Hurlburt1 1Lockheed Martin Corp.. Exhibit Hall The Heliophysics Events Knowledgebase (HEK) system is being developed to help solar and heliospheric researchers locate features and events of interest to their science topics. After 9 months of operations using data from SDO we present an overview of the HEK system In action. 155.08 Using P-mode Oscillations of Infrared CO Lines to Probe the Solar Atmosphere Erin Cox1 1NSO. Exhibit Hall Using the 14 m vertical spectrograph on the NSO McMath-Pierce telescope, CO spectra of the Sun are obtained that are centered around 4.6 µm. From these spectra, Gaussian fits are made to the 46664 Å line to acquire velocity, temperature and continuum parameters. With these parameters, full disk maps are made for each. By creating 3-D maps of velocity and temperature, p-mode oscillations are found by taking a power spectrum of both. Variations in power and central frequency with µ for the velocity map are found by taking power spectra at different annuli of µ. It is seen that power increases as µ increases. The next step is to measure the phase difference and coherence between the velocity and temperature maps, which will be presented. These are also found for different values of µ to better understand how CO changes higher in the solar atmosphere. This work is carried out through the National Solar Observatory Research Experiences for Undergraduate (REU) site program, which is co-funded by the Department of Defense in partnership with the National Science Foundation REU Program. The National Solar Observatory is operated by the Association of Universities for Research in Astronomy, Inc. (AURA) under cooperative agreement with the National Science Foundation. 155.09 Early Results from the Atmospheric Imaging Assembly (AIA) on the Solar Dynamics Observatory (SDO) Theodore D. Tarbell1, AIA Team 1Lockheed Martin Advanced Technology Center. Exhibit Hall SDO was launched on February 11, 2010, and first light was in late March. AIA provides multiple simultaneous high-resolution full-disk images of the corona and transition region up to 0.5 R above the solar limb with 1.5" spatial resolution (0.6" pixels) and 10 second temporal resolution. AIA consists of four telescopes that employ normal incidence multilayer coated optics to provide narrow band imaging of seven EUV band-passes centered on specific lines: Fe XVIII (94 A), Fe VIII, XX, XXIII (131 A), Fe IX (171 A), Fe XII, XXIV (193 A), Fe XIV (211 A), He II (304 A), and Fe XVI (335 A). One telescope observes C IV (1600 A) and the nearby continuum (1700 A), and a filter that observes in the visible enables coalignment with images from other telescopes. The temperature diagnostics of the EUV emissions covers the range from 0.06M °K to 20M °K. Since early April, these images have been taken nearly continuously, usually with a cadence of 12 seconds. Although solar activity has only been increasing slowly in this cycle, there have been a large number of filament ejections that interact with large regions over the solar surface. In addition, because of the rapid cadence of images, a number of new wave phenomena have been discovered associated both with small flares and the interaction of expanding magnetic structures with pre-existing structures. Movies illustrating some of these events will be shown. AIA is supported by NASA (GSFC) contract NNG04EA00C at the Lockheed Martin Advanced Technology Center. 155.10 Analysis of Solar Transition Region Bright Points and Application to Existing Heating Models Norton B. Orange1, H. M. Oluseyi1, D. Chesny1, C. Neira1, L. Preuss1, D. DeBoth1, M. Ebert1, L. Cohen1 1Florida Institute of Technology. Exhibit Hall I have conducted an analysis on the spatial, spectral, and magnetic field data of bright point phenomena that occur in the Sun's upper transition region atmosphere. There are two main aspects to this study: an empirical study of the statistical distribution and properties of upper transition region bright points (UBPs) and a comparison of the measured quantities with theoretical models of their generation and characteristics. I also conducted a comparison of UBPs to other well-studied transition region (TR) phenomena such as blinkers, explosive events, and spicules. Our empirical study of UBPs is made possible through archived SOHO and Hinode data that contain full-disk images of the solar TR and corona with effective temperatures ranging from 0.10 MK to 2.0 MK. We measured surface densities, sizes, radiative outputs, Dopplergrams and magnetic structures of UBPs at 0.25 MK and 0.63 MK in the quiet Sun. The UBPs were modeled as hydrostatic loops to determine of volumetric heating rates. Comparison of the measured and modeled parameters suggest that magnetic reconnection is likely the dominate generation mechanism of UBPs, although MHD waves (or a combination of both) can not be ruled out. 155.11 Empirical Measurements of Loop Structures in the Sun's Transition Region Compared with Energy Balance Models David Chesny1, H. M. Oluseyi1, N. B. Orange1, D. DeBoth1, L. Preuss1, C. Neira1, M. Ebert1, L. Cohen1 1Florida Institute of Technology. Exhibit Hall We have measured the properties of solar upper transition region loop structures barely resolvable in 1-arcsecond resolution data from the Transition Region and Coronal Explorer (TRACE) satellite and from the Solar Ultraviolet Measurements of Emitted Radiation (SUMER) instrument aboard the SOHO satellite for the purpose of investigating the mechanisms that generate and energize these structures. The images were wavelet transformed to elucidate and isolate fine-scale loops, whose lengths, widths, emergent flux, flows, and underlying magnetic field were measured. It was found that the loops' magnetic geometries were well-fit by potential field models. However, hydrostatic models were unable to self-consistently reproduce the loop's observed properties for a wide range of parameter space. 155.12 Magnetic Cycles and Buoyant Magnetic Structures in a Rapidly Rotating Sun Nicholas J. Nelson1, B. P. Brown2, S. Brun3, M. S. Miesch4, J. Toomre1 1University of Colorado-Boulder, 2University of Wisconsin-Madison, 3CEA-Saclay, France, 4High Altitude Observatory - NCAR. Exhibit Hall Observations of sun-like stars rotating faster than our current sun show that they exhibit solar-like magnetic cycles and features, such as star spots. Using global 3-D simulations to study the coupling of large-scale convection, rotation, and magnetism in a younger sun, we have probed the effects of more rapid rotation on stellar dynamos and the nature of magnetic cycles. Our anelastic spherical harmonics (ASH) code allows study of the convective envelope, occupying the outer 30% by radius of a sun-like star. Major MHD simulations carried out at three times the current solar rotation rate reveal magnetic dynamo action that can produce wreaths of strong toroidal magnetic field at low latitudes, often with opposite polarity in the two hemispheres. The presence of the wreaths is quite surprising, for they arise as quite persistent global structures amidst the vigorous and turbulent convection. We have recently explored behavior in systems with considerably lower diffusivities, achieved with a dynamic Smagorinsky treatment of unresolved turbulence. The lower levels of diffusion create magnetic wreaths that undergo prominent variations in field strength, even exhibiting global magnetic cycles that involve polarity reversals. Additionally, during the cycle maximum, when magnetic energies and mean magnetic fields peak, the wreaths possess buoyant magnetic structures that rise coherently through much of the convective envelope via a combination of advection by convective upflows and magnetic buoyancy. We explore aspects of these rising magnetic structures and the evolving global dynamo action which produces them. 156 The Solar System Poster Session Exhibit Hall 156.01 VLBA Astrometry of Cassini Dayton L. Jones1, J. Border1, V. Dhawan2, W. Folkner1, E. Fomalont2, R. Jacobson1, G. Lanyi1, J. Romney2 1JPL/Caltech, 2NRAO. Exhibit Hall We have carried our a series of Very Long Baseline Array (VLBA) astrometric observation of the Cassini spacecraft, which is currently orbiting Saturn, to determine the position of Saturn's center of mass in the International Celestial Reference Frame (ICRF). Our positional accuracies are typically 0.2-0.3 milli-arcseconds, corresponding to about 2 km at the distance of Saturn. The goal of the project is to improve the Saturn ephemeris. This paper reports the results of our first eight epochs of observing, from October 2006 through April 2009. A new planetary ephemeris (DE 422) has been fit to these data, plus two earlier VLBA observations of Cassini by others and a Cassini-based VLBA gravitational deflection experiment by Fomalont et al. in February 2009. Post-fit residuals for DE 422 have a mean offset less than 0.2 mas in both coordinates, but not all of our phase reference sources have ICRF position with this accuracy yet. Future observations will improve reference source positions, and will continue to follow Saturn through more than 1/4 of its orbital period. (The Cassini mission is currently funded to operate until 2017.) We are grateful to Larry Teitelbaum for support of this project through the Advanced Tracking and Observational Techniques of JPL's Interplanetary Network Directorate, and to John Benson and the VLBA operations team at NRAO for their excellent support of these observations. The VLBA is a facility of the National Radio Astronomy Observatory, which is operated by Associated Universities, Inc., under a cooperative agreement with the National Science Foundation. Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. 156.02 Quantifying Uncertainties in the Evolution of the Solar Flux John Sheets1, M. Claire1, I. Ribas2 1University of Washington, 2Institut de Ci`encies de l’Espai, Spain. Exhibit Hall Understanding changes in the solar flux over geologic timescales is essential to studies of planetary atmospheres and how planets evolve in general. To this end, we have developed quantitative estimates of the wavelength-dependent solar flux over time. Using multi-wavelength data from the Sun and solar analogs we present a parametrization of the solar flux which is nominally valid from 2-20000 nm, and from ~0.02 through 7.1 Gyr. The parameterization is subject to large uncertainties inherent in primary measurement error, the unknown ages of the solar proxies, and the intrinsic variability of the solar analogs. This poster details our procedures in quantifying the effect of these uncertainties on our estimates of the evolving solar flux. From the X-ray to the near UV, we derived thousands of different power law fits to the observational data via a Monte Carlo simulation. During each iteration of the simulation, an age for each solar analog was selected randomly from age ranges found in the literature. These ages are fit against the observational data, which are themselves randomized by their measurement errors and assumed intrinsic variability. This produces multiple power laws fits for flux versus time in various wavelength regimes and strong lines, which we compare against fits assuming exact ages and flux values. We find the integrated mean error (standard deviation / mean) of our Monte Carlo simulations to never be in excess of 100%, with significant decreases in error at older stellar ages. The mean absolute error on any flux value from any wavelength is never above 50%. We therefore submit our model of the solar flux as viable for planetary atmosphere studies which are concerned with the first order evolution of the Sun in time. 156.03 Analysis Of Spitzer IRS 5.6 To 7.7 ?m Observations Of Comets 6P/d'Arrest And C/2007 N3 (Lulin) David Emerson Harker1, C. E. Woodward2, M. S. Kelley3, D. Bockelee-Morvan4, J. Crovisier4, D. H. Wooden5 1UC, San Diego/CASS, 2Univ. of Minnesota, 3Univ. of Maryland, 4LEISA, Observatoire de Paris, France, 5NASA Ames. Exhibit Hall The production rate of volatiles from comet nuclei through sublimation of ices is a measure of the activity and volatile abundance. Sublimation of water, the dominant ice in cometary bodies, is the main source of activity at heliocentric distances rh < 3 AU from the Sun. The water production rate (Q(H2O)), the rotational temperature (Trot) and the ortho-to-para ratio (OPR) are of particular interest in the study of cometary atmospheres and cometary physics, and cometary origins. We present Spitzer IRS 5.6 to 7.7 ?m spectra of comets 6P/d'Arrest (6P) obtained 2008 Sept 12 UT (post-perihelion; rh = 1.39 AU), and C/2007 N3 (Lulin) obtained 2008 Oct 04 UT, (pre-perihelion; rh = 1.90 AU). The 6.3 ?m ?2 vibrational band is detected in both comets. Both comets also show an as yet unidentified broad feature at ?7.2 ?m that appears in other IRS observations of comets. Fluorescence models of water emission are used to calculate Q(H2O), Trot, and OPR towards the nucleus of both comets and into the coma ?9" and ?18" away from the nucleus to assess the coma spatial distribution of Trot, and the OPR. Limits are placed on emission from controversial cometary constituents, carbonates and PAHs. Support for this work is provided in part by NASA through contract 1355318. 156.04 Modeling the Interior Structure of Tempel 1 Victoria Hartwick1, G. Sarid2 1University of Wisconsin - Madison, 2Institute for Astronomy. Exhibit Hall Processes that determine the correlation between nuclear activity and coma structure in comets are largely unknown. Since ground based observations of comet nuclei are impossible, complex models present the best current method for interpreting coma changes during orbit, with the exception of in situ observations. Using data collected from the Deep Impact mission in 2005 and ground based observations from 1983 to 2005, we present a preliminary model of the interior activity of Tempel 1. Matching of output production rates to observed production rates provides information about the model’s accuracy. 156.05 Efficient Prediction of Asteroid Positions from Solar System Models Yusra AlSayyad1, S. Krughoff1, A. J. Connolly1, L. Jones1, T. Budavari2, B. Howe1 1University of Washington, 2Johns Hopkins University. Exhibit Hall When simulating the distribution of sources across the night sky, querying for stationary objects, such as galaxies, is relatively simple. For moving objects, such as near earth objects (NEOs) and main belt asteroids (MBAs), this becomes increasing more complex. Each family of solar system objects has a range of abundances and speeds through ra/dec space. For example, MBAs are plentiful (~107) but move slowly (< 1 deg/day), and NEOs are rare (~105) but can move up to 70 deg/day. How do we optimally store and query all families of moving objects? We describe performance results and experiences using different methods, such as storing bounding boxes for the trajectories, and spatial abstraction tools, such as MSSQL geospatial support and SkyServer’s HTM index and library of spatial constructs. We apply these results to simulations of the data flow from the Large Synoptic Survey Telescope with the goal of querying simulated catalogs quickly for a list of objects that would appear in the LSST’s circular aperture at a given pointing and epoch. 156.06 Asteroid Astrometry Accuracy Hugh C. Harris1, M. A. Murison1 1U.S. Naval Obs.. Exhibit Hall Predictions of asteroid (or comet) positions depend on the accuracy of their orbits, and in turn on the history and quality of their measured postitions as they move around the sky. Currently the error of a single observation is limited by catalog errors of ~50 mas, even with the best available catalogs such as Tycho or UCAC. We discuss errors in catalogs, asteroid orbits, and predicted positions for bright asteroids (V < 17), including the 6000 asteroids being monitored by the Flagstaff Astrometric Scanning Transit Telescope. For purposes of predicting occultations, it is desirable to improve asteroid orbits and the positions of the occulted stars. We discuss an experiment to greatly reduce the error of their relative positions, and improve the predicted occultation path. This work received funding from NASA NNH08AI17I. 156.07 The Impact Of The Lcross Satellite With The Moon As Seen By The Hubble Space Telescope Alex Storrs1, L. Guillou1, A. O'Hara1 1Towson Univ.. Exhibit Hall We present Hubble Space Telescope (HST) images and NUV spectra of the near lunar region at the time of the impact of the LCROSS experiment (Colaprete 2007) into a permanently shadowed crater on the lunar south pole. Images immediately before and after the impact show an enhancement in the scattered light near 300 nm within a minute of the event. Spectra show persistent emission of the OH (1-0) band at 283 nm, which may indicate a permanent lunar exosphere of OH as reported by Sridharan et al (2010), rather than OH produced by photolysis of water liberated by the impact event. Analysis of the data is limited by uncertainty in the HST pointing, as the observations were made under gyro control. References: A. Colaprete, G. Briggs, K. Ennico, D. Wooden, J. Heldmann, L. Sollitt, E. Asphaug, D. Korycansky, P. Schultz, A. Christensen, K. Galal, and the LCROSS Team (2007): “An Overview of The Lunar Crater Observation and Sensing Satellite (LCROSS) Mission - An ESMD Mission to Investigate Lunar Polar Hydrogen”, LEAG Workshop on Enabling Exploration: The Lunar Outpost and Beyond, held October 1-5, 2007 in Houston, Texas. LPI Contribution No. 1371, p.3017 R. Sridharan, S.M. Ahmed, Tirtha Pratim Das, P. Sreelatha, P. Pradeepkumar, Neha Naik and Gogulapati Supriya (2010): “‘Direct’ evidence for water (H2O) in the sunlit lunar ambience from CHACE on MIP of Chandrayaan I”, Planetary and Space Science Volume 58, Issue 6, May 2010, Pages 947-950 156.08 Jupiter In The Crosshairs: Recent Impacts And Their Implications Heidi B. Hammel1, I. de Pater2, A. A. Simon-Miller3, L. Fletcher4, M. B. Boslough5, G. S. Orton6, G. Djorgovski7, P. Yanamandra-Fisher6, M. H. Wong2, R. Hueso8, A. Sánchez-Lavega8, C. Go9, A. Wesley10, S. Pérez-Hoyos8, M. Edwards11, J. T. Clarke12, K. S. Noll13 1Space Science Institute, 2UC Berkeley, 3NASA's GSFC, 4Oxford, United Kingdom, 5Sandia, 6JPL, 7Caltech, 8Univ. del Pais Vasco, Spain, 9U. San Carlos, Philippines, 10Acquerra Pty. Ltd., Australia, 11Gemini, Chile, 12Boston U., 13STScI. Exhibit Hall 156.09 Effective Mitigation of a Potentially Hazadous Objtect by a Subsurface Explosion Robert Weaver1, C. Plesko1, W. Dearholdt1 1LANL. Exhibit Hall Disruption or mitigation of a potentially hazardous object (PHO) by a high-energy subsurface burst is considered. This is just one possible method of impact-hazard mitigation. We present xRAGE hydrocode models of the shock-generated disruption of PHOs by subsurface nuclear bursts using scenario-specific models from realistic RADAR shape models. We will show 2D and 3D models for the disruption by a large energy source at the center of such PHO models (~100 kton - 10 Mton) specifically for the shape of the Itokawa asteroid. We study the effects of non-uniform compistion (rubble pile), effective source energy, and the optimal depth of burial from the surface explosion to the central explosion. 156.10 Investigating the Dynamical History of the Solar System Schuyler Wolff1, R. Murray-Clay2, R. Dawson3 1Western Kentucky University, 2Smithsonian Astrophysical Observatory, 3Harvard University. Exhibit Hall The current dynamical structure of the Kuiper belt was shaped by the evolution of giant planet orbits during the era of planet formation. Numerical models of this process, while reproducing many properties of the belt, have difficulty generating the high inclinations and eccentricities observed for some objects while maintaining a low eccentricity and low inclination "cold classical" population. We present a parameter study of the effect of different dynamical histories on orbits in the Kuiper belt using N-body simulations. In particular, we probe which combinations of migration, eccentricity damping, and inclination damping of Neptune over the history of the solar system allow the cold classical population to survive. This work is supported in part by the NSF REU and DOD ASSURE programs under NSF grant no. 0754568 and by the Smithsonian Institution. 156.11 Rotation Rates of 8 Main Belt Asteroids Dicy Ann E. Saylor1, M. A. leake2 1University of Georgia, 2Valdosta State University. Exhibit Hall We report the rotation rates of the 8 main-belt asteroids 205 Martha, 252 Clementina, 506 Marion, 567 Eleutheria, 613 Ginevra, 869 Mellena, 996 Hilaritas, and 1490 Limpopo and discuss future work. These bodies include one P and seven C-class asteroids located at heliocentric distances of 2.3 to 3.6 AU. Seven of the light curves produced useful results; three of the periods are reported here for the first time, one expands on a previous publication, and the remaining three periods support previously published results. The study of main belt asteroids is an important topic because they can give us insight into planet formation and evolution. The focus of this paper is to use photometry to learn rotation periods. Future work will focus on using this information to obtain shape and pole orientation. Knowing the rotation rate, shape and orientation and their dynamics can place constraints on the early solar system. This project was funded by the National Science Foundation Research Experiences for Undergraduates (REU) program through grant NSF AST-1004872. 156.12 Physical Characterization of the Binary Asteroid 66146 (1998 Tu3) Thien-Tin Truong1, M. Hicks2, D. Mayes2, T. Barajas3, K. Garcia1 1California State University - LA, 2Jet Propulsion Laboratory California Institute of Technology, 3Los Angeles City College. Exhibit Hall The near-Earth asteroid 66146 (1998 TU3) was discovered on 1998 October 13 by the LINEAR NEO survey (MPEC 1998-U03). We obtained five nights of Bessel BVRI observations (2010 Aug 6,7,10,12,13 UT) and one night of Bessel R (August 8 PST) at the JPL Table Mountain Observatory (TMO) 0.6-m telescope near Wrightwood, California. These observations were obtained as part of our ongoing survey at TMO of Potentially Hazardous Asteroids (PHAs), planetary radar targets, and low delta-V near-Earth asteroids (NEOs). The object's rotationally averaged colors (B-R=1.238+/-0.011 mag; V-R=0.440+/-0.008 mag; R-I=0.275+/-0.010 mag) were found most compatible with an Sk-type spectral classification (Bus Taxonomy)/S-type (Tholen Taxonomy). This association was obtained through a comparison of our colors with the 1341 asteroid spectra in the SMASS II database (Bus & Binzel 2002). Our classification differs significantly from the Q-type taxonomy reported by Whitely (2002). Assuming a solar phase parameter g=0.15 we performed a period search using standard Fourier techniques. We found a best-fit rotational period Psyn=2.378+/-0.001 hr, in excellent agreement with the 2.3779+/-0.0004 period determined by Richards et al. (2007). The dispersion in the phased single period lightcurve strongly suggests that 1998 TU3 is be a binary system, with variations in observed flux caused by an unresolved, tidally locked secondary companion. Fitting a 2-period model as described by Pravec et al. (2000), we found that our photometry agrees well with a binary model (P1=2.378+/-0.01 hr, P2=28.28+/-0.05 hr). We have three additional nights scheduled for this object at TMO (Oct 8, 9, 10 2010 UT), extending our solar phase coverage and allowing us to refine our rotational models. 1998 TU3 will experience an exceptional apparition in 2012. This object may be a good candidate for shape/pole modeling via lightcurve inversion, especially if photometry can be obtained from both northern and southern hemispheres. We welcome any potential collaborations. 157 Instrumentation: Ground Based or Airborne Poster Session Exhibit Hall 157.01 Monitoring High Energy Transients With Crro Tiffany Watkins1, D. Macomb1, J. Norris2 1Boise State University, 2University of Denver. Exhibit Hall We describe the capabilities and early results from a newly developed optical observatory, the Challis Rapid Reaction Observatory (CRRO). Our initial nightly observing program concentrates on blazars, accreting binaries and gamma-ray bursts. The CRRO is located in central Idaho at 2165 m (7100 feet) elevation, in a mountain desert micro-climate that enjoys the driest (~ 5” yearly precipitation) and clearest nights in the State. It is completely remotely operable, with all necessary capabilities for automated operation in response to GRB alerts. This facility adds materially to the U.S. geographic coverage for GRB afterglows, being the only automated, remotely operable facility in the northwest part of the country. 157.02 EVLA Commissioning: Status and Prospects Michael P. Rupen1, EVLA Scientific Commissioning Team 1NRAO. Exhibit Hall We report progress in commissioning the Expanded Very Large Array (EVLA), a project to improve the key observational capabilities of the VLA (point source sensitivity, instantaneous bandwidth, frequency resolution, and flexibility) by roughly an order of magnitude, while extending the suite of receivers to allow tuning the array anywhere between 1 and 50 GHz. The first scientific data were taken on March 2, 2010, and commissioning and scientific operations continue at a rapid pace. Here we report on the status of the upgrades and present some recent observational results. We also review the schedule through the end of the construction/commissioning period with special emphasis on the scientific capabilities we expect to offer the community. Full operations are scheduled to begin at the end of 2012. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. 157.03 Michi: A MIR Instrument Concept for the TMT Christopher C. Packham1, Y. K. Okamoto2, A. Tokunaga3, J. Carr4, M. Chiba5, M. Chun3, K. Enya6, H. Fujiwara6, T. Fujiyoshi7, M. Honda8, M. Imanishi7, Y. Ita5, H. Kataza9, T. Kotani9, H. Izumiura10, N. A. Levenson11, T. Matsuo12, M. Matsuura13, T. Minezaki14, J. Najita15, T. Onaka14, T. Ootsubo5, M. Richter16, I. Sakon14, M. Takami17, C. M. Telesco1, C. Warner1, C. M. Wright18, T. Yamashita12 1Univ. of Florida, 2Univ. of Ibaraki, Japan, 3Univ. of Hawaii, 4NRL, 5Univ. of Tohoku, Japan, 6ISAS, Japan, 7Subaru Observatory, 8Univ. of Kanagawa, Japan, 9ISAS/JAXA, Japan, 10NOAJ, Japan, 11Gemini Observatory, Chile, 12NAOJ, Japan, 13UCL, United Kingdom, 14Univ. of Tokyo, Japan, 15NOAO, 16UC Davis, 17ASIAA, Japan, 18UNSW, Australia. Exhibit Hall A mid-infrared (MIR) imager and spectrometer is under consideration for construction in the first decade of the Thirty Meter Telescope’s (TMT) operation. When combined with a MIR adaptive optics system, the instrument will afford 15 times higher sensitivity, 4 times better spatial resolution (0.08”) than 8m-class telescopes, and ~4.5 times better spatial resolution than the JWST. Additionally, its huge light gathering power opens a new window of high-dispersion spectroscopy in the MIR. We discuss the key science drivers, from star and planet formation to galaxies and black holes and cosmology; science drivers which are in close synergy with the recent Astro 2010 Decadal Survey report. We flow down our science cases to produce fundamental and optional instrument capabilities, including imaging, long-slit and IFU spectroscopy, and polarimetry. 157.04 Early Science Planning of Protoplanetary Disks and Protostars in the Orion Nebula Cluster Using SOFIA/FORCAST Keri Hoadley1, J. D. Adams2, T. L. Herter2, G. Gull2, C. Henderson2, J. Schoenwald2, L. Keller3, T. S. Megeath4 1Florida Institute of Technology, 2Cornell University, 3Ithaca College, 4University of Toledo. Exhibit Hall The Faint Object Camera for the SOFIA Telescope (FORCAST) is a mid-infrared facility instrument for the Stratospheric Observatory For Infrared Astronomy (SOFIA). In late May of this year, FORCAST achieved first light on SOFIA during a Telescope Assembly characterization flight, successfully taking photometry of Jupiter, its moons, and M82 from an altitude of 35,000 ft. Analysis of images of Jupiter and one of its moons, Ganymede, show the in-flight sensitivity to be comparable to that expected from preflight (lab) measurements and models. In preparation for SOFIA Short Science, we constructed Spectral Energy Distributions (SEDs) for known proplyds and protostars (Smith et al. 2005) in the core of the Orion molecular cloud using 2MASS (Skrutskie et al. 2006), IRAC on Spitzer, TReCS on Gemini South (Smith et al. 2005), and 880mm SCUBA data (Mann and Williams 2009). FORCAST will provide important wavelength coverage (20 - 40 microns) which when used in conjunction with previous data will constrain the physical properties of the proplyds and protostars. We fit the observed SEDs with those from radiative transfer models for circumstellar disks and protostars from Robitaille et al (2006, 2007). With these models, we can extrapolate into the 20 - 40 micron region of FORCAST and determine the range of models that FORCAST is capable of detecting. Using the FORCAST sensitivity model and the SEDs of known proplyds, we expect to detect 67% of the proplyds found by other investigations. However, detectability will be greatly influenced by the presence of structures in the diffuse dust emission associated with the HII region complex. Comparing FORCAST observations with the radiative transfer models will help to understand the physical properties of proplyds and protostars, and perhaps illuminate the impact of their environments, such as photoevaporation of disks and effects from crowding. 157.05 Simultaneous Lidar and All-Sky IR Camera Observations to Measure Cloud Transmission Peter C. Zimmer1, J. Sebag2, J. T. McGraw1, D. C. Zirzow1, D. V. Vorobiev1, UNM Measurement Astrophysics (MAP) Research Group 1Univ. of New Mexico, 2NOAO. Exhibit Hall We present initial results of combined lidar and all-sky thermal infrared camera measurements of transmission losses through clouds. Thermal IR observations in the 10 micron window have long been used at observatories to detect the presence of clouds by measuring the contrast in downwelling thermal radiation between clear and cloudy sky. The ability of these techniques to measure thin cirrus at high altitudes, the sort of clouds that typically ruin otherwise photometric conditions, has always been limited due to their low temperature and low emissivity. Lidar, on the other hand, is quite effective at measuring both the presence and optical depth of thin cirrus clouds, well below 1% transmission losses. A lidar can only operate in one direction at a time and thus is limited in its ability to measure transmission over wide fields of view. The combination of wide field thermal IR imaging plus lidar measurements of transmission hold significant promise for helping solve the time and field dependence of atmospheric transmission caused by clouds, especially sub-visual cirrus. To test this instrumental combination, the LSST all-sky infrared camera was deployed for several weeks at the UNM Campus Observatory in Albuquerque, NM, the location of the Astronomical Lidar for Extinction (ALE). The two instruments were operated together under various cloud cover conditions and when conditions permitted, narrowband photometry of bright stars was simultaneously obtained to verify the temporal and spatial variation of extinction. MAP atmospheric transmission research is supported by NIST Award 60NANB9D9121 and NSF Grant AST-1009878. 157.06 Generic Misalignment Aberration Patterns in Wide-Field Telescopes Rebecca Sobel1, P. L. Schechter1 1MIT. Exhibit Hall Aligned telescopes either produce third-order Seidel aberrations or are specifically designed to balance them out. These Seidel aberrations manifest in the field as patterns of point spread functions. When optics are misaligned, breaking the axial symmetry of the telescope, another set of generic third-order aberration patterns arise, one each for coma, astigmatism, and curvature of field, and two for distortion. Each misalignment pattern is characterized by a two dimensional vector, which is in turn a linear combination of the mirror tilts and decenters. For an N-mirror telescope, 2(N-1) patterns must be measured to keep the telescope aligned. Common practice for two mirror telescopes is to use misalignment coma and astigmatism patterns to align the secondary mirror. However, for three mirror telescopes, it will be necessary to either measure the curvature of field and one of the distortion patterns, or alternately to measure smaller fifth order misalignment patterns in order to maintain alignment. This work was supported by the National Science Foundation through a Graduate Research Fellowship. 157.07 The Infrared Camera for RATIR, a Rapid Response GRB Followup Instrument David A. Rapchun1, W. Alardin2, B. C. Bigelow3, J. Bloom4, N. Butler4, A. Farah2, O. D. Fox5, N. Gehrels6, J. Gonzalez2, C. Klein4, A. S. Kutyrev7, G. Lotkin1, C. Morisset2, S. H. Moseley6, M. Richer2, F. D. Robinson8, M. V. Samuel6, L. M. Sparr6, C. Tucker1, A. Watson2 1NASA/GSFC/GST, 2University of Mexico, Mexico, 3University of California, Santa Cruz, 4University of California, Berkeley, 5NASA/GSFC/ORAU, 6NASA GSFC, 7NASA/GSFC/CRESST, 8NASA/GSFC/Orbital. Exhibit Hall RATIR (Reionization and Transients Infrared instrument) will be a hybrid optical/near IR imager that will utilize the "J-band dropout" to rapidly identify very high redshift (VHR) gamma-ray bursts (GRBs) from a sample of all observable Swift bursts. Our group at GSFC is developing the instrument in collaboration with UC Berkeley (UCB) and University of Mexico (UNAM). RATIR has both a visible and IR camera, which give it access to 8 bands spanning visible and IR wavelengths. The instrument implements a combination of filters and dichroics to provide the capability of performing photometry in 4 bands simultaneously. The GSFC group leads the design and construction of the instrument's IR camera, equipped with two HgCdTe 2k x 2k Teledyne detectors. The cryostat housing these detectors is cooled by a mechanical cryo-compressor, which allows uninterrupted operation on the telescope. The host 1.5-m telescope, located at the UNAM San Pedro Martir Observatory, Mexico, has recently undergone robotization, allowing for fully automated, continuous operation. After commissioning in the spring of 2011, RATIR will dedicate its time to obtaining prompt follow-up observations of GRBs and identifying VHR GRBs, thereby providing a valuable tool for studying the epoch of reionization. 157.08 The Balloon Experimental Twin Telescope for Infrared Interferometry (BETTII): High Angular Resolution in the Far-Infrared Stephen Rinehart1 1NASA's GSFC. Exhibit Hall Astronomical studies at infrared wavelengths have dramatically improved our understanding of the universe, and observations with Spitzer, Herschel, and SOFIA will continue to provide exciting new discoveries. The relatively low angular resolution of these missions, however, is insufficient to resolve the physical scale on which mid-to far-infrared emission arises, resulting in source and structure ambiguities that limit our ability to answer key science questions. Interferometry enables high angular resolution at these wavelengths - a powerful tool for scientific discovery. We are building the Balloon Experimental Twin Telescope for Infrared Interferometry (BETTII), an eight-meter baseline Michelson stellar interferometer to fly on a high-altitude balloon. BETTII's spectral-spatial capability, provided by an instrument using double-Fourier techniques, will address key questions about the nature of disks in young star clusters and active galactic nuclei and the envelopes of evolved stars. BETTII will also lay the technological groundwork for future balloon programs, paving the way for interferometric observations of exoplanets. 157.09 The Magdalena Ridge Interferometer: Telescope Delivery to Laboratory Fringe Measurements Colby Jurgenson1, F. Santoro1, A. Olivares1, R. Selina1, I. Payne1, M. Creech-Eakman1, D. Buscher2, C. Haniff2, J. Young2 1NMT/MRO, 2University of Cambridge, United Kingdom. Exhibit Hall This report focuses on recent developments at the Magdalena Ridge Observatory Interferometer (MROI) in three major areas: 1) telescope delivery and array infrastructure construction, 2) installation of the first vacuum delay line and 3) laboratory fringe measurements with the first fringe beam combiner. Construction of the telescope foundations and utilities began in August of 2010 and will be complete in September of 2011 for delivery of the first of ten telescopes. The MROI now has the longest (100m) evacuated fast delay line in the world. Initial performance tests that began in November of 2010 are reported here. First broadband fringe measurements have been recorded in the laboratory with the fringe tracking beam combiner. These measurements demonstrate high optical quality, and visibilities matching the predicted values for its architecture type. 157.10 The Willard L. Eccles Observatory: Preliminary Characterization of the Site for Optical Astronomy Nic Ramsrud1, K. Dawson1, D. Della Corte1, P. Gondolo1, P. Ricketts1, U. Samarasingha1, W. Springer1 1University of Utah. Exhibit Hall The University of Utah Department of physics and Astronomy recently completed construction of the Willard L. Eccles Observatory, a new facility on the edge of the Great Basin desert in western Utah. Located between Las Vegas and Salt Lake City, the site was chosen after careful consideration of climate, light pollution, seeing quality, and available infrastructure. The observatory is located on a prominent peak at an altitude of 9551 feet and houses a 0.8 meter optical telescope from DFM Engineering. The first images taken with the telescope have produced sub-arcsecond seeing and minimal sky background as would be expected for this remote site. We will present a description of the observatory and a preliminary characterization of the site. The construction of this observatory was made possible by the generous support of the Willard L. Eccles Foundation and the Katherine W. and Ezekiel R. Dumke, Jr. Foundation. 157.11 Robo-AO: The First Autonomous Laser Guide Star Adaptive Optics System for Small Telescopes Reed L. Riddle1, C. Baranec1, A. N. Ramaprakash2, N. Law3, S. Tendulkar1, S. Kulkarni1, K. Bui1, M. Burse2, P. Chordia2, H. Das2, R. Dekany1, M. Kasliwal1, E. Ofek1, J. Zolkower1 1California Institute of Technology, 2Inter-University Centre for Astronomy and Astrophysics, India, 3University of Toronto, Canada. Exhibit Hall Robo-AO will be the first fully autonomous laser guide star adaptive optics and science system. Specifically designed to take advantage of small (1 to 3 meter) telescopes, Robo-AO will deliver high angular resolution science in the visible and near infrared for up to hundreds of targets per night. This will enable the exploration of science programs not practical for larger aperture adaptive optics systems. This presentation discusses the current status of the Robo-AO project, including the laboratory testbed, laser guide star facility and plans for a demonstration of the fully autonomous system next year. 157.12 Zodiac: A Balloon Facility for Exoplanet Debris Disk Observations Stephen C. Unwin1, W. Traub1, G. Bryden1 1JPL. Exhibit Hall Zodiac is a telescope-coronagraph system, operating at visible wavelengths, mounted on a balloon-borne gondola in the stratosphere. The science objective is to image debris disks around nearby stars. Debris disks, usually found in the outer reaches of a planetary system, are significant for exoplanet science because (a) they tell us that planet formation did actually get started around a star, (b) they are a contributing source of potentially obscuring dust to the inner part of the disk where we will someday start searching for terrestrial planets, and (c) for a disk with an inner edge, this feature is a signpost for a shepherding planet and thus a sign that planet formation did indeed proceed to completion around that star. The telescope has a 1-m diameter, clear-aperture primary mirror, designed to operate in the cold stratospheric environment. The coronagraph is designed to suppress starlight, including its diffracted and scattered components, and allow a faint surrounding debris disk to be imaged. We will control the speckle background to be about 7 orders of magnitude fainter than the star, with detection sensitivity about one more order of magnitude fainter, in order to comfortably image the expected brightness of typical debris disks. Zodiac will be designed to make scientifically useful measurements on a conventional overnight balloon flight, but would also be fully compatible with future Ultra Long Duration Balloon flights. Zodiac has a technical objective of advancing the technology levels of future mission components from the lab to near-space flight status. These components include deformable mirrors, wavefront sensors, coronagraph masks, lightweight mirrors, precision pointing, and speckle rejection by wavefront control. The research described in this talk was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Government sponsorship acknowledged. 157.13 A Summary of the First Year of Observations from the West Mountain Observatory 0.9-meter Telescope Michael D. Joner1, E. G. Hintz1, C. D. Laney1, J. W. Moody1 1Brigham Young Univ.. Exhibit Hall We present a summary of selected projects that have made use of the new 0.9-meter telescope located at the Brigham Young University West Mountain Observatory during its first year of operation. Projects are limited to direct imaging but include a wide variety of subjects. Targets include intrinsic variable stars, standard star photometry, narrow band imaging studies, and long term monitoring of various objects such as high mass X-ray binaries, active galactic nuclei, pre-main sequence objects, and Cepheid variable stars. The use of filters with excellent transmission characteristics, along with a high quantum efficiency CCD, has greatly extended the effective limiting magnitude for this system. The 0.9-meter telescope was made possible through a grant from the National Science Foundation PREST program (AST-0618209). We also acknowledge continued support from the Brigham Young University Department of Physics and Astronomy for continued operational funding and research support at the West Mountain Observatory. 157.14 Progress to First Light for AMASING, an Aperture Masking Instrument Luke M. Schmidt1, F. G. Santoro2, C. A. Jurgenson2 1New Mexico Tech, 2Magdalena Ridge Observatory, New Mexico Tech. Exhibit Hall We report on construction progress for the AMASING (Aperture Masking And Speckle ImagiNG) instrument. AMASING is designed for aperture masking and speckle interferometry at optical wavelengths. This report will focus on three main aspects of the instrument construction. The optical and electronic components have been selected and are assembled in a laboratory. We describe the optical alignment procedures and expected visibility performance across the design wavelengths as well as a discussion on the types of aperture masks developed for the instrument. The support structure and enclosure have been designed to provide a stable platform for the instrument optics. We document the construction, predicted performance and the procedure for aligning the structure with the optical axis of the telescope. Finally we discuss the instrument software control architecture and interface with the telescope. This work has been supported by LANL-NMT MOU UCDRD funding, a College Cost Reduction and Access Act grant to Amarillo College, the New Mexico Space Grant Consortium and the New Mexico Tech Graduate Student Association Matuszeski Research Grant. 157.15 NIST-traceable SI Calibration of Standard Stars John T. McGraw1, P. C. Zimmer1, D. C. Hines2, J. T. Woodward3, C. E. Cramer3, K. R. Lykke3, S. W. Brown3, A. W. Smith3, G. T. Fraser3, C. W. Stubbs4, A. B. Hull1, D. C. Zirzow1, D. V. Vorobiev1, Measurement Astrophysics Research Team 1Univ. of New Mexico, 2Space Telescope Science Institute, 3NIST, 4Harvard University. Exhibit Hall We describe optical spectrophotometric observing techniques for bright stars, and two independent procedures for calibrating these observations to NIST-calibrated detectors, resulting in absolute spectral energy distributions in SI irradiance units of W/m2/nm. Stars, thermal point sources with physically well understood structures and atmospheres, radiate from the ultraviolet to the infrared and thus provide excellent radiometric standards against which to compare and calibrate ground- and space-based astronomical observations. We have evolved techniques for ground-based standardization of the spectral energy distributions of stars from 350 nm to 1050 nm for an initial set of standard stars with V < 5.5. With adequate photometric and spectrophotometric vetting, stable standard star candidates can be identified. The Measurement Astrophysics (MAP) standardization technique uses a unique objective spectrometer supported by an atmospheric extinction-sensing lidar for the stellar observations. The spectrometer is calibrated using two separate NIST detector-based standardization techniques. The first is implemented by observing a far-field, point-like NIST spectrophotometrically monitored source approximately one kilometer distant, and the second uses a near-field collimated source illuminated wavelength-by-wavelength using a monochrometer. We describe in detail the calibration procedures and analyze the utility of calibrating astronomical standard stars using two independent procedures. MAP standard star research is supported by NIST Award 60NANB9D9121 and NSF Grant AST-1009878. 157.16 Deriving Telescope Properties Using Daytime Sky Observations Shannon Hall1, D. Harrington2 1Whitman College, 2University of Hawaii. Exhibit Hall High-resolution spectropolarimetry in night-time astronomy is a relatively new but powerful remote sensing technique. In order to make accurate spectropolarimetric measurements using large telescopes it is necessary to derive the calibration of the telescope by recovering the Mueller matrix elements. These calibrations are typically difficult to recover and are functions of wavelength and telescope pointing. We demonstrate a novel technique using observations of the bright, highly polarized, and easily accessible daytime sky. With the calibration of the AEOS 3.67m telescope on Haleakala and the new low-resolution spectropolarimeter LoVIS we illustrate the spectropolarimetric accuracy with observations of AB Aurigae. 157.17 Evolving Technology for Fabricating 1 to 3.5 meter Optics for New Generations of Ground-based Telescopes Blaise Canzian1, A. Clarkson1, F. Piche1, J. B. Barentine2, J. Daniel2, T. Hull2 1L-3 Communications/ Brashear, 2L-3 Communications/ Tinsley. Exhibit Hall The advent of new requirements for intermediate and large telescopes has been accompanied by development of new processes and equipment to fabricate optics associated with these telescopes. We will discuss powerful new optical processing solutions that are being demonstrated. These methods offer extreme optical convergence of aspheric forms achieving demanding surface structure functions. Affected areas of astronomical telescope architecture include methods for rapid processing of segmented mirrors, and production of meniscus mirrors. We discuss finish and test of large turning flats as well as on-axis and off-axis aspheric primary and secondary mirrors. Furthermore, methods are now available to nearly fully mitigate substructure print-through of advanced lightweighted mirrors. Emerging optical fabrication solutions enlarge the design space for new generations of advanced astronomical telescopes. 157.18 Current Status of MMT Polarimeter (MMTPol) Megan M. Krejny1, K. Dewahl1, T. J. Jones1, C. Packham2, C. Warner1 1University of Minnesota, 2University of Florida. Exhibit Hall We present a progress report for MMTPol, an imaging polarimeter operating at 1-5 microns on the MMT telescope. MMTPol will work in conjunction with the adaptive optics secondary to produce images with high spatial resolution and polarimetric precision, making it ideal to observe phenomena such as protoplanetary disks, AGN and comets. We discuss the design and construction of the optics and cryogenics systems. We present results from the initial installation of the science grade detector array. Finally, we discuss the hexapod mount used to integrate MMTPol with the telescope. 157.19 The Productivity and Impact of Large Optical Telescopes Dennis Crabtree1 1NRC-HIA, Canada. Exhibit Hall The primary scientific output from an astronomical telescope is the collection of papers published in refereed journals. A telescope's productivity is measured by the number of papers published which are based upon data taken with the telescope. The scientific impact of a paper can be measured quantitatively by the number of citations that the paper receives. In this poster, I examine the productivity and impact of the several 8-m class telescopes including Gemini, Keck, Magellan, Subaru, and the VLT telescopes using paper and citation counts. I also present results for a subset of 4-m telescopes and HST for comparison. 158 Education, Public Outreach, Citizen Science and Science Impact Poster Session Exhibit Hall 158.01 Asteroids Outreach Toolkit Development: Using Iterative Feedback In Informal Education Vivian White1, M. Berendsen1, S. Gurton1, P. B. Dusenbery2 1Astronomical Society of the Pacific, 2Space Science Institute’s National Center for Interactive Learning. Exhibit Hall The Night Sky Network is a collaboration of close to 350 astronomy clubs across the US that actively engage in public outreach within their communities. Since 2004, the Astronomical Society of the Pacific has been creating outreach ToolKits filled with carefully crafted sets of physical materials designed to help these volunteer clubs explain the wonders of the night sky to the public. The effectiveness of the ToolKit activities and demonstrations is the direct result of a thorough testing and vetting process. Find out how this iterative assessment process can help other programs create useful tools for both formal and informal educators. The current Space Rocks Outreach ToolKit focuses on explaining asteroids, comets, and meteorites to the general public using quick, big-picture activities that get audiences involved. Eight previous ToolKits cover a wide range of topics from the Moon to black holes. In each case, amateur astronomers and the public helped direct the development the activities along the way through surveys, focus groups, and active field-testing. The resulting activities have been embraced by the larger informal learning community and are enthusiastically being delivered to millions of people across the US and around the world. Each ToolKit is delivered free of charge to active Night Sky Network astronomy clubs. All activity write-ups are available free to download at the website listed here. Amateur astronomers receive frequent questions from the public about Earth impacts, meteors, and comets so this set of activities will help them explain the dynamics of these phenomena to the public. The Space Rocks ToolKit resources complement the Great Balls of Fire museum exhibit produced by Space Science Institute’s National Center for Interactive Learning and scheduled for release in 2011. NSF has funded this national traveling exhibition and outreach ToolKit under Grant DRL-0813528. 158.02 A Cluster Of Activities On Coma From The Hubble Space Telescope, StarDate, And McDonald Observatory Mary Kay Hemenway1, S. Jogee1, K. Fricke1, S. Preston1 1Univ. of Texas. Exhibit Hall With a goal of providing a vast audience of students, teachers, the general public, and Spanish-speakers with activities to learn about research on the Coma cluster of galaxies based on the HST ACS Treasury survey of Coma, McDonald Observatory used a many-faceted approach. Since this research offered an unprecedented legacy dataset, part of the challenge was to convey the importance of this project to a diverse audience. The methodology was to create different products for different (overlapping) audiences. Five radio programs were produced in English and Spanish for distribution on over 500 radio stations in the US and Mexico with a listening audience of over 2 million; in addition to the radio listeners, there were over 13,000 downloads of the English scripts and almost 6000 of the Spanish. Images were prepared for use in the StarDate Online Astronomy Picture of the Week, for ViewSpace (used in museums), and for the StarDate/Universo Teacher Guide. A high-school level activity on the Coma Cluster was prepared and distributed both on-line and in an upgraded printed version of the StarDate/Universo Teacher Guide. This guide has been distributed to over 1700 teachers nationally. A YouTube video about careers and research in astronomy using the Coma cluster as an example was produced. Just as the activities were varied, so were the evaluation methods. This material is based upon work supported by the National Aeronautics and Space Administration under Grant/Contract/Agreement No. HST-EO-10861.35-A issued through the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. 158.03 Starship Asterisk: APOD and General Astronomy Discussion Forum Robert J. Nemiroff1 1Michigan Technological Univ.. Exhibit Hall A main discussion venue for the popular Astronomy Picture of the Day (APOD) website has been recently redesigned and upgraded. The online bulletin board is directly linked from the bottom of recent APODs served from http://apod.nasa.gov/ . Formerly known as "The Asterisk," the site's new design is called "Starship Asterisk" and now declares its forums to be places on a starship, with the current APOD considered as appearing on the main view screen on the Bridge. A central "mission" of Starship Asterisk is to support APOD in various ways. Toward this end, the Bridge forum exists primarily for the (archived) discussion of that day's APOD, the Observation Deck forum facilitates APOD image submissions, and the Library creates a forum where no student question about astronomy is considered to be too easy or too hard. Additionally, Starship Asterisk now includes an astronomy news-oriented links forum titled the Communications Center, a citizen science-oriented links collection called the Science Labs, and classrooms including a free online, textbook-free Astro 101 course, taught by the author, complete with video lectures and powerpoint slides. Typically, over 1,000 astronomy enthusiasts will browse Starship Asterisk on any given day. Although the vast majority of readers prefer to browse anonymously, the site has now garnered over 60,000 posts. A small but dedicated group of volunteer "officers" administer the bulletin board, answer questions about astronomy from curious APOD readers, and openly discuss various astronomy topics, frequently with intended humor. Perhaps surprisingly, the majority of volunteer officers tend NOT to be professional astronomers, but typically quite knowledgeable retirees exercising a lifelong interest in astronomy. 158.04 Amidst the Beauty of the Night Sky, Which of the Constellations am I? Kimberly A. Herrmann1 1Lowell Observatory. Exhibit Hall A well known constellation am I- I never set in the northern sky. Native Americans and Greeks, you see, Wrote legends when they recognized me. Two close stars still test for keen eyesight. Two point to the North Star - what a light! Look for my galaxies, you know where. I am ---- -----, the ----- ----! (If you've an answer you'd care to try, Or check out more riddles, please stop by! Note: All my astronomy riddles are copyrighted.) 158.05 Dark Skies, Bright Kids: Year 2 Joleen K. Carlberg1, K. Johnson1, R. Lynch1, L. Walker1, R. Beaton1, J. Corby1, G. de Messieres1, M. Drosback1, N. Gugliucci1, L. Jackson1, A. Kingery1, S. Layman2, E. Murphy1, W. Richardson1, P. Ries1, C. Romero1, G. Sivakoff1, K. Sokal1, G. Trammell1, D. Whelan1, A. Yang1, G. Zasowski1 1University of Virginia, 2Charlottesville Astronomical Society. Exhibit Hall The Dark Skies, Bright Kids (DSBK) outreach program brings astronomy education into local elementary schools in central Virginia's Southern Albemarle County through an after-school club. Taking advantage of the unusually dark night skies in the rural countryside, DSBK targets economically disadvantaged schools that tend to be underserved due to their rural locale. The goals of DSBK are to foster children's natural curiosity, demonstrate that science is a fun and creative process, challenge students' conceptions of what a scientist is and does, and teach some basic astronomy. Furthermore, DSBK works to assimilate families into students' education by holding family observing nights at the school. Now in its third semester, DSBK has successfully run programs at two schools with very diverse student populations. Working with these students has helped us to revise our activities and to create new ones. A by-product of our work has been the development of lesson plans, complete with learning goals and detailed instructions, that we make publically available on our website. This year we are expanding our repertoire with our new planetarium, which allows us to visualize topics in novel ways and supplements family observing on cloudy nights. The DSBK volunteers have also created a bilingual astronomy artbook --- designed, written, and illustrated by UVa students --- that we will publish and distribute to elementary schools in Virginia. Our book debuted at the last AAS winter meeting, and since then it has been extensively revised and updated with input from many individuals, including parents, professional educators, and a children's book author. Because the club is currently limited to serving a few elementary schools, this book will be part of our efforts to broaden our impact by bringing astronomy to schools we cannot go to ourselves and reaching out to Spanish-speaking communities at the same time. 158.06 The Hubble Education Program’s Tactile Astronomy: Making the Universe Touchable Bonnie Eisenhamer1, M. Mutchler1, K. Cordes1, D. Weaver1, H. Ryer1 1STScI. Exhibit Hall Tactile Astronomy supports the Hubble Education Program’s efforts in bringing the wonders of the universe to everyone, regardless of their visual ability. This new section of the Amazing Space Website features "Images of the Month;" a collection of the latest Hubble images that can be printed in a tactile format. The images are specifically designed to be downloaded and printed on a thermal paper expansion machine, thus allowing the visually impaired to feel what they cannot see. In addition, there is a "special projects" section that currently features the limited-edition Tactile Carina Nebula booklet and accompanying materials, such as background text about the Carina Nebula and an audio tour. The opening of Tactile Astronomy is in celebration of Hubble's 20th anniversary and features the 20th anniversary image of a small portion of the Carina Nebula. New tactile images and additional projects will continue to be added to the site. 158.07 7 Minutes of Totality in 7 Years: Planning Ahead for August 2017 Jennifer L. Bartlett1, S. Bell2 1US Naval Observatory, 2HM Nautical Almanac Office, United Kingdom. Exhibit Hall In rapid succession, two chances to experience a total solar eclipse will soon occur over the middle of the United States. Usually, a total solar eclipse is, at most, a once in a lifetime event. However, the celebrated shadows will race over the Shawnee National Forest, near Makanda, Illinois, twice in less than 7 years. The centerlines of the 2017 August 21 and 2024 April 08 eclipses will cross at this convenient location. If you are planning a trip to that legendary heart of darkness, you should consider a site just northwest of Makanda for both events. The two eclipse centerlines are expected to intersect at 37º 38.2’ N and 89º 15.4’ W, in the Shawnee National Forest. In 2017, totality lasting about 2 min 45 sec is expected at this location, which is the maximum duration for that eclipse. In 2024, nearly 4 min 13 sec of darkness will occur at the crossover point, but the longest period of totality for this eclipse will be seen in Mexico. Historically, southern Illinois is mostly sunny in late August and early April. If rain or clouds mar your 2017 experience, you can hope for better weather when you return in 2024. A number of activities can enrich your outreach program: spotting planets and stars, locating shadow effects, monitoring climate changes, and watching wildlife responses. In addition, you will be able to compare and contrast your observations during the two eclipses there. Planning an expedition to this rare intersection reduces your flexibility in case of inclement weather--a small price for the novelty of multiple visits. Unless you are a dedicated eclipse chaser, 2017 may not seem imminent. However, your outreach program choices now may shape your plans for the eclipses to come. For additional information, visit the USNO Eclipse Portal at http://www.eclipse.org.uk/eclbin/query_usno.cgi 158.08 Public Outreach Efforts of the Canadian Astronomical Society Dennis Crabtree1, J. Rosvick2, J. Bolduc-Duval3, J. Cami4, J. Di Francesco1, Y. Dutil5, L. Edwards6, J. E. Hesser1, N. Martimbeau7, P. Newbury8, G. Sarty9, I. Short10, H. Theijsmeijer11 1NRC-HIA, Canada, 2Thompson Rivers University, Canada, 3Cégep de Thetford Mines, Canada, 4University of Western Ontario, Canada, 5T3E, Canada, 6Caltech/IPAC, 7Montréal Planetarium, Canada, 8University of British Columbia, Canada, 9University of Saskatchewan, Canada, 10St. Marys University, Canada, 11Manitoulin Secondary School, Canada. Exhibit Hall The Canadian Astronomical Society (CASCA) has a very active Education and Public Outreach (EPO) Committee that promotes and supports astronomy education and outreach across Canada. The Committee submitted a White Paper to Canada’s Long Range Planning Panel in 2010 outlining the goals of Canadian astronomy EPO for the next 10 years. This poster will summarize the current activities of CASCA’s EPO Committee and present the Committee’s vision for the next decade of EPO in Canada. 158.09 More Than a Pretty Picture: Making WISE Data Accessible to the Public Nancy Ali1, B. Mendez1, K. Fricke1, E. L. Wright2, P. R. Eisenhardt3, R. M. Cutri4, R. Hurt5, WISE Team 1University of California Berkeley, 2UCLA, 3JPL, 4IPAC/Caltech, 5Caltech. Exhibit Hall NASA's Wide-field Infrared Survey Explorer (WISE) has surveyed the sky in four bands of infrared light, creating a treasure trove of data. This data is of interest not only to the professional astronomical community, but also to educators, students and the general public. The Education and Public Outreach (E/PO) program for WISE is creating opportunities to make WISE data accessible to these audiences through the Internet as well as through teacher professional development programs. Shortly after WISE took its first light image in January 2010, images have been featured weekly on the WISE website. These images serve to engage the general public through “pretty pictures” that are accompanied by educational captions. Social media such as Facebook and Twitter are used to further engage the public with the images. For a more comprehensive view of WISE images, we are creating a guided tour of the infrared sky on the WorldWide Telescope. The public will be able to use the free WorldWide Telescope software to interact with WISE images and listen to narration that describes features of the Universe as seen in infrared light. We are also developing resources for teachers and students to access WISE data when in becomes public in 2011 to learn about astronomical imaging and to conduct authentic scientific investigations. 158.10 GLOBE At Night: Mobilizing The Citizen-scientist Constance E. Walker1, M. Newhouse1 1National Optical Astronomy Observatory. Exhibit Hall GLOBE at Night is an annual international citizen-science event encouraging everyone to measure local levels of light pollution in February and March and contribute their observations online to a world map. (See www.globeatnight.org.) The campaign is hosted by the National Optical Astronomy Observatory (NOAO) in partnership with ESRI. In the last three years citizen-scientists from around the world contributed more than 50,000 observations, with nearly 18,000 data points from the 2010 campaign. During the same time, millions of touch-based, GPS-enabled smartphones and tablets have been sold worldwide. Each year NOAO staff has to discard data points due to inaccurate reporting of the location (latitude and longitude). Despite the use of innovative mapping tools on the data reporting web page, it is too easy to mistype numbers or forget a negative sign, spuriously relocating data points. Additionally, there is a time lag between when the data is collected at night and when it is reported later that can allow for additional error. One approach to address these problems would be to create a way to submit the data when it is observed and have a more automated GPS capability for reporting an accurate location. The rise in popularity of GPS-enabled mobile devices provides such a solution. These phones include state-of-the-art browsers that have access to the GPS and other data (date, time). These devices can potentially be used to show an appropriate magnitude/sky chart to the citizen-scientist and submit the data in real time, as the observation is made. NOAO staff is building a web application for mobile devices that will help realize these possibilities and potentially enable the accurate reporting of many more observations this year. Our poster will discuss this effort and describe what we hope to accomplish. 158.11 Citizen Sky, An Update on the AAVSO's New Citizen Science Project Rebecca Turner1, A. Price1, A. Henden1, R. Stencel2, B. Kloppenborg2 1AAVSO, 2University of Denver. Exhibit Hall Citizen Sky is a multi-year, NSF-funded, citizen science project focusing on the bright variable star, epsilon Aurigae. Citizen Sky goes beyond simple observing to include a major data analysis component. The goal is to introduce the participant to the full scientific process from background research to paper writing for a peer-reviewed journal. The first year of the project, 2009-10, was dedicated to developing project infrastructure, educating participants about epsilon Aurigae, and training these participants to observe the star and report their data. Looking forward, years two and three of the project will focus on assembling teams of participants to work on their own analysis and research. Results will be published in a special issue of the peer-reviewed Journal of the AAVSO. This project has been made possible by the National Science Foundation. 158.12 Development of DSLR Photometry as an Example of a Citizen Sky Team Brian K. Kloppenborg1, R. E. Stencel1, A. Price2, R. Turner2, A. Henden2 1University of Denver, 2AAVSO. Exhibit Hall One of the primary goals of the Citizen Sky project is to foster the development of Teams of every-day people with an interest in astronomy. These groups are composed of people with different, yet complementary skill sets who work together towards a common goal. Each team has a team leader and a professional astronomer assigned to act as an advisor. Here we highlight the work of one particular team who has produced documentation and software to teach first-time observers how to use consumer-grade digital cameras to produce accurate photometric magnitudes. We present a short history, the completed products, and lessons learned from this team. We acknowledge support from the NSF Informal Science Education Division, to the AAVSO and the University of Denver. 158.13 Facebooking Citizen Science with the Zooniverse Joseph Moore1, P. L. Gay2, K. Hogan2, C. Lintott3, C. Impey4, C. Watson5 1Southern Illinois University Edwardsville, 2Southern Illinois University Edwardsville / Astronomy Cast, 3Adler Planetarium / Oxford University, 4University of Arizona, 5freelance. Exhibit Hall While fully online citizen science projects like Galaxy Zoo and Moon Zoo are able to garner participation by tens to hundreds of thousands of people, this success pales next to the number of people who use Facebook. With a population well over half a billion, Facebook is, at the time of this writing, the largest single online community. As an experiment in social science-engagement, we have created Facebook fan pages for Zooniverse science tasks, social-sharing apps for Moon Zoo and Galaxy Zoo, and a novel galaxy-related citizen science project all within Facebook. In this poster we present early analysis on how these engagements attract both old and new users, and how users choose to share and interact through these pages. 158.14 Motivation of Citizen Scientists Participating in Moon Zoo Shanique Brown1, P. L. Gay1, C. S. Daus1 1Southern Illinois University Edwardsville. Exhibit Hall Moon Zoo is an online citizen science project with the aim of providing detailed crater counts for as much of the Moon’s surface as possible. In addition to focusing on craters, volunteers are encouraged to remain vigilant for sightings of atypical features which may lead to new discoveries. Volunteers accomplish these tasks by exploring images captured by NASA's Lunar Reconnaissance Orbiter (LRO) which has a resolution of 50cm per pixel. To be successful, Moon Zoo needs to attract and retain a large population of citizen scientists. In this study, we examine the factors motivating Moon Zoo participants who invest many hours exploring these images. In this, the first of a two-phased study, we conducted a qualitative analysis using semi-structured interviews as a means of data collection. A stratified sample of participants was used in an attempt to uncover the driving forces behind decisions to participate from a wide-range of participants. Inquiring and probing questions were asked about factors which led volunteers to Moon Zoo as well as reasons which kept them committed to exploring the Moon’s surface through this online portal. Responses were then categorized using a grounded theory approach, and frequency distributions are calculated where appropriate. Aggregate results from these interviews are presented here including the demographics of the sample and motivators as per the content analysis. The information gathered from this phase will be used to guide the development of an online survey to further explore volunteers’ motivation based on the presented classification schemes. The survey will then be used to guide future research and development in the area of citizen science in the field of astronomy. These findings will also be useful in charting new boundaries for future research. 158.15 Stars Above, Earth Below: Astronomy in the National Parks Tyler E. Nordgren1 1Univ. of Redlands. Exhibit Hall The U.S. national parks that protect our enjoyment of the landscape around us by day, also protect our enjoyment of the sky above at night. With the growth of light pollution, the view of the stars and Milky Way overhead has become as rare as the views of glaciers, geysers, and grizzlies that bring millions of visitors to the parks every year. Through the pristine view of a starry sky at night park visitors are primed to learn about our planet, its place in the solar system, and the larger Universe in which we live. The national parks are therefore the largest informal educational setting for reaching millions of people from all over the world who might not otherwise encounter astronomical outreach. The material in this presentation has been field tested in national parks, campgrounds, lodges, and visitor centers over the last four years and is elaborated on in the just released book: “Stars Above, Earth Below: A Guide to Astronomy in the National Parks.” Funding for this project was provided by The Planetary Society. Monday, January 10, 2011, 10:00 AM - 11:30 AM 102 Results from the First Year of Observations with the Cosmic Origins Spectrograph Special Session Ballroom 6C 102.01 Quasar Absorption Lines in the Extreme Ultraviolet: The Smoking Guns of Cosmic Feedback Todd Tripp1 1University of Massachusetts. 10:00 AM - 10:15 AM Ballroom 6C Three years ago at the winter AAS meeting I presented a talk entitled, perhaps somewhat pretentiously, "Terra Incognita: Probing The IGM-Galaxy Interface With COS." Now that the Cosmic Origins Spectrograph (COS) has been successfully installed on the Hubble Space Telescope, this instrument is delivering data that even exceed my hopes and predictions from three years ago. This talk will demonstrate that COS is enabling investigations of aspects of the Universe that have never been seen before. Specific examples will include the following: (1) Detections of absorption lines of Ne VIII and Mg X, which probe highly-ionized and low-density plasmas that can exist at temperatures in excess of 106 K. Due to the low density of galaxy halos and the IGM, X-ray emission from these plasmas is entirely undetectable with current or future missions. (2) Detections of remarkably strong O VI absorbers spanning velocity ranges in excess of hundreds of km/s, probably arising in galactic winds. While such outflows can be seen from the ground, the extreme ultraviolet provides a much richer suite of physical conditions diagnostics. (3) Detection of molecular hydrogen in unexpected places. An unifying thems of these examples is cosmic feedback and accretion -- these observations provide important new constraints on how galaxies interact with their surroundings. 102.02 The DAO of Tau: Disks, Accretion, and Outflows in an FUV Survey of T Tauri Stars Gregory J. Herczeg1 1Max-Planck-Institut, Germany. 10:15 AM - 10:30 AM Ballroom 6C Classical T Tauri stars offer a unique window into star+disk systems that are still in the accretion/outflow phase yet are no longer surrounded by an opaque circumstellar envelope. These objects hold the key to understanding how magnetospheric accretion occurs, how accretion powers outflows, and what the physical and chemical conditions are in the disks where planet formation occurs. Far-ultraviolet spectra of classical T Tauri stars provide powerful and unique diagnostics of each of these processes. In the ongoing Disks, Accretion, and Outflows of T Tau stars (DAO of Tau) program, we are using HST/COS and STIS to survey these diagnostics in high-resolution FUV spectra of 26 CTTSs and 6 WTTSs. Our first results include identifying new emission line diagnostics of the disk surface, detecting weak accretion in profiles of hot lines from a WTTS with a disk, finding warm winds from only some objects, and catching an amazing flare on a WTTS. 102.03 Observational and Theoretical Studies of the Intergalactic Medium J. Michael Shull1 1Univ. of Colorado. 10:30 AM - 10:45 AM Ballroom 6C The Cosmic Origins Spectrograph (COS) installed on the Hubble Space Telescope provides access to high-quality ultraviolet spectra of the intergalactic medium (IGM) and galactic halos. I will report on new COS results on the physical state, baryon content, and spatial distribution of the the IGM at redshifts z < 0.5. COS has also recently measured the epoch of reionization in helium (He II) toward HE2347-4342 at redshifts z < 2.9. This talk will also describe the Colorado group's numerical simulations of the IGM and dynamical and radiative feedback from galaxy formation, using the adaptive-mesh N-body hydrodynamic code Enzo. These simulations help us understand the effects of IGM shock-heating, metal-transport, radiative cooling, and photoionization of the complex structures in the "Cosmic Web" of matter. 102.04 Mysteries of the North Star: Far Ultraviolet HST/COS Spectroscopy of the Classical Cepheid Polaris Edward F. Guinan1 1Villanova Univ.. 10:45 AM - 11:00 AM Ballroom 6C Polaris (? UMi; F7Ib-II) is the best known star in the northern sky. It has enjoyed special standing since the Earth’s precession brought our north celestial pole to its almost exact direction. Polaris is also the nearest (~130 pc) and brightest (V ~ 1.97-mag) classical Cepheid. Polaris has proven to be full of surprises, displaying both a systematic decrease in light amplitude, an increase in pulsation period and a probable increase in luminosity. Presently Polaris has a light amplitude ?V~ 0.045-mag, its 3.97-day period is increasing at +3.5sec/year and its mean brightness has apparently increased by ~0.2-mag over the past century (Engle & Guinan 2006). Recent FUSE observations show the presence of CIII 977/1176A and OVI 1032/1038A emissions, indicative of hot ~30,000-300,000 K plasmas (Engle & Guinan, 2007). A study of IUE data indicates a possible small temperature increase (which in the FUV-region is very sensitive to Teff) between 1978/79 and 1991/93, indicating an increase of ~35+/-12K. Also, Polaris, along with two other Cepheids beta Dor and delta Cep, have been detected as soft-X-ray sources with log LX ~ 29.0 ergs/sec. But Polaris has a nearby binary companion that could contribute to the observed X-ray emission. HST/COS medium-resolution ~1150-2000Å spectrometry was conducted during Dec-2009. These observations were conducted to investigate possible evolutionary changes (manifested by small changes in Teff) and also to study upper atmospheric high energy emissions. Below ~1400A data is essentially free of the stellar continuum of the F8-supergiant and contains important diagnostic high energy emission lines such as C III, Ly-alpha, NV, OI, CII, & Si IV. At wavelengths >1600A, the stellar photospheric flux rapidly increases. We report on analyses of the COS observations and discuss implications for Cepheid evolution and upper atmosphere heating mechanisms. This work is supported by NASA Grant-HST-GO-11726. 102.05 Size and Kinetic Luminosity of Low Redshift Quasar Outflows Nahum Arav1 1Virginia Tech. 11:00 AM - 11:15 AM Ballroom 6C Over the past several months the new UV spectrograph aboard HST is giving us high quality data of AGN outflows, aka warm absorbers to the X-ray community. I will describe very new results from our program that aim at finding the size, kinetic luminosity and chemical abundances of these outflows. We acknowledge support from NASA through HST program (11686), and from NSF grant AST 0837880. 103 Kepler I Oral Session Ballroom 6B 103.01 Confirming The Planetary Nature Of Kepler Transit Candidates Orbiting Pulsating Stars With Light Travel Time Measurements Jessie Christiansen1, J. F. Rowe1, F. Mullally1, Kepler Science Team 1NASA Ames Research Center/SETI Institute. 10:00 AM - 10:10 AM Ballroom 6B The first extrasolar planets were found orbiting pulsars, and were detected via the changes in the arrival time of the pulses caused by the gravitational effect of the planets on the pulsar. Planets orbiting pulsating stars, such as delta Scuti/gamma Doradus stars, will distort the arrival times of maximum light in the light curves of these stars in the same fashion. We investigate the possibility of detecting this phenomenon in Kepler light curves, and constrain the mass limits that could be set on transiting companions. This method would provide an independent test of the planetary nature of Kepler transiting candidates. Kepler was selected as the 10th mission of the Discovery Program. Funding for this mission is provided by NASA, Science Mission Directorate. 103.02 A Bayesian Approach to Systematic Error Correction in Kepler Photometric Time Series Jon Michael Jenkins1, J. VanCleve1, J. D. Twicken1, J. C. Smith1, Kepler Science Team 1SETI Institute. 10:10 AM - 10:20 AM Ballroom 6B In order for the Kepler mission to achieve its required 20 ppm photometric precision for 6.5 hr observations of 12th magnitude stars, the Presearch Data Conditioning (PDC) software component of the Kepler Science Processing Pipeline must reduce systematic errors in flux time series to the limit of stochastic noise for errors with time-scales less than three days, without smoothing or over-fitting away the transits that Kepler seeks. The current version of PDC co-trends against ancillary engineering data and Pipeline generated data using essentially a least squares (LS) approach. This approach is successful for quiet stars when all sources of systematic error have been identified. If the stars are intrinsically variable or some sources of systematic error are unknown, LS will nonetheless attempt to explain all of a given time series, not just the part the model can explain well. Negative consequences can include loss of astrophysically interesting signal, and injection of high-frequency noise into the result. As a remedy, we present a Bayesian Maximum A Posteriori (MAP) approach, in which a subset of intrinsically quiet and highly-correlated stars is used to establish the probability density function (PDF) of robust fit parameters in a diagonalized basis. The PDFs then determine a “reasonable” range for the fit parameters for all stars, and brake the runaway fitting that can distort signals and inject noise. We present a closed-form solution for Gaussian PDFs, and show examples using publically available Quarter 1 Kepler data. A companion poster (Van Cleve et al.) shows applications and discusses current work in more detail. Kepler was selected as the 10th mission of the Discovery Program. Funding for this mission is provided by NASA, Science Mission Directorate. 103.03 Validating Kepler Planet Candidates Jack J. Lissauer1, G. Torres2, G. Marcy3, T. Brown4, R. Gilliland5, T. N. Gautier6, H. Isaacson3, A. Dupree2, Kepler Science Team 1NASA Ames Research Center, 2Center for Astrophysics, 3University of California, 4LCOGT, 5STScI, 6JPL. 10:20 AM - 10:30 AM Ballroom 6B The Kepler Science Team has identified more than 700 transit-like signatures in the first 43 days of data returned from the spacecraft (Borucki et al. 2010, arXiv1006.2799B). However, only 7 of these candidates have been confirmed as planets as of late September 2010. The number of true planets in this sample is clearly far larger than 7, but the sample is also 'contaminated' with false-positives, including many from eclipsing binary stars. Separating the wheat from the chaff requires a careful study of individual candidates using both Kepler photometry and spectroscopic and imaging data from the ground. Techniques that the Science Team is developing to address these issues, which include detailed analysis of the photometric data and follow-up observations with ground-based telescopes, will be presented. Kepler was selected as the 10th mission of the Discovery Program. Funding for this mission is provided by NASA, Science Mission Directorate. 103.04 Kepler Discovery Of An A-star With A Hot-planetary Companion. Jason Rowe1, W. J. Borucki1, S. B. Howell2, R. L. Gilliland3, L. A. Buchhave4, N. M. Batalha5, D. W. Latham6, Kepler Science Team 1NASA Ames Research Center, 2National Optical Astronomy Observatory, 3Space Telescope Science Institute, 4Niels Bohr Institute, Copenhagen University, Denmark, 5San Jose State University, 6Harvard-Smithsonian Center for Astrophysics. 10:30 AM - 10:40 AM Ballroom 6B We present Kepler photometry of a bright (Kepmag=10) closely separated (1”) A-star stellar binary. Time series photometry of the system reveals a transiting Jupiter-sized companion in a 1.76 d orbit. Detailed modeling of the phased light curve in conjunction with high-resolution speckle imaging allow us to identify the true host of the transiting companion and to account for third light contamination. The high-duty cycle and precision of Kepler photomety enables us to observe phase-changes of the planet as well as Doppler boosting and ellipsoidal distortions of the host star. With these observations we measure the mass, radius, temperature and orbital solution of the companion and confirm its planetary nature. Kepler was selected as the 10th mission of the Discovery Program.  Funding for this mission is provided by NASA, Science Mission Directorate. 103.05 The Architectures of Planetary Systems from Transit Observations Eric B. Ford1, D. C. Fabrycky2, M. J. Holman3, J. J. Lissauer4, A. V. Moorhead1, R. C. Morehead1, D. Ragozzine3, J. H. Steffen5, D. Koch4, Kepler Science Team 1Univ. of Florida, 2UC Santa Cruz, 3CfA, 4NASA Ames, 5Fermilab. 10:40 AM - 10:50 AM Ballroom 6B The architectures of multiple planet systems can provide valuable constraints on models of planet formation, including the extent and cause of orbital migration, eccentricity excitation and inclination excitation. NASA's Kepler mission has discovered a planetary system with multiple transiting planets (Holman et al. 2010) and several stars with multiple transiting planet candidates (Steffen et al. 2010). For each planet, transit photometry can measure the orbital period, orbital phase, transit duration, planet size (relative to the host star), and, in favorable cases, the orbital inclination. For systems with multiple transiting planets, one can begin to piece together the architecture of the planetary system, including key features such as the proximity to mean motion resonance, potential for significant secular interactions, and the likely relative inclinations. The set of potential architectures can often be further narrowed by incorporating the constraint of long-term orbital stability (for plausible mass-radius relations) and/or incorporating complimentary observations (e.g., radial velocities, Rossiter-McLaughlin effect, transit timing, out-of-transit light curve). We describe the methodology for characterizing the architecture transiting planet systems and present early results of such analyses for the Kepler-9 system, as well as candidate multiple planet systems previously identified by Kepler. Funding for Kepler is provided by NASA's Science Mission Directorate and for this research by the Kepler Participating Scientist Program. 103.06 The Distribution of Orbital Eccentricities for Kepler Planet Candidates Althea Moorhead1, E. B. Ford1, R. Morehead1, Kepler Science Team 1University of Florida. 10:50 AM - 11:00 AM Ballroom 6B The population of exoplanets detected with the radial velocity method has revealed that Jupiter-size planets possess a large range in orbital eccentricity, with a characteristic eccentricity of about 0.3. This discovery has revolutionized our theories of planet formation. With the additional discovery of hundreds of exoplanet candidates by the Kepler mission, we can probe the eccentricity distribution of smaller exoplanets.  Due to a near degeneracy between the eccentricity, direction of pericenter and impact parameter, transit photometry alone will not measure the orbital eccentricity for most planets discovered by Kepler. In some cases, it will be possible to measure eccentricities of individual planets thanks to complementary observations (e.g., radial velocities, transit timing variations, occultation photometry, NIR transit photometry). Even in the absence of individual eccentricities, it is possible to study the distribution of eccentricities based on the distribution of transit durations (relative to the maximum transit duration for a circular orbit). We present an early analysis of the duration distribution for planet candidates identified by the Kepler mission and discuss the implications for the eccentricity distribution. We compare results for giant and smaller planet candidates. Additionally, we identify planet candidates whose transit durations exceed the maximum transit duration for a circular orbit (which depends on the density of the host star). We consider the possibility of inaccurate stellar densities and the implications of the long-duration transit candidates for the exoplanet eccentricity distribution and its dependence on planet size. 103.07 KOI-54: The Remarkable Pulsating, Periastron-Pumped Binary Star William F. Welsh1, J. A. Orosz1, R. L. Gilliland2, C. Aerts3, T. M. Brown4, E. Brugamyer5, W. D. Cochran5, J. A. Guzik6, D. W. Kurtz7, D. W. Latham8, G. W. Marcy9, S. A. Quinn8, W. Zima3, D. G. Koch10, W. J. Borucki10, Kepler Science Team 1San Diego State University, 2STScI, 3Instituut voor Sterrenkunde, KU Leuven, Belgium, 4LCOGT, 5Univ. of Texas, 6LANL, 7Univ. Central Lancashire, United Kingdom, 8CfA, 9UC Berkeley, 10NASA Ames. 11:00 AM - 11:10 AM Ballroom 6B A previously-known unremarkable A star has been discovered by Kepler to be a fascinating object: KOI-54 exhibits sharp brightening events every 42 days and a beat-pattern of pulsations locked in phase with the brightenings. We have determined that this is a highly eccentric face-on binary star system and the brightenings are due to tidal distortion plus mutual irradiation of the stars at periastron passage. The periodic driving produces a rich set of tidally-induced g-mode pulsations locked to the orbital period. We present spectral analysis, radial velocities, the exquisite Kepler photometry of KOI-54, and a model that successfully reproduces these observations. Kepler was selected as the 10th mission of the Discovery Program. Funding for this mission is provided by NASA, Science Mission Directorate. 103.08 The High Albedo of the Hot-Jupiter Kepler-7b Brice-Olivier Demory1, S. Seager1, H. Kjeldsen2, Kepler Science Team 1Massachusetts Institute of Technology, 2Department of Physics and Astronomy Aarhus University, Denmark. 11:10 AM - 11:20 AM Ballroom 6B Kepler-7b is the least dense extrasolar planet discovered to date. This 4.9-day period hot-Jupiter has a mass of half of Jupiter (0.47 MJ) but a radius 50% larger (1.48 RJ). We present a global analysis of this system including more than 180 high-precision transits and occultations obtained with NASA's Kepler mission. Our best fit to the observations yields a high geometric albedo, with a minor part due to the planetary thermal emission. Therefore most of the planet light observed by Kepler is scattered light, suggesting the presence of a highly reflective layer in its upper atmosphere. We discuss the nature of this layer, possibly made of silicate condensates forming high-altitude clouds decks. Kepler was selected as the 10th mission of the Discovery Program. Funding for this mission is provided by NASA, Science Mission Directorate. 103.09 Validation And Characterization Of Kepler Exoplanet Candidates With Warm Spitzer Jean-Michel Desert1, Kepler Science Team 1Harvard University. 11:20 AM - 11:30 AM Ballroom 6B I present the status and results from an ongoing project to use 800 hours of the Spitzer SpaceTelescope to gather near-infrared photometric measurements of transiting extrasolar planet candidates detected by the Kepler Mission. By combining occultation measurements of the reflected starlight in the optical with estimates of the thermal emission in the near-infrared, we are able to constrain the energy budget of these planets and compare such constraints to those for the Solar system giant planets. By comparing the light curves spanning times of primary transit for candidates observed with Kepler and Spitzer, we can exclude significant sources of astrophysical false positives resulting from blends (e.g. background eclipsing binaries) that mimic an exoplanetary signature in the Kepler bandpass. I show how our infrared observations can help to validate the planetary nature of several candidates with small radii, which could be rocky in composition. 104 HEAD: High Energy Processes in Star Formation Special Session Ballroom 6A 104.01 X-Ray Spectroscopy of Accretion Shocks in Young Stars Nancy S. Brickhouse1 1Harvard-Smithsonian, CfA. 10:00 AM - 10:15 AM Ballroom 6A High resolution X-ray spectroscopy of accreting young stars is providing new insights into the physical conditions of the shocked plasma. While young stars exhibit exceedingly active coronae (>10 MK) with highly energetic flares, the relatively low temperature (~3 MK), high density (>1012 cm-3) accretion shock can only be clearly distinguished at high spectral resolution. The nearby Classical T Tauri star TW Hydrae was the first to show evidence of accretion using 50 ks with the Chandra High Energy Transmission Grating (HETG). More recently a Chandra HETG Large Program (489 ks obtained over the course of one month) on TW Hydrae has found evidence for a new type of coronal structure. In the standard model, the accreting gas shocks near the atmosphere of the star and gently settles onto the surface as it slows down and cools. On TW Hydrae the observed post-shock region is not this predicted settling flow, since its mass is 30 times the mass of material that passes through the shock. Instead the stellar atmosphere must be heated to soft X-ray emitting temperatures. Of the CTTS systems observed with the gratings on Chandra and XMM-Newton not all show the accretion shock signature; however, all of them show excess soft X-ray emission related to accretion. The production of highly charged ions in the proximity of both open and closed magnetic field lines has important implications for coronal heating, winds and jets in the presence of accretion. This work is supported by the Chandra X-ray Observatory through a NASA contract with the Smithsonian Astrophysical Observatory. 104.02 X-ray Irradiation of Protoplanetary Accretion Disks Alfred E. Glassgold1 1UC, Berkeley. 10:15 AM - 10:30 AM Ballroom 6A Young stellar objects radiate large numbers of keV-photons that are able to penetrate significant columns of gas and thus ionize and heat circumstellar material, including the accretion disks and outflows of very young stars. The unshielded ionization rates are high. At a distance of 1 AU from a young stellar object with a moderately strong X-ray source, they can be 100 million times the standard ionization rate associated with galactic cosmic rays. X-ray irradiation of a typical T Tauri star disk generates a layered atmosphere, ranging from a thin H II region through hot and warm regions on top of the main accretion disk. In the transition from warm to cool, the gas changes from atomic to molecular. This transition region produces a rich set of emission lines from the ultraviolet through the infrared. A good diagnostic of the effects of X-rays from young stellar objects is the Ne II fine structure line at 12.8 microns. This line has now been detected in more than fifty young stellar objects by Spitzer and ground-based telescopes. Since X-rays from young stellar objects penetrate disks down to vertical column densities of order 10 g per square cm, they help determine the location of the active accretion layer of disks governed by the magneto-centrifugal instability. In addition to directly probing the disk, stellar X-rays affect the stellar and disk winds of young stellar objects, including photo-evaporative flows, and thereby influence the dispersal of circumstellar disks. 104.03 X-rays from Young Massive Stars David H. Cohen1 1Swarthmore College. 10:30 AM - 10:45 AM Ballroom 6A O stars are powerful sources of X-ray emission and are often the strongest X-ray sources in young clusters and SFRs. Massive stars are not magnetically active, even in the minority of cases where they have detectable magnetic fields. Rather, their X-ray emission is caused by one (or more) of three mechanisms: embedded wind shocks in all O stars, colliding wind shocks in close binaries, and magnetically channeled wind shocks in massive stars with strong dipole magnetic fields. I will discuss these mechanisms and their manifestations in three specific examples: the O2 supergiant HD 93129A in Trumpler 14, Kleinman's Anonymous Star in M17, and theta1 Ori C in the Orion Nebula Cluster. 104.04 Numerical Simulations of Accretion and Outflows in Young Stars Marina M. Romanova1 1Cornell University. 10:45 AM - 11:00 AM Ballroom 6A I will discuss results of 2D and 3D MHD simulations of disk accretion onto young rotating magnetized stars. The disk magnetosphere interaction leads to formation of funnel streams and hot spots on the stellar surface. The energy distribution in the spots is such that the highest energy photons are expected to radiate from the central parts of spots. The oscillation of the shock wave is expected but it can be smeared by the inhomogeneity in the shock front. If the disk carries the magnetic field, then the disk magnetosphere interaction leads to reconnection events and possibly to the X-ray flares. MRI simulations show different flaring behavior in cases of the parallel and anti-parallel fields. Non-stationary accretion can lead to the conical shaped winds similar to X-winds from the disk-magnetosphere boundary, where 10-30 percent of matter is accelerated by the magnetic force up to and beyond the escape speed. A smaller part of matter is accelerated up to much higher velocities in the axial region along stellar field lines. Research is supported by NASA and NSF grants. 104.05 The High-Energy Environment of Young Stars Manuel Guedel1 1University of Vienna, Austria. 11:00 AM - 11:15 AM Ballroom 6A The environment of young stars is shaped by a complex interplay between stellar radiation, circumstellar material such as disks or envelopes, mass accretion flows onto the star, mass outflows from the star or the stellar disk, and jets accelerated near the star. High-energy radiation and particles are especially important in ionizing and heating the circumstellar gas and to drive chemical networks. Radio and soft X-ray radiation provide the best evidence for high-energy processes in young stars, and relevant observations suggest that much of the high-energy output is the consequence of frequent flaring. This concept predicts high-energy output not yet accessible to observations, such as non-thermal hard X-ray radiation beyond 10 keV, frequent coronal mass ejections, and high-energy particles in the stellar winds. On larger scales, outflows and jets produce high-energy radiation as well, although the heating mechanism is not entirely clear. Jet X-rays add to the circumstellar radiation field On the largest scales, one finds extended plasma bubbles in star-forming regions that contribute further X-ray emission to the stellar environment. I will discuss the above issues and present new observations that suggest an important role for high-energy processes in young stellar environments. 104.06 Fast Magnetic Reconnection and Acceleration of Energetic Particles Alex Lazarian1 1Univ. of Wisconsin. 11:15 AM - 11:30 AM Ballroom 6A Magnetic reconnection is a process that changes magnetic field topology and releases magnetic energy. In most astrophysical environments, including most of the ISM, the electric conductivity is high and the transforming of magnetic energy into Ohmic heating during reconnection is negligible. This opens interesting possibilities of transforming a substantial part of the magnetic energy into the energy of cosmic rays, provided that there exist a process of fast magnetic reconnection. A model of magnetic reconnection proposed in Lazarian & Vishniac (1999) is appealing as it predicts that the only requirement for the fast reconnection is the presence of turbulence. The latter is ubiquitous in astrophysical environments. The model has been successfully tested numerically recently and I shall discuss its implications for particle acceleration. I shall show evidence of the existence of both the first and second order Fermi acceleration processes in the numerical simulations that make use of the reconnection set ups in weakly turbulent environments. The recent data obtained with Voyagers and with MILAGRO data is suggestive that magnetic reconnection does accelerate energetic particles. This opens a new avenue for the cosmic ray acceleration research. 105 Binary Stellar Systems, X-ray Binaries Oral Session Room 615/617 105.01D Optical Studies of ?-Ray Binaries Christina Aragona1 1Lehigh University. 10:00 AM - 10:20 AM Room 615/617 Recently, the launch of the Fermi Gamma-Ray Observatory has led to the discovery of many new ?-ray sources, including ?-ray binaries. These systems are high mass X-ray binaries which exhibit an unusual feature of very high energy MeV-TeV emission. Six high mass X-ray binaries have been observed which fulfill these criteria: LS 5039, LS I +61 303, PSR B1259--63, Cyg X-1, Cyg X-3, and HESS J0632+057. LS 5039, LS I +61 303, and Cyg X-3 have all been detected by Fermi and are included in the Fermi LAT one-year Point Source Catalog. Analysis of the high energy emission for these sources relies partly on optical studies which reveal details about the orbital parameters, the mass donor star, and the stellar wind. Here, I will present results from optical spectra of LS 5039 and HD 259440, the proposed optical counterpart of HESS J0632+057. I have used spectra of the H alpha line obtained with the Southern Astrophysical Research (SOAR) Telescope to examine the stellar wind of LS 5039. The possible binarity of HD 259440 has not been confirmed although X-ray and gamma-ray properties of the system are consistent with other known gamma-ray binaries. Using optical spectra of this system, I have determined the physical properties of the massive star and placed constraints on the orbital parameters. I am grateful for support from NASA DPR Nos. NNX08AV70G, NNX09AT67G, NNG08E1671, and an institutional grant from Lehigh University. 105.02D Fundamental Properties of Accreting Compact Objects Jennifer L. Blum1 1University of Michigan. 10:20 AM - 10:40 AM Room 615/617 Galactic accreting compact objects, such as stellar-mass black holes and neutron stars can give us a unique perspective into the behavior of matter in extreme conditions. However, the exact nature of accretion onto these objects is not yet well understood. X-ray studies provide us with a means to observe the innermost regions around these objects and to test our theories of general relativistic physics. Through X-ray analyses we can constrain the physical parameters necessary to make logical deductions regarding compact object properties, such as disk winds, relativistic jets, the Kerr metric, and the neutron star equation of state. Here we present spectral modeling results from three accreting X-ray binaries. Specifically, we analyze Suzaku spectra from two stellar-mass black hole X-ray binaries, GRS 1915+105 and H1743-322, and one neutron star X-ray binary, 4U 1636-53. For GRS 1915+105 and 4U 1636-53, we use the relativistic iron line, which is part of a reflection spectrum, as a diagnostic for measuring black hole spin and neutron star radius, respectively. We find that while we can exclude a spin of zero at the 2 sigma level of confidence for GRS 1915+105, data selection and disk reflection modeling nuances can be important when estimating the spin value. For 4U 1636-53, we provide upper limits on the neutron star radius by estimating the radial extent of the inner accretion disk, which are important for constraining models for the neutron star equation of state. Moreover, when testing for the presence of disk winds in H1743-322 (which are key to understanding the nature of accretion disk outflow), we do not detect Fe XXV or Fe XXVI absorption lines in its spectra of H1743-322; implying that disk winds may be state dependent. 105.03 Planetary Nebulae, Blue Stragglers and Binary Mergers Orsola De Marco1, G. H. Jacoby2, J. Davies3, H. E. Bond4, P. Harrington5 1Macquarie University, Australia, 2Carnagie Observatories & GMT, 3Caltech, 4Space Telescope Science Institute, 5University of Maryland. 10:40 AM - 10:50 AM Room 615/617 The plot has thickened over the origin of planetary nebulae (PN) and the role played by binary interactions. One of the outstanding questions is why the brightest PN in every galaxy is limited to the same maximum brightness (making the ensemble of PN a standard candle): in older galaxies PN should be less luminous than in younger galaxies because their central stars have lower mass and luminosity. It has been proposed that the bright end of the PN luminosity function is populated by PN descending from blue stragglers, stars that have a binary or even merger origin, making over-massive and over-luminous PN in old populations. Without blue stragglers, PN should be absent in the oldest populations such as globular clusters. There are, however, 4 PN known in the Galactic globular cluster system. We present here HST observations of two of them, JaFu1 (in Pal 6) and IRAS18333-2357 (in M22) that reveal characteristics (e.g., central star mass, nebular morphology) that support the binary origin hypothesis. 105.04 Angular Momentum Transport during Direct Impact Mass Transfer Jeremy F. Sepinsky1, B. Willems2, V. Kalogera2 1University of Scranton, 2Northwestern University. 10:50 AM - 11:00 AM Room 615/617 We investigate the transfer of angular momentum between the components of an interacting binary system where mass in transferred via Roche lobe overflow resulting in direct impact onto the surface of the accretor. We model the stars as spherically symmetric rigid spheres and assume the mass transfer stream follows the trajectory of a ballistic point mass ejected from the inner Lagrangian point of the donor star. We approximate the mass transfer stream by discrete, non-interacting ballistic particles, conserving the linear and angular momentum of the three-body problem during ejection, accretion, and transport. We find that, contrary to popular assumptions, direct impact accretion can actually facilitate the transfer of angular momentum from the spin of the donor star to the binary orbit. Thus, by increasing the orbital angular momentum of the binary, direct impact mass transfer may increase the stability of such systems, significantly affecting the expected evolution timescales. We show the exchange of orbital angular momentum between the components of a binary system undergoing this process for a wide range of system parameters. 105.05 Vlbi Astrometric Orbit Solutions Of The Triple Systems Algol And Ux Arietis Robert Lucien Mutel1, W. M. Peterson1, M. Guedel2, M. Goss3 1Univ. of Iowa, 2University of Vienna, Austria, 3NRAO. 11:00 AM - 11:10 AM Room 615/617 Multi-epoch phase-referenced VLBI observations are a powerful technique to make sub-milliarcsecond astrometric measurements. We report on high-accuracy orbit and proper motion determination of the well-known active binaries Algol and UX Arietis, combining multi-epoch HSA and VLBA phase-referenced observations with archival VLBI datasets. We find that both Algol and UX Arietis are triple systems, For Algol, we refine the proper motion and outer orbit solutions, confirming the recent optical result of Zavala et al. (2010) that component C’s position angle had been reported in error by 180 deg. For UX Arietis, we find a third component orbital solution that accounts for previous VLBI reports of an acceleration term in the proper motion fit. 105.06 Multi-wavelength Observations Of The Psr B1259-63/ Ss 2883 Be Star Periastron In 2010 Aous Abdo1, Fermi LAT collaboration, S. Johnston2, E. Grundstrom3, M. Roberts4 1Naval Research Laboratory, 2ATNF, Australia, 3Vanderbilt University, 4Eureka Scientific. 11:10 AM - 11:20 AM Room 615/617 PSR B1259-63/SS 2883 is a unique binary system consisting of a 47.7 ms radio pulsar orbiting a massive (10 - 15 M?) Be companion star. The pulsar orbits the companion star with a period of ~3.4 years in a highly eccentric orbit. We have scheduled a coordinated radio, IR, optical, X-ray, and GeV gamma-ray observing campaign for the December 2010 periastron passage. This is the first periastron since the launch of the Fermi Gamma-ray Space Telescope and thus provides for the first time the opportunity to observe the passage of the source through the Be stellar disk at GeV energies with such a sensitive instrument. We will present results from our multi-wavelength campaign. 105.07 Low-Frequency Oscillations in Global Simulations of Black Hole Accretion Sean M. O'Neill1, C. S. Reynolds2, M. C. Miller2, K. Sorathia3 1University of Colorado at Boulder/JILA, 2University of Maryland, College Park/Joint Space Science Institute (JSI), 3University of Maryland, College Park. 11:20 AM - 11:30 AM Room 615/617 We present the results of a numerical exploration of low-frequency variability in black hole accretion disks. Specifically, we have conducted a global, magnetohydrodynamic simulation of a thin, magnetized accretion flow that evolves for over 1,500 inner disk orbits. We have identified in this simulation the presence of dynamo cycles that manifest themselves predominantly as oscillations in the azimuthal magnetic field over timescales ten to twenty times longer than the local orbital period. Interestingly, these cycles occupy discrete frequencies that in many instances share power across broad radial ranges. We also connect the simulated dynamo cycles to several properties of observed low-frequency quasi-periodic oscillations in galactic black hole binary systems, noting that the cycles have the appropriate frequencies and narrow-band profiles and that they are located in a region associated with X-ray emission in real systems. This work clearly illustrates that magnetized disk dynamos can exhibit variability on timescales much longer than any timescale that would emerge from test particle considerations. Funding for this work has been supplied by the NSF, NASA, and the Maryland-Goddard Joint Space Science Institute (JSI). 106 AGN, QSO, Blazars I Oral Session Room 618/620 106.01 Discovery Of A Radio-selected Z ~ 6 Quasar Gregory Zeimann1, R. H. Becker1, R. L. White2, S. A. Stanford3 1UC Davis, 2Space Telescope Science Institute, 3Lawrence Livermore National Laboratory. 10:00 AM - 10:10 AM Room 618/620 High redshift (z>5.7) represent some of the earliest and brightest objects in the Universe. These distant super-massive black holes are important in the study of galaxy evolution and the re-ionization epoch. Much of the ~60 known z>5.7 quasars are optically-selected with red i'-z' colors and blue z'-J colors. Optical-selection may miss a substantial population of reddened quasars (red z'-J colors) that can be found through radio-selection. McGreer et al. (2006) discovered a z=6.21 radio-selected quasar with colors that placed it outside of the usual optical-selection. We present the discovery of only the second radio-selected z>5.7 quasar known (z=5.92). We also discuss the implications of the discovery and future efforts. 106.02D The Hot Environments of X-shaped Radio Galaxies Edmund J. Hodges-Kluck1, C. S. Reynolds1 1University of Maryland. 10:10 AM - 10:30 AM Room 618/620 X-shaped radio galaxies (XRGs) are unusual radio galaxies with a second pair of inactive lobes in addition to the canonical double-lobed source. The origin of the inactive lobes is not understood, and two dramatically different hypotheses have been proposed: either they are the result of a rapid reorientation of the AGN jet axis (possibly due to a supermassive black hole merger---XRGs have been held up as a predictor of merger rates) or they are produced by the deflection of relativistic lobe plasma flowing back (backflow) from the "hot spot" terminal shocks in the active lobes. These hypotheses have been explored by radio and optical observations, but the backflow hypothesis relies on the hot ISM or intragroup/intracluster medium to shape the radio source. In this work, we have studied the effect of the hot medium with Chandra and 3D hydrodynamic modeling of extragalactic radio sources. We present these results and argue that while the properties of the hot gas atmospheres are important, the backflow hypothesis needs to be modified before it can successfully explain XRG morphology. We also demonstrate that X-ray observations can be used to constrain the rapid reorientation model using one particular XRG. This research was funded in part by Chandra grants GO89109X, GO90111X, and GO011138A. 106.03D Fermi Large Area Telescope Observations of a Candidate Young Radio Source William McConville1, L. Ostorero2, R. Moderski3, L. Stawarz4, C. C. Cheung5, Fermi LAT Collaboration 1NASA GSFC / University of Maryland, 2Dipartimento di Fisica Generale ``Amedeo Avogadro'', Universita degli Studi di Torino, Italy, 3Nicolaus Copernicus Astronomical Center, Poland, 4Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Japan, 5Space Science Division, Naval Research Laboratory. 10:30 AM - 10:50 AM Room 618/620 Using 19 months of Fermi LAT data, we investigate the gamma-ray properties of the radio-loud active galaxy 4C+55.17 (z=0.896) and re-examine its classification as a quasar-hosted blazar, considering instead its possible nature as a gamma-ray emitting young radio source. The active galaxy 4C+55.17 has a history of gamma-ray observations dating back to the EGRET era. Commonly classified as a Flat Spectrum Radio Quasar (FSRQ) due to its radio spectral shape and broad optical emission lines, the association of the EGRET source with 4C+55.17 remained tentative at the time, as the source exhibited spectral and morphological properties that were unlike any of the other bright gamma-ray blazars. With the improved angular resolution and sensitivity of the Large Area Telescope on board the Fermi Gamma-ray Space Telescope, the association of the gamma-ray source with 4C+55.17 is now confirmed due to the precise gamma-ray localization. An investigation of the gamma-ray properties of this source has revealed it to be an atypical member of the gamma-ray emitting FSRQ's, with an unusually hard and non-variable gamma-ray spectrum which extends up to the observed photon energies of 145 GeV despite its considerably high redshift for a very-high energy (>100 GeV) emitter. We further show that the high energy (>100 MeV) spectrum of this source may be formally extrapolated into the detectable range of ground-based Cherenkov telescopes, making it a compelling candidate for very-high energy observations, and in particular for future studies of the extragalactic background light. 106.04 The Sudden Death Of The Nearest Quasar Kevin Schawinski1, D. A. Evans2, S. Virani3, M. Urry1, W. C. Keel4, P. Natarajan1, C. J. Lintott5, A. Manning4, P. Coppi1, S. Kaviraj6, S. Bamford7, G. I. G. Jozsa8, M. Garrett8, H. van Arkel8, P. Gay9, L. Fortson10 1Yale University, 2MIT, 3James Madison University, 4University of Alabama, 5Oxford University, United Kingdom, 6Imperial College, United Kingdom, 7University of Nottingham, United Kingdom, 8ASTRON, Netherlands, 9Southern Illinois University Edwardsville, 10University of Minnesota. 10:50 AM - 11:00 AM Room 618/620 Galaxy formation is significantly modulated by energy output from supermassive black holes at the centers of galaxies which grow in highly efficient luminous quasar phases. The timescale on which black holes transition into and out of such phases is, however, unknown. We present the first measurement of the shutdown timescale for an individual quasar using X-ray observations of the nearby galaxy IC 2497, which hosted a luminous quasar no more than 70,000 years ago that is still seen as a light echo in `Hanny's Voorwerp', but whose present-day radiative output is lower by over 4 orders of magnitude. This extremely rapid shutdown provides new insights into the physics of accretion in supermassive black holes, and may signal a transition of the accretion disk to a radiatively inefficient state. 106.05 Black Holes and Starbursts in the Cosmic Web: Clustering and Evolution of Quasars and Submillimeter Galaxies Ryan C. Hickox1, A. D. Myers2, Bootes Survey Collaboration 1Durham University, United Kingdom, 2University of Illinois. 11:00 AM - 11:10 AM Room 618/620 The growth of massive galaxies and their central supermassive black holes is linked to the their surrounding dark matter halos, whose masses can be inferred from measurements of spatial clustering. I will present a a novel technique for deriving real-space clustering using full photometric-redshift probability distributions, and discuss a recent study using this technique to measure clustering of dust-obscured (Type 2) and unobscured (Type 1) luminous quasars. I will present a similar measurement of the clustering of submillimeter galaxies, and will place the results in context of current models for the co-evolution of quasars and rapid starbursts. Finally I will briefly point toward future observational opportunities with Herschel and the proposed Wide Field X-ray Telescope mission. RCH is funded by an STFC Postdoctoral Fellowship. 106.06 M94 As A Unique Testbed For Black Hole Mass Estimates At Low Luminosities Anca Constantin1, A. C. Seth2 1James Madison University, 2Harvard-Smithsonian Center for Astrophysics. 11:10 AM - 11:20 AM Room 618/620 The newly discovered broad Halpha emission line in the nuclear spectrum of M94, which is unambiguously associated with X-ray, radio, and variable UV compact source detections, identifies this object as one of the least luminous accretion-type LINERs discovered thus far, and therefore, an important example of accretion at extremely low levels. Its true nature remains however ambiguous, mainly because of our inability to estimate its black hole mass. We present our comparison of four independent black hole mass estimates that reveal a discrepancy of two orders of magnitude between the value predicted by the Mbh-sigma relation and the value toward which methods based on emission activity in optical, mid-IR and X-rays, converge. If M94's black hole mass obeys these three latter methods that have not been verified in the low luminosity regime exhibited by this system, we have revealed the best case for an actively accreting intermediate mass black hole. In addition, this object would clearly violate the M-sigma relation. We discuss possible resolutions of this conundrum. 106.07 Testing the Consistency of Stellar and Gas Dynamical Black Hole Mass Measurements in AGNs Jonelle Walsh1, A. J. Barth1, R. C. E. van den Bosch2, M. Sarzi3, J. C. Shields4 1University of California, Irvine, 2Max-Planck Institut für Astronomie, Germany, 3University of Hertfordshire, United Kingdom, 4Ohio University. 11:20 AM - 11:30 AM Room 618/620 NGC 3998 and NGC 4203 are two nearby S0 galaxies with LINER nuclei. The mass of the black hole in NGC 3998 has been measured previously through gas dynamical modeling of the emission-line disk using HST/STIS observations, while a gas dynamical measurement of the black hole mass in NGC 4203 is currently in progress. As both objects are also good targets for stellar dynamical modeling, they provide an excellent opportunity for the direct comparison of black hole mass measurements via the stellar and gas dynamical techniques. This necessary consistency check has so far only been attempted on a few galaxies with limited results. We will present laser guide star adaptive optics observations of NGC 3998 and NGC 4203 with the integral field spectrograph OSIRIS on the Keck II telescope. We measure high resolution stellar kinematics from the K-band CO bandheads, resolving the black hole sphere of influence. Additional large-scale observations of the stellar kinematics were taken at multiple slit positions with LRIS on the Keck I telescope and with the integral field spectrograph VIRUS-P on the 2.7m telescope at the McDonald Observatory. We will present preliminary results from the stellar dynamical modeling and constraints on the black hole masses. 107 Hydrogen Epoch of Reionization Arrays (HERA): Progress and Planning Special Session Room 611/612 107.01 Hydrogen Epoch of Reionization Arrays: Introduction Jacqueline N. Hewitt1 1MIT. 10:00 AM - 10:06 AM Room 611/612 The prospect of observing the Epoch of Reionization (EoR) that marks the end of the Dark Ages and the onset of structure formation is currently of great interest in astrophysics. The 21cm line of neutral hydrogen is a particularly promising probe. A sequence of Hydrogen Epoch of Reionization Arrays (HERA) has been proposed to provide measurements of EoR structures with increasing fidelity and depth as capability improves. The current first generation of HERA arrays is under construction or starting operation, and we can now begin to address the technical challenges of the next generation. I summarize the observational signatures targeted by the sequence of arrays, and identify some of the technical challenges. 107.02 Exploring the Dawn of Structure with the Redshifted 21 cm Signal Jonathan Pritchard1 1Harvard University. 10:06 AM - 10:15 AM Room 611/612 The first billion years of the Universe contains the formation of the first galaxies and reionization. This period lies beyond the current observational frontier presenting challenges to theory and observation. Low frequency radio observations of the redshifted 21 cm line of neutral hydrogen will be key in developing our understanding of this period. In this talk, I will describe two aspects of the 21 cm signal from the period of "cosmic dawn": the global 21 cm signal and 21 cm fluctuations. I will discuss what can be learnt about the first galaxies and reionization from this technique and explore some of the challenges and opportunities ahead for global 21 cm experiments. 107.03 Extracting The Astrophysics Of The First Sources From The 21 Cm Global Signal Jonathan R. Pritchard1, A. Loeb1 1CfA. 10:15 AM - 10:21 AM Room 611/612 Low frequency radio observations of the redshifted 21 cm line of neutral hydrogen have the potential to open a new window into the period from redshift z=6-30 when the first galaxies formed and reionization occurred. Single dipole experiments targeted at the frequency evolution of the 21 cm global signal are likely to provide the first constraints on this epoch. In this talk, I discuss the science of this signal and quantify the prospects for these instruments using a Fisher matrix based approach. I will show that there is considerable room for these simple experiments to constrain the star formation rate and production of X-ray and UV photons by the first luminous sources, provided that issues of calibration, RFI, and the ionosphere can be controlled. 107.04 The Low-Frequency Array (LOFAR) and EoR Key-Science Project Leon V. E. Koopmans1, A. G. de Bruyn2, M. Brentjens2, S. Zaroubi1 1Kapteyn Astronomical Institute, Netherlands, 2ASTRON, Netherlands. 10:21 AM - 10:32 AM Room 611/612 The Low-Frequency ARray (LOFAR) is a novel radio-telescope facility with its core and operation center in the Netherlands. LOFAR is one of several current pathfinders toward SKA. One of LOFAR's key science projects is the detection and characterization of the redshifted 21-cm emission from neutral hydrogen coming from the Epoch of Reionization and Dark Ages at redshifts beyond 6. With role-out of the core and outer stations in the Netherlands and related computational facilities nearing completion, science operations are expected to commence soon. I will present a short overview of the current status of LOFAR and that of our Epoch-of-Reionization Key Science Project. 107.05 The GMRT EoR Experience Ue-Li Pen1, T. Chang2 1CITA, Canada, 2CITA/ASIAA, Canada. 10:32 AM - 10:43 AM Room 611/612 The Giant Metrewave Radio Telescope (GMRT) Epoch of Reionization Project has been actively searching for the 21cm signal from 7.5<z<9.5. We report on the current status, lessons learned, and future initiatives. 107.06 Results from 16 and 32 Antenna PAPER Deployments Aaron Parsons1, D. C. Backer1 1UC, Berkeley. 10:43 AM - 10:54 AM Room 611/612 We present observational results from 16- and 32-antenna deployments of the Precision Array for Probing the Epoch of Reionziation (PAPER) in Green Bank, West Virginia, and the Karoo Desert of South Africa. We discuss a novel technique for accessing the 3-dimensional power spectrum of reionization using these observations, and present new constraints on the amplitude and redshift of the peak 21cm fluctuations from cosmic reionization. We go on to discuss the impacts of systematics and foregrounds on these measurements and describe our next steps going forward. 107.07 Results From MWA Miguel F. Morales1, MWA collaboration 1University of Washington. 10:54 AM - 11:05 AM Room 611/612 The Murchison Widefield Array (MWA) is a US-Australia-India low frequency observatory optimized for Epoch of Reionization measurements. This talk will review the current state of the Murchison Widefield Array and showcase results from the 32 antenna prototype. 107.08 Results From EDGES Judd D. Bowman1, A. E. E. Rogers2 1Arizona State University, 2MIT Haystack Observatory. 11:05 AM - 11:14 AM Room 611/612 The Experiment to Detect the Global Epoch of Reionization Signature (EDGES) has constrained the duration of reionization to span a redshift interval longer than dz>0.07 at 95% confidence, assuming reionization occurred between redshifts 6<z<13. The instrument measured the all-sky radio spectrum between 100 and 200 MHz with 10 mK sensitivity at the Murchison Radio-astronomy Observatory (MRO) between August and November, 2009. Rapid reionization would leave a characteristic step in the all-sky spectrum due to the disappearance of redshifted 21 cm emission from neutral hydrogen gas when it was ionized. No evidence for a sharp step was found in the observations. I will present the latest results and future plans for probing the reionization history and earlier epoch of first light in more detail with EDGES. 107.09 The Dark Ages Radio Explorer (DARE) Jack O. Burns1, J. Lazio2, J. Bowman3, R. Bradley4, C. Carilli4, S. Furlanetto5, G. Harker1, A. Loeb6, J. Pritchard7 1Univ. of Colorado at Boulder, 2JPL, 3Arizona State University, 4NRAO, 5UCLA, 6Harvard University, 7CfA. 11:14 AM - 11:20 AM Room 611/612 “What were the first objects to light up the universe, and when did they do it”? (NRC, 2011). These are among the most fundamental questions in modern astrophysics and cosmology as articulated in the recent NRC report, New Worlds, New Horizons in Astronomy and Astrophysics. The Astro2010 Decadal Survey singles out this epoch as one of the top three science objectives for the coming decade. The birth of the first stars and black holes - the end of the Dark Ages or the “Cosmic Dawn” - is one of the truly transformative events in the history of the Universe. It provides the key connection between observations of the extraordinarily smooth Universe 400,000 years after the Big Bang seen via the Cosmic Microwave Background, and telescopic images that reveal the wealth of structures and galaxies seen today. Unfortunately, this epoch has remained tantalizingly out of reach for decades and its exploration requires fundamentally new techniques. With the Dark Ages Radio Explorer (DARE), we will investigate this early epoch of the Universe (~80-350 million years after the Big Bang) for the first time using the sky-averaged, redshifted 21-cm Background (z=13-35) arising from the time when the first stars and black holes appeared in the Universe. DARE consists of a pair of tapered dipole antennas in lunar orbit operating in the shielded zone above the farside at 40-120 MHz. In this talk, we will discuss the science objectives and the instrument package for DARE. 107.10 Hydrogen Epoch of Reionization Arrays Lincoln J. Greenhill1, D. Backer2 1Harvard-Smithsonian, CfA, 2UC, Berkeley. 11:20 AM - 11:30 AM Room 611/612 Tomography of the intergalactic medium over a range of redshifts, backward through the Epoch of Reionization and into the Dark Age requires new generations of radio instruments, ones capable of detecting faint signatures of the redshifted 21 cm Hydrogen line. I will discuss the Hydrogen Epoch of Reionization Array concept (HERA), which was proposed in the Astro2010 process. A progression of larger and more scientifically capable arrays will target detection and characterization of multidimensional power spectra, and ultimately, direct imaging of discrete structures at higher and higher redshift. With the final stage corresponding to about a square kilometer of collecting area and a few kilometer geographic extent, the end-stage technical challenges will be substantial, in particular with regard to signal processing and calibration. Each step up in array size, will enable incremental deployment and demonstration of new technologies and techniques to achieve new science, starting with present-day pathfinders. At about an order magnitude larger scale, the next generation array is anticipated to be practical to build and operate at about the middle of the decade. 108 Gamma Ray Bursts Oral Session Room 4C-3 108.01D Dust Properties of Gamma Ray Burst Host Galaxies Adria C. Updike1, D. H. Hartmann1, D. A. Kann2 1Clemson University, 2Thuringer Landessternwarte Tautenburg, Germany. 10:00 AM - 10:20 AM Room 4C-3 With the intent of furthering our understanding of the dust properties of the universe as a function of redshift, we investigate the utility of using GRBs as probes of dust composition. Using the measured optical properties of graphite and silicate particles, we can reproduce the extinction observed in GRB spectral energy distributions (SEDs). The photometric SEDs of 78 GRBs with redshifts in the range 0 < z < 5 are fit according to this method, allowing us to measure the graphite and silicate column densities along the line of sight to the GRB, the visual extinction in the host frame, and, in cases where the hydrogen column density for that GRB has also been measured, the dust-to-gas ratio of the host galaxy. In addition, we present computational models of dust evolution in galaxies as a function of redshift. We compare the results of our observations to the predicted trends in the model and discuss the use of GRBs as probes of dust evolution and star formation. 108.02D The Afterglows and Host Galaxies of Dust-Obscured Gamma-Ray Bursts Daniel A. Perley1, J. S. Bloom1, S. B. Cenko1, A. J. Levan2, H. Chen3, N. R. Tanvir4 1UC, Berkeley, 2Univ. of Warwick, United Kingdom, 3U. Chicago, 4Univ. of Leicester, United Kingdom. 10:20 AM - 10:40 AM Room 4C-3 While gamma-ray bursts and their host galaxies are normally assumed (and observed) to originate from low-extinction sightlines and from blue, low-mass galaxies, both of these conclusions are subject to large selection effects as a result of the need to detect an optical afterglow to locate the host galaxy and measure the redshift. Many GRBs have exceedingly faint optical afterglows, and only since the launch of Swift have follow-up observational capabilities been able to consistently localize their positions. Evidence from observations of a uniform sample of Swift GRBs indicates that the majority of these "dark" bursts are heavily extinguished by dust in their host galaxies. New results from our five-year Keck Observatory GRB Host Survey, along with recent infrared observations from Gemini-North and the Spitzer Space Telescope, identify the host galaxies of many dark bursts to be highly infrared-luminous and dusty sources, contrasting dramatically with the hosts of GRBs selected via optical afterglow positions. This may suggest that GRBs can form at higher metallicites, and trace cosmic star-formation more closely, than previously believed. In other cases, even extremely dust-obscured bursts have hosts that are quite blue, suggesting a large hidden obscured component can exist even in apparently dust-free galaxies. 108.03 Threshold for Extended Emission in Short Gamma-Ray Bursts Jay P. Norris1, N. Gehrels2, J. D. Scargle3 1University of Denver, 2NASA/GSFC, 3NASA/ARC. 10:40 AM - 10:50 AM Room 4C-3 The initial pulse complex (IPC) in short gamma-ray bursts is sometimes accompanied by a softer, low-intensity extended emission (EE) component. In cases where such a component is not observed, it has not been clear if it is present but below detection threshold. Using Bayesian Block methods, we have measured the EE component and shown that it is present in one quarter of a Swift/BAT sample of 51 short bursts. We simulated bursts with EE to calibrate the BAT threshold for EE detection. The EE component would have been detected in nearly half of BAT short bursts if it were present, to intensities ~ 10-2 counts cm-2 s-1, a factor of five lower than actually observed in the bursts with EE. The 2-sigma upper on the ratio, Rint = average EE intensity to IPC peak intensity, for the average of those 39 bursts without an EE component, is Rint < 8 x 10-4. Our results (ApJ, 717, 2010) suggest that a physical threshold mechanism operates near Rint ~ few x 10-3 - below which the EE component is not manifest - but do not necessarily favor two different progenitors for short bursts. 108.04 GRB 081029: A Step Towards Understanding Multiple Afterglow Components Stephen Holland1, M. De Pasquale2, J. Mao3, T. Sakamoto4, P. Schade5, S. Covino3, P. D'Avanzo3, A. Antonelli6, V. D'Elia7, G. Chincarini3, F. Fiore7 1CRESST/USRA/NASA/GSFC, 2MSSL, United Kingdom, 3INAF-OAB, Italy, 4NASA/GSFC, 5Max Planck Institute, Germany, 6INAF-RAO, Italy, 7INAF-OAR, Italy. 10:50 AM - 11:00 AM Room 4C-3 We present an analysis of the unusual optical light curve of the gamma-ray burst GRB 081029 at a redshift of z = 3.8479. We combine X-ray and optical observations from Swift with optical and infrared data from REM to obtain a detailed data set extending from ? 0.1 ks to ? 100 ks after the BAT trigger, and from 10 keV to 1600 nm. The X-ray afterglow showed a shallow initial decay followed by a rapid decay after about 18 ks. The optical afterglow, however, shows an uncharacteristic rise at about 5 ks that has no corresponding feature in the X-ray light curve. The data are not consistent with a single-component jet. It is possible that there are multiple physical components contributing to the afterglow of GRB 081029. 108.05D In Search for a Relation with Physical Origin for GRBs Razieh Behkam1 1Arizona State University. 11:00 AM - 11:20 AM Room 4C-3 Gamma-ray burst observations provide a great opportunity for cosmography in high redshift. Some tight GRB correlations are already known. The relations with physical origin will have a better potential to utilize GRBs for cosmography. Ryde (2004) showed that the prompt emission spectrum is interpreted as composition of a thermal component in addition to the non-thermal one. We show here that analysing the thermal component of the GRB prompt emission leads us to a well-correlated relation. We also perform monte carlo test and show that this correlation is acceptably insensitive to our assumptions. Our correlation looks similar to Ghilanda's in quality, and provides some physical insights to Ghirlanda's relation. 108.06 Nova V407 Cygni 2010: First Detection of GeV Gamma-rays from a Nova Kent S. Wood1, C. C. Cheung2, A. B. Hill3, P. Jean4, S. Razzaque2 1NRL, 2NRC/NRL, 3LAOG, France, 4CESR, France. 11:20 AM - 11:30 AM Room 4C-3 We report the Fermi-LAT discovery of variable >100 MeV gamma-ray emission from the optical nova of the symbiotic star V407 Cygni in March 2010, the first detection of gamma-rays in the GeV band from any nova. The spectrum and light curve of the gamma-ray emission can be understood broadly as consequences of shock acceleration in the nova shell as it interacts with the dense ambient medium of the red giant companion. Viable gamma-ray production mechanisms via pi-0 decay from proton-proton interactions and inverse Compton scattering of the radiation from the red giant are outlined. 109 Galaxy Clusters: Intracluster Medium and Cluster Masses Oral Session Room 609 109.01 Cluster Mass Profiles from the Hectospec Cluster Survey (HeCS) Kenneth J. Rines1, M. J. Geller2, A. Diaferio3 1Western Washington University, 2Smithsonian Astrophysical Observatory, 3Universita di Torino; INFN, Italy. 10:00 AM - 10:10 AM Room 609 The Hectospec Cluster Survey (HeCS) is a spectroscopic survey of a flux-limited sample of X-ray-selected galaxy clusters at 0.10.8. The apparent tension between ?8 from primary CMB power and from analytic SZ spectra inferred using ACT and SPT data is lessened with our AGN feedback. 109.04D The Physical Origin of Intrinsic Scatter in the Cluster X-ray and SZ Scaling Relations Hsiang-Yi Yang1, P. Ricker1, S. Bhattacharya2, P. Sutter1 1University of Illinois at Urbana-Champaign, 2Los Alamos National Laboratory. 10:50 AM - 11:10 AM Room 609 Clusters of galaxies are invaluable cosmological probes, but systematic biases and the form and evolution of scatter in the mass-observable relations need to be understood to obtain accurate mass estimates. We use N-body plus hydrodynamic simulations including different physical processes to study the impact of halo concentration, dynamical state, radiative cooling and AGN feedback on scatter in the X-ray temperature-mass and the SZ flux-mass (Y-M) scaling relations. We find that the variation in concentration is a significant source of scatter in both relations, which can be used to tighten the relations for better mass estimates. Contrary to intuition, the effect of dynamical state is statistically negligible. Due to the sensitivity of the SZ effect to cluster morphology and projection effect, we find that the Y-M scatter has positive skewness and kurtosis to a degree that can bias cosmological constraints assuming lognormality. Fortunately, because the errors in the SZ and X-ray relations are not correlated, cross-calibrations of cluster masses can be effective in identifying the outliers due to projection errors. The influence of additional gas physics in cluster cores such as radiative cooling and AGN feedback is also discussed. 109.05 More Powerful than a Speeding "Bullet"? New HST Images and Analysis of the Galaxy Cluster Merger Abell 2744 Dan A. Coe1, R. Dupke2, N. Benitez3, T. Broadhurst4, R. Massey5, A. Zitrin6, J. Merten7, E. Cypriano8, F. Braglia9, B. Frye10, M. Meneghetti11, L. Moustakas12, J. Rhodes12, J. Krick13, L. Sodre8, J. Bregman2, Y. Jimenez-Teja3, R. Bernstein14 1STScI, 2U Michigan, 3IAA, Spain, 4UPV/EHU, Spain, 5Edinburgh, United Kingdom, 6Tel Aviv, Israel, 7Heidelberg, Germany, 8Sao Paolo, Brazil, 9UBC, Canada, 10USF, 11INAF, Italy, 12JPL, 13SSC, 14Santa Cruz. 11:10 AM - 11:20 AM Room 609 Abell 2744 is a galaxy cluster merger similar to the Bullet Cluster but more massive and somewhat more complex. A2744 exhibits an even larger (the largest observed) projected separation between dark matter and the stripped, shocked cluster gas (~54" ~240 kpc). We may even be witnessing a triple merger similar to "The Cosmic Train Wreck" (Abell 520) as evidenced in part by Chandra X-ray observations which reveal high temperature shock regions (as high as 15 keV) and a complicated structure. We have obtained new deep (16 orbit), multiband (BVI) HST/ACS images of A2744's core. These images reveal in detail several prominent strong gravitational lensing features due to the SE subcluster, and our lens modeling reveals many more (~30 total). Here we present these images and new "non-parametric" mass models of A2744 based on simultaneous fitting to strong + weak lensing data in the HST and ground-based images. We discuss the relative positions of the dark matter peaks, galaxies, and gas peaks and implications for limits on the self-interaction cross section of dark matter particles. 109.06 Resurrecting The Red From The Dead: Optical Properties Of BCGs In X-ray Luminous Clusters Chris Bildfell1, H. Hoekstra2, A. Babul1, A. Mahdavi3 1University of Victoria, Canada, 2Leiden Observatory, Netherlands, 3San Francisco State University. 11:20 AM - 11:30 AM Room 609 Brightest Cluster Galaxies (BCG) reside deep inside luminous X-ray clusters and represent the most massive end of the galaxy mass function. As such they offer a unique perspective on current problems in both galaxy formation and cluster gas physics. Baryonic feedback processes like AGN and star formation along with radiative cooling are believed to be responsible for the scatter in X-ray cluster scaling relations and should also leave observable signatures in the BCG properties. A detailed study of BCGs can allow one to probe the interaction and relative importance of these critical baryonic processes. We present measurements of surface brightness and colour profiles for the BCGs in a sample of 48 X-ray luminous galaxy clusters. These data were obtained as part of the Canadian Cluster Comparison Project (CCCP). We find that while most BCGs show monotonic colour gradients consistent with a decrease in metallicity with radius, 25% show colour profiles that turn bluer towards the centre (blue cores). We interpret this bluing trend as evidence for recent star formation. The excess blue light leads to a typical offset from the red sequence of 0.5 to 1.0mag in (g' - r'), thus affecting optical cluster studies that may reject the BCG based on colour. All of the blue-core BCGs are located within ~10kpc of the peak in the cluster X-ray emission. Furthermore, virtually all of the BCGs with recent star formation are in clusters that lie above the Lx-Tx relation. Based on photometry alone, these findings suggest that central star formation is a ubiquitous feature of BCGs in dynamically relaxed cool-core clusters. This implies that while AGNs and other heating mechanisms are effective at tempering cooling, they do not full compensate for the energy lost via radiation. This research was funded in part by NSERC. 110 Strategies for Addressing Harassment and Prejudice Special Session Room 4C-4 110.01 Building Respect and Inclusion in Astronomy - Strategies for Understanding and Overcoming Harassment. Sheryl Bruff1 1Space Telescope Science Institute. 10:00 AM - 10:45 AM Room 4C-4 Building a respectful and inclusive workplace, whether in universities, research centers, governmental agencies, etc., is critical to the production of great scientific work. Behaviors that divide or exclude, such as harassment, bias or prejudice, diminish our ability to fully gain the value of scientific intellect and creativity. Harassing, biased and intolerable conditions can arise in a variety of interpersonal situations - working relationships, collegial partnerships, academic study, etc., where clear expectations and boundaries are not identified and established and/or where situational power and control are not managed appropriately. Historically, situations have often been ignored and/or rationalized rather than addressed simply because the perpetrator “did not mean it” or did not realize the impact of his/her behavior. Victims frequently suffered in silence out of rationalization or fear of reprisal. Identifying and addressing harassing behaviors in the workplace has become more complex and expansive over the past few decades. In today’s workplace, these behaviors are defined more by outcome than by intent. It is critical that all individuals understand what behaviors fall into these classifications and what to do when confronted by these behaviors. This session will focus on understanding: •what is meant by harassment and prejudice •what prohibited behaviors fall into these categories •how to respond and protect yourself •remedies and protections afforded by laws, policies and programs •what to expect from your organization. Scenarios from real life circumstances and options for responding to harassing situations will be presented for discussion and review. 110.02 What to do about Inappropriate Behavior Bernice Durand1 1University of Wisconsin. 10:45 AM - 11:30 AM Room 4C-4 If you believe you are a victim of harassment, bias, or prejudice, your first need is to know what person you should confide in who would be qualified to help you understand and go through the process of resolving your difficult situation. You will be best off if you have an accessible, trustworthy institutional infrastructure in place for dealing with inappropriate behavior. The exact nature of the infrastructure varies among institutions; but it starts with leadership from the top person in every unit, for example the university president, the dean, the department chair, and the research group leader. A good “safety net” structure also includes a reliable system for reporting and addressing problems before they escalate; an institutional “enforcer” who is widely known to mean business; and trainings and frequent publicity about the consequences of such behavior. The components of a good structure, as well as some alternative routes to take if you don’t have such a system, will be described in the contexts of different types of institutions; and you will learn the criteria for prohibited behaviors. There will be time for analysis and discussion of scenarios taken from real incidents, altered to protect privacy. 111 HAD IV History of Astronomy Oral Session Room 613/614 111.01 Report of Some Comets: The Discovery of Uranus and Comets by William, Caroline, and John Herschel Jay M. Pasachoff1, R. J. M. Olson2 1Williams College and Caltech, 2New-York Historical Society. 10:00 AM - 10:15 AM Room 613/614 We report on the discovery and drawings of comets by William, Caroline, and John Herschel. The first discovery, by William Herschel, in 1781 from Bath, published in the Philosophical Transactions of the Royal Society with the title "Report of a Comet," turned out to be Uranus, the first planet ever discovered, Mercury through Saturn having been known since antiquity. William's sister Caroline was given duties of sweeping the skies and turned out to be a discoverer of 8 comets in her own right, in addition to keeping William's notes. Caroline's comets were discovered from Slough between 1786 and 1797. In the process, we also discuss original documents from the archives of the Royal Society and of the Royal Astronomical Society. We conclude by showing comet drawings that we have recently attributed to John Herschel, including Halley's Comet from 1836, recently located in the Ransom Center of the University of Texas at Austin. Acknowledgments: Planetary astronomy at Williams College is supported in part by grant NNX08AO50G from NASA Planetary Astronomy. We thank Peter Hingley of the Royal Astronomical Society and Richard Oram of the Harry Ransom Center of The University of Texas at Austin for their assistance. 111.02 The Herschels in Canada Peter Broughton1 1Royal Astronomical Society of Canada, Canada. 10:15 AM - 10:30 AM Room 613/614 William Herschel, the father of the astronomical dynasty, may possibly have lived in Canada. A couple of his descendants certainly did, and their lives and contributions to astronomy will be briefly discussed. Furthermore, some geographic features in Canada commemorate the Herschel name. Where these landmarks are and how they came to have this distinction will be described. 111.03 King Charles` Star: A Multidisciplinary Approach To Dating The Supernova Known As Cassiopeia A Martin Lunn1, L. Rakoczy1 1Yorkshire Museum, United Kingdom. 10:30 AM - 10:45 AM Room 613/614 Few astronomical phenomena have been as studied as the supernova known as Cassiopeia A. Widely believed to have occurred in the latter half of the seventeenth century, it is also thought to have gone unrecorded. This paper will argue that Cas A did not go unobserved, but in fact was seen in Britain on May 29, 1630, and coincided with the birth of the future King Charles II of Great Britain. This ‘noon-day star’ is an important feature of Stuart/Restoration propaganda, the significance of which has been widely acknowledged by historians and literary experts. The argument here, however, is that in addition the historical accounts provide credible evidence for a genuine astronomical event, the nature of which must be explained. Combining documentary analysis with an overview of the current scientific thinking on dating supernova, the authors put forward their case for why Charles’ star should be recognized as a sighting of Cas A. Finally, it will be argued that a collaborative approach between the humanities and the sciences can be a valuable tool, not just in furthering our understanding of Cas A, but in the dating of supernovae in general. 111.04 The "Three York Astronomers" and the Royal Society of London Linda M. French1 1Illinois Wesleyan Univ.. 10:45 AM - 11:00 AM Room 613/614 John Goodricke, the discoverer of the periodicity of Algol and Delta Cephei; his mentor and collaborator Edward Pigott; and Edward’s father Nathaniel Pigott flourished in York, England in the 1780’s. All three made substantial contributions to astronomy. Nathaniel and Edward had determined the longitudes of the principal cities of the Low Countries before moving to York. Edward worked closely with Goodricke on the observations of Algol and discovered the variability of Eta Aquilae, a Cepheid, before Goodricke discovered Delta Cephei’s behavior. All three corresponded with members of the Royal Society, including Nevil Maskelyne and William Herschel, yet the treatment accorded them differed widely. Nathaniel Pigott was elected a member of the Society in 1772. Goodricke received the Society’s Copley Medal for his paper on the periodicity of Algol in 1783 at the age of nineteen. In 1786, after being nominated by Nathaniel Pigott, Goodricke was elected to membership in the Royal Society. Edward Pigott was apparently never nominated. Some possible reasons why Goodricke was lionized and Edward Pigott passed over will be explored. This research was supported by an AAS Small Research Grant and by the Herbert C. Pollack Award of the Dudley Observatory. 111.05 The Historical 'Science Driver': Early Telescopes and Scientific Incentive. Peter Abrahams1 1Historical Astronomy Division. 11:00 AM - 11:15 AM Room 613/614 The term 'science driver' was first used in the 1980s. The modern meaning of 'science' is far removed from its meaning in the first centuries of the telescope. It is anachronistic to refer to the 'science driver' of a historic telescope. However, there were scientific motivations behind many early telescopes, large reflectors in particular. The chronology of larger and improved telescopes will be placed in the context of the rationale for their creation. The evolution of scientific purpose of these instruments will be extracted and examined for patterns and significance. 111.06 Blind Astronomers Thomas A. Hockey1 1University of Northern Iowa. 11:15 AM - 11:30 AM Room 613/614 The phrase “blind astronomer” is used as an allegorical oxymoron. However, there were and are blind astronomers. What of famous blind astronomers? First, it must be stated that these astronomers were not martyrs to their craft. It is a myth that astronomers blind themselves by observing the Sun. As early as France’s William of Saint-Cloud (circa 1290) astronomers knew that staring at the Sun was ill-advised and avoided it. Galileo Galilei did not invent the astronomical telescope and then proceed to blind himself with one. Galileo observed the Sun near sunrise and sunset or through projection. More than two decades later he became blind, as many septuagenarians do, unrelated to their profession. Even Isaac Newton temporarily blinded himself, staring at the reflection of the Sun when he was a twentysomething. But permanent Sun-induced blindness? No, it did not happen. For instance, it was a stroke that left Scotland’s James Gregory (1638-1675) blind. (You will remember the Gregorian telescope.) However, he died days later. Thus, blindness little interfered with his occupation. English Abbot Richard of Wallingford (circa 1291 - circa 1335) wrote astronomical works and designed astronomical instruments. He was also blind in one eye. Yet as he further suffered from leprosy, his blindness seems the lesser of Richard’s maladies. Perhaps the most famous professionally active, blind astronomer (or almost blind astronomer) is Dominique-Francois Arago (1786-1853), director until his death of the powerful nineteenth-century Paris Observatory. I will share other _ some poignant _ examples such as: William Campbell, whose blindness drove him to suicide; Leonhard Euler, astronomy’s Beethoven, who did nearly half of his life’s work while almost totally blind; and Edwin Frost, who "observed” a total solar eclipse while completely sightless. 112 Interstellar Medium: Dust Particles and Emission Oral Session Room 608 112.01 An Approach To Investigating Dust Properties In Galaxies Through Simulations Of Extinction Of Sne Ia Spectra Susana E. Deustua1, A. Cikota2, K. Gordon1 1Space Telescope Science Institute, 2University of Zurich, Switzerland. 10:00 AM - 10:10 AM Room 608 Because they are so bright, Type Ia Supernovae (SNeIa) are probably the most accurate distance indicators on cosmological scales. And, although SNeIa are not equally bright, they are standardizable candles through the known correlation between their peak brightness and the width of their light curves. However, the correlation fails for some SNeIa which can appear dimmer and redder either because of host galaxy dust extinction or perhaps due to intrinsic properties. We have undertaken a study to examine the effects of dust on SNe Ia observations, including investigating possible differences between the dust properties in galaxies, both nearby and at high redshifts. One of our goals with this study is to investigate the uncertainties on SN Ia extinction values using multicolor data of nearby galaxies. We have taken advantage of The Spitzer Infrared Nearby Galaxies Survey (SINGS), a comprehensive study of 75 nearby galaxies (Kennicutt et al. 2003) with good estimates of their dust masses (Draine et al. 2007). We combine this date with SNe Ia templates to bound the effects of extinction. To investigate high redshift galaxy dust properties in high-z galaxies we compare the simulated spectra to the PHASE extracted data set of 139 spectra of 124 Type Ia supernovae obtained at the VLT during the first three years of the CFHT Supernova Legacy Survey (Balland et al). We discuss the methods used in our simulations and the significance of the results of this study based on comparing computed extinction for template spectra to published observational data of low and high redshift SNe Ia. 112.02D Dust Formation and Evolution in Core Collapse Supernovae Jennifer E. Andrews1 1Louisiana State University. 10:10 AM - 10:30 AM Room 608 Detection of large amounts of dust in high redshift galaxies suggest that core collapse supernovae (CCSNe) may play an important role in the dust budget of the universe. At an age of only 1Gyr, there has not been enough time for low-mass stars to form and evolve to the asymptotic giant branch, but there has been sufficient time for CCSNe, which quickly evolve and return their material to the surrounding interstellar medium. For the past three years, I have been following the Type IIP SNe 2007it and 2007od with Gemini, HST, and Spitzer to look for indicators of dust formation, which appear within the first few years of discovery. The data obtained have significant temporal and wavelength coverage, and the SNe show unusual and interesting characteristics. In both cases we are seeing evidence of CSM interaction in their spectral evolution, although neither was initially classified as a Type IIn. We found SN 2007it to be oxygen rich with 56Ni masses quite large for a Type IIP, while SN 2007od is oxygen poor with a very low 56Ni mass. Light echoes also seem to be present in both SNe. We estimate ~10-4 Msun of dust has formed in each SN, consistent with other CCSNe, but still smaller than needed to account for the amount of dust seen at high redshift. This work has been supported by NSF grant AST-0707691 and NASA GSRP grant NNX08AV36H. This work was supported by Spitzer Space Telescope RSA 1415602 and RSA 1346842, both issued by JPL/Caltech. 112.03 Star Formation Rates From 8 Micron PAH Emission: Quantifying The Contamination From Old Star Excitation Alison Faye Crocker1, D. Calzetti1, D. A. Thilker2, KINGFISH Team 1UMass Amherst, 2Johns Hopkins University. 10:30 AM - 10:40 AM Room 608 Dust emission in the mid-infrared (MIR), mainly from polycyclic aromatic hydrocarbons (PAHs), is used as a star formation rate tracer at both low and high-redshifts. However, PAHs can be excited not only by young UV-emitting stars, but also by the softer radiation field of older stars. Yet no study quantifying the fraction and spatial distribution of this 'diffuse' MIR component has been performed. To do this, we compare the Spitzer 8 micron emission (stellar subtracted) to the distribution of the H? recombination line in a sample of SINGS spiral galaxies. Dust-corrected H? emission accurately traces star formation as only hot young stars can produce the required ionizing continuum (outside of the immediate environs of an AGN or strong shocks). The 8 micron and H? images show qualitative differences, with the H? appearing much more limited to clumpy HII regions and the 8 micron having a smoother appearance (after convolution to the same resolution). Considering only diffuse regions (i.e. ignoring HIIphot-identified HII regions), we see that the diffuse/total 8 micron emission ratio is significantly greater than the diffuse/total H? emission ratio. This difference implies that some of the PAH excitation in normal star-forming spiral galaxies is due to older stars (20% in the first galaxy analyzed, NGC 628). Applying identical techniques to the good-resolution FIR Herschel data on a similar sample of galaxies will provide an estimate of the FIR dust emission attributable to diffuse heating. 112.04 Observations of strong Diffuse Interstellar Bands in M31 and M33 Martin Cordiner1, N. L. J. Cox2, K. T. Smith3, C. J. Evans4 1NASA Goddard Space Flight Center, 2Institute for Astronomy, K.U. Leuven, Belgium, 3School of Chemistry, The University of Nottingham, United Kingdom, 4UK ATC, Royal Observatory Edinburgh, United Kingdom. 10:40 AM - 10:50 AM Room 608 We report the first detections of diffuse interstellar bands (DIBs) in absorption towards early-type supergiant stars in the Local Group spiral galaxies M 31 and M 33. The ??4430, 5705, 5780, 5797, 6203, 6269, 6283, 6379 and 6613 DIBs are detected at radial velocities matching the blue-shifted M 31 and M 33 Na I absorption lines. The overall spectrum of DIBs and the ratios of strengths between the different M 31 and M 33 DIBs are found to be similar to those typically observed in the Milky Way. These results are discussed in the context of the different interstellar physical and chemical conditions of these galaxies compared with the Milky Way, including the metallicity, the interstellar radiation field, the dust extinction properties and the PAH abundances. Some of the M 31 and M 33 DIB equivalent widths are found to be exceptionally large per unit reddening (E(B-V)) compared with those typically observed in the Galaxy. These results indicate that conditions in M 31 and M 33 are favourable for the production of the large organic molecules that are believed to be the carriers of at least some of the DIBs. A negative correlation is found in M 31 between the DIB strengths and the strength of the interstellar NUV radiation field, which suggests that the DIB carriers and/or their chemical precursors are destroyed by NUV radiation. This work has been funded by the NASA Institute for Astrobiology, the Faculty of the European Space Astronomy Centre (ESAC), Queen's University Belfast, and the UK Engineering and Physical Sciences Research Council (EPSRC). 112.05 The Importance of Aluminum in Silicate Glasses Arielle L. Newgard1, A. Speck1, A. Whittington1, A. Hofmeister2, J. Tartar1 1University of Missouri - Columbia, 2Washington University. 10:50 AM - 11:00 AM Room 608 It is well known that silicate dust plays an important role in many astrophysical environments with an emphasis in the literature on olivines and pyroxenes due to their lower condensation temperature. However these two types of silicates tend to be Al-free and it would be remiss to exclude the role of Al from silicate dust. For example, Al is seen in CAI (Ca-Al inclusions) in primitive meteorites and the Al is the fourth most abundant metal after Si, Mg, and Fe. However, we expand upon the currently presented knowledge of the role of Al in silicate dust by looking more closely at the structure (polymerization) represented in NBO/T ratio (Non-bridging oxygens to SiO4 tetrahedra). We present a sample of silicates of known Al abundance and discuss how the Al affects these samples both physically and spectrally. Potential applications of these data are also discussed. 112.06 UV-Visible Laboratory Spectra Of Dust Analogs: Mg-silicates, Spinel, And Glasses Karly M. Pitman1, A. M. Hofmeister2, A. K. Speck3 1Planetary Science Institute, 2Washington University - St. Louis, 3University of Missouri - Columbia. 11:00 AM - 11:10 AM Room 608 There is a great need for UV-vis data to analyze many astronomical environments but past laboratory analog spectra in the UV-vis are insufficient to reliably determine the composition and structure of dust from astronomical observations and models. To address this need, we will present the spectral behavior of selected silicates, silicate glasses, and an oxide that may be present in space over the mid-UV to HST wavelength range ? =190-1100 nm. Priority compounds for this study are the Mg-rich crystalline silicates (forsterite Mg2SiO4; enstatite Mg2Si2O6) that are predicted in abundance models and found in multiple objects (e.g., AGB stars, PNe, YSOs, comets, ultraluminous IR galaxies, O-rich stellar outflows, ?-Pic, Herbig Ae/Be stars). We will also present new UV-vis data for the oxide spinel (MgAl2O4), relevant to presolar grains, chondritic meteorites, AGB, and SN. Finally, we will present UV lab data on silicate glasses to connect to complementary IR silicate glass data and assist in testing the hypothesis that the majority of interstellar dust in our own galaxy was formed in dark molecular clouds, rather than the outflows of evolved stars. By determining the UV properties of both crystalline and glassy silicates, we may be able to distinguish whether the ISM silicate is truly glass, and thus determine whether ISM dust is formed in situ. This work is supported through NSF AST-1009544. 112.07 The Alignment of Dust Grains With the Magnetic Field in Dense Regions of Taurus Nicholas L. Chapman1, P. Goldsmith2, D. Li2, D. Clemens3 1Northwestern University, 2Jet Propulsion Laboratory, 3Boston University. 11:10 AM - 11:20 AM Room 608 We present maps of the plane-of-sky magnetic field within two regions of the Taurus molecular cloud: one in the dense core L1495 and the other in a diffuse region for comparison. The field direction is measured from the polarization of background starlight seen through the cloud. Because our data are at near-infrared wavelengths, we are able to measure the polarization even in the densest portion of L1495. In this region, we find that the percentage polarization increases with column density, suggesting that the dust grains are aligned with the magnetic field to some significant depth in the cloud rather than grain alignment being confined to a thin surface layer. This is in contrast to some previous results in Taurus and other regions, but is consistent with a more recent analysis that showed that grain alignment by means of radiative torques could explain a correlation between polarization percentage and column density. This work was supported by the Jet Propulsion Laboratory, California Institute of Technology and NSF grant AST-090930. 112.08 Hi-GAL Observations: Emissivity Spectral Index along the Galactic Plane Marcella Veneziani1, D. Paradis1 1SSC-Caltech. 11:20 AM - 11:30 AM Room 608 Variations in the dust emissivity are critical for gas mass determination derived from far-infrared observations, but also for separating dust foreground emission from the Cosmic Microwave Background. Hi-GAL observations allow for the first time to study dust emissivity variations in the inner regions of the Galactic plane. We present emissivity spectral index maps derived from the Herschel PACS 160 and SPIRE 250, 350 and 500 micron data combined to the IRIS 100 micron data, and we analyze the spatial variations of the spectral index as a function of dust temperature and wavelength in the two Science Demonstration Phase Hi-GAL fields, centered at l=30deg and l=59deg. Applying two different methods, we determine both dust temperature and emissivity spectral index between 100 and 500 micron, at an angular resolution of 4 arcmin. Combining both fields, the results evidence variations of the emissivity spectral index in the range 1.8-2.6 for temperatures between 14 and 23 K. The median values of the spectral index are identical in both fields, i.e. 2.3 in the range 100-500 micron, for median dust temperature equal to 19.1 K and 16.0 K in the l=30deg and l=59deg field, respectively. Statistically, we do not see in the emissivity spectra any significant deviations from a power law between 100 and 500 micron. We show an inverse correlation between the emissivity spectral index and the dust temperature, found in previous analysis in various environments. 113 YSOs, Etc. I Oral Session Room 604 113.01 Fragmentation Of Cold Atlasgal Dust Clumps Jagadheep D. Pandian1, T. Troost2, F. Wyrowski2, J. P. Williams1, F. Schuller2, K. M. Menten2 1Institute for Astronomy, 2Max Planck Institute for Radio Astronomy, Germany. 10:00 AM - 10:10 AM Room 604 The APEX Telescope Large Area Survey of the Galaxy (ATLASGAL) has revealed a large sample of dust continuum sources that are potential sites of high-mass star/cluster formation. This dataset, when combined with 70 and 24 micron data from the Spitzer MIPSGAL survey allows identification of sources at the earliest phases of star formation. One of the open questions in high-mass star formation is the nature of fragmentation in early evolutionary phases. To address this question, we have observed a sample of high-mass ATLASGAL sources that have no counterpart at 70 micron or 24 micron in MIPSGAL, at 345 GHz using the SMA in its compact configuration. The sources are chosen to have kinematic distances less than ~ 5 kpc, and consequently our observations probe scales down to 0.1 pc. We present initial results of this work and discuss the mass assembly from large scale dust clumps to small scale cores. 113.02 VLA Ammonia Observations of IRAS 16253-2429: A Very Young and Low Mass Protostellar System Jennifer J. Wiseman1, M. Barsony2, R. Sahai3 1NASA / GSFC, 2Space Science Institute, 3NASA Jet Propulsion Laboratory. 10:10 AM - 10:20 AM Room 604 IRAS 16253-2429, the source of the Wasp-Waist Nebula seen in Spitzer IRAC images, is an isolated, very low luminosity (“VeLLO”) Class 0 protostar in the nearby rho Ophiuchi cloud. We present VLA ammonia mapping observations of the dense gas envelope feeding the central core accreting system. We find a flattened envelope perpendicular to the outflow axis, and gas cavities that appear to cradle the outflow lobes as though carved out by the flow and associated (apparently precessing) jet. Based on the NH3 (1,1) and (2,2) emission distribution, we derive the mass, velocity fields and temperature distribution for the envelope. We discuss the combined evidence for this source as possibly one of the youngest and lowest mass sources in formation yet known. 113.03D The Search For Pulsation In Young Low-mass Stars And Brown Dwarfs: A High-precision Photometric Census Of Variability At 3-5 Myr Ann Marie Cody1, L. Hillenbrand1 1Caltech. 10:20 AM - 10:40 AM Room 604 In 2005, Palla & Baraffe proposed that brown dwarfs and very low mass stars (<0.1 solar masses) may be unstable to radial oscillations during the pre-main-sequence deuterium burning phase. With associated oscillation periods of 1-4 hours, this potentially new class of pulsation offers unprecedented opportunities to probe the interiors and evolution of low-mass objects in the 1-15 My age range. Furthermore, several previous reports of short-period variability have suggested that deuterium-burning pulsation is in fact at work in young clusters. As part of my dissertation, I developed a photometric monitoring campaign to search for low-amplitude periodic variability in young brown dwarfs and very low mass stars. I will discuss the details of high-precision, high-cadence time series photometry in four young clusters, using meter-class telescopes from both the ground and space. The survey achieves sensitivity to periodic oscillations with photometric amplitudes down to several millimagnitudes. I will present the census of variability on timescales ranging from minutes to days in a sample of ~100 young, low-mass cluster members. While I find a dearth of photometric periods under 10 hours, the campaign's high time resolution and precision have enabled detailed study of diverse light curve behavior in the clusters: rotational spot modulation, accretion signatures, and occultations by surrounding disk material. Analysis of our data has led to the establishment of a lower limit for the time scale of photometry variability in young low-mass and substellar objects, an extension of the rotation period distribution to the brown dwarf regime, as well as a new study on the connection between variability and circumstellar disks in the Sigma Orionis cluster. 113.04 Using Spitzer IRS Spectroscopy to Characterize the Massive Young Stellar Objects in the G333 Massive Star Forming Region Janet P. Simpson1, A. S. Cotera1, I. Bains2, M. G. Burton3, M. Cunningham3, N. Lo4 1SETI Institute, 2Swinburne University, Australia, 3University of New South Wales, Australia, 4University of Chile, Chile. 10:40 AM - 10:50 AM Room 604 Mid-infrared spectroscopy provides unique and crucial information that can be used to characterize massive young stellar objects (MYSOs) and resolve questions regarding the evolutionary states of these objects. We have used the Spitzer Space Telescope Infrared Spectrograph in the Short-Low, Short-High, and Long-High modules (5-36 micron) to map the thirteen very red sources that we found in Spitzer IRAC (GLIMPSE) and MIPS (MIPSGAL) images of the G333 giant molecular cloud. The objects, which have luminosities ranging from ~2X103 Lsun to ~5X104 Lsun, are divided into two groups: seven MYSOs associated with extended emission in IRAC band 2 at 4.5 micron ("outflow sources", also known as "EGOs" or "green fuzzies") and six MYSOs that have extended emission in all IRAC bands peaking at the longest wavelengths ("red sources"). All the YSOs associated with outflows show evidence of massive envelopes surrounding the star, which produce deep silicate absorption features and absorption by ices at 6.0, 6.8, and 15.2 micron. There is shocked gas associated with the 4.5 micron emission, as seen by the presence of [S I] 25 micron line emission in over half of the outflows (but not by any associated H2 line emission, as has been suggested elsewhere). For four of the red sources, our spectral maps show that there are ionized neon and sulfur lines concentrated to the YSO locations, from which we infer that these red YSOs can already ionize H II regions. For several objects of both types, the lines from the highly excited Ne++ ions peak at some distance from the peak of the low excitation lines. We conclude that both types of MYSO have outflows that produce shocked gas and that the outflow MYSOs, which have slightly cooler spectral energy distributions than the red YSOs, are younger than the H II region producing, red MYSOs. 113.05 A High-resolution Study of the Spectrum of HD 190073 (V1295 Aql) Charles R. Cowley1, S. Hubrig2 1Univ. of Michigan, 2Astrophysikalisches Institut Potsdam, Germany. 10:50 AM - 11:00 AM Room 604 Detailed abundance work on Herbig Ae stars began in the last decade. Acke and Waelkens's (A&A, 427, 1009, 2004, henceforth AW) study is exemplary. We report results for HD 190073 (V1295 Aql), based on significantly better spectroscopic material: 8 averaged HARPS spectra from the ESO archive (RP=110,000, Fourier-filtered, S/N 200-350). There is significant line emission, not only in the Balmer cores, but also in myriad metal lines. We assume with AW that abundances may be derived from equivalent widths of lines not involved with emission, taken to belong to a photosphere not badly deviant from models. We confirm AW for HD 190073, in that consistent results may be obtained from two stages of ionization of several elements, and internal excitations within an ionization stage. We adopt Teff=9100K, and log(g)=3.0, slightly different from AW's 9250K and log(g)=3.5. The adopted parameters give fits to the wings of the Balmer lines. We find no indication of anomalous saturation found for HD 101412 (A&A, in press, arXiv:1008.1601), in spite of the far more prominent emission of HD 190073. The latter star is more massive, and younger, and probably observed nearly pole on. The iron abundance is closely solar, but we find a larger nitrogen excess than AW, +0.8 dex. Sodium is in excess by the same amount, while zinc is overabundant by 0.3 dex. The emission-line spectrum was described recently by Catala, et al. (A&A, 462, 293, 1967). We model the region as a hot slab above an approximate stellar photosphere. Metallic emission below the Balmer jump is often optically thick, while the line centers rarely approach unit optical depth above it. 113.06 Constraining the Size of the Solar Nebula Katherine A. Kretke1, H. F. Levison1 1Southwest Research Institute. 11:00 AM - 11:10 AM Room 604 Observations indicate that the circumstellar gaseous disks around young stars vary significantly in size, ranging from 10s to 1000s of AU. As we try to unravel the events leading to the formation of our own solar system, we would like to understand the properties of our own primordial disk. Fortunately, the dynamics of objects in the Kuiper belt provide interesting constraints. After Jupiter formed, it must have scattered a significant number of planetesimals into eccentric orbits. If there had been a massive, extended protoplanetary disk at that time, then the disk would have excited Kozai oscillations in the scattered objects, driving some into high-inclination, low-eccentricity orbits. The dissipation of the gaseous disk would strand some objects in these high-inclination orbits; orbits that are stable on Gyr timescales. The fact that we have yet to observe Kuiper belt objects on these orbits therefore places a strict limits size of the disk at the time of planet formation, revealing important information about the environment from which our solar system emerged. 113.07 The Evolution Of The Solar Flux: Quantitative Estimates For Planetary Studies Mark Claire1, J. Sheets1, M. Cohen2, I. Ribas3, D. Catling1 1Univ. of Washington, 2Univ. of California, 3Institut de Ciencies de l’Espai, Spain. 11:10 AM - 11:20 AM Room 604 Understanding changes in the solar flux over the age of the solar system is vital for understanding the evolution of planetary atmospheres. We describe a numerical parameterization for wavelength dependent changes to the non-attenuated solar flux appropriate for most times and places in the solar system. We combine published data from the Sun and solar analogs to estimate enhanced FUV and Xray fluxes for the young Sun, describe a new parameterization for the near UV where both the chromosphere and photosphere contribute to the flux, and use Kurucz models to estimate variable visible and infrared fluxes. The parameterization, a series of multipliers relative to the modern top of the atmosphere flux at Earth, is valid from 2 nm through the infrared, and from 0.6 Gyr through 6.7 Gyr, and is extended from the solar zero age main sequence to 8.0 Gyr subject to additional uncertainties. The parameterization is applied to a representative modern day solar flux, providing quantitative estimates of the wavelength dependence of solar flux for a range of paleodates that are relevant to studies of the chemical evolution of planetary atmospheres. We validate the code by comparison to the solar proxies Kappa1 Ceti and EK Draconis, and provide an Monte Carlo analysis of the uncertainties due to measurement error, unknown stellar ages, and intrinsic variability. 114 Starburst Galaxies Oral Session Room 606 114.01 Distribution of Star Formation in Distant Galaxies Marianne Y. Takamiya1, I. Cunnyngham1, C. Willmer2, M. Chun3, M. Young4, MTakamiyaUHH 1Univ. of Hawai - Hilo, 2Steward Observatory, University of Arizona, 3Institute for Astronomy, UH, 4Indiana University. 10:00 AM - 10:10 AM Room 606 The distribution in the Star Formation Rates (SFR) of distant galaxies are presented based on integral field unit observations with the GMOS-IFU on Gemini. Galaxies from the HDF and SA68 with redshifts between 0.6 and 0.8 were selected based on the presence and strength of H-beta and [OII]3727 emission lines measured in Keck/LRIS slit spectra. From the sample of 10 galaxies, only the bluest sources show [OII] in the IFU data regardless of total galaxy luminosity. The [OII] emission is distributed in an arc-like structure several kiloparsecs in scale. We posit that the brightest galaxies in the sample do not show significant emission lines possibly because the star formation is distributed uniformly across the disk at a lower intensity than the detection limit of the IFU. Moreover, the amount of extinction in brighter galaxies is likely to be larger and thus the star-forming sites may be highly obscured contributing to the non-detection of these optical lines in the IFU. At this redshift range, we identify two distinct modes of star formation among this seemingly homogenous group of z=0.7 star-forming galaxies. The sample of galaxies is being extended to include more IFU spectra from the Gemini Science Archive. By increasing the sample, we expect to characterize these modes of star formation which could be high-redshift counterparts of the U/LIRGs and dwarf starburst galaxies like NGC 1569 and NGC 4449. The authors wish to acknowledge funds provided by the Cottrell Research Corporation and the National Science Foundation (AST 0909240). 114.02D OH Masers from Andromeda to the Peak of Cosmic Star Formation Kyle Willett1 1University of Colorado. 10:10 AM - 10:30 AM Room 606 OH masers are well-known astronomical phenomena in which 18-cm radiation is amplified through the process of stimulated emission. My dissertation research focuses on the study of OH masers in multiple environments. The first portion is a Spitzer spectroscopic study of OH megamaser host galaxies. Several infrared properties of the host galaxy are shown to strongly correlate with the presence of an OH megamaser. These requirements include a smooth, optically thick dust environment and dust temperatures of 40-100 K in the circumnuclear region. I also demonstrate that the presence of an AGN highly selects against the presence of a megamaser - OHM hosts are dominated by starburst galaxies. I also use combined radio and IR data to make the first detailed test of an OH pumping model using the global parameters of the host galaxies. Based on our analysis, current models must be updated to include much higher optical depths and a variety of dust geometries. Secondly, I describe results from a new high-redshift search for OH megamasers using the Green Bank Telescope. The combination of new OHM detections and upper limits are used to construct an expanded OH luminosity function. Since the presence of an OHM traces both merging galaxies and extreme star formation, megamasers can serve as a powerful probe of galaxy evolution across cosmic time. The discovery of OHMs at z~1 is crucial for achieving this goal. Finally, I describe results of a new and complete OH survey of the Andromeda galaxy (M31). The goal of this survey is to find masers that can be used to measure M31's proper motion, which is as yet unknown. Any constraints on this will significantly impact our understanding of the Local Group's dynamics, history, and future evolution. 114.03 Obscured Starburst Activity in High Redshift Clusters and Groups Dale Kocevski1, B. Lemaux2, L. Lubin2, R. Gal3 1University of California, Santa Cruz, 2University of California, Davis, 3Institute for Astronomy, University of Hawaii. 10:30 AM - 10:40 AM Room 606 Using Spitzer MIPS 24um imaging and extensive Keck spectroscopy we have found evidence for environmentally triggered starburst activity within six clusters and groups at z~0.9. I will show that the density of 24um-detected galaxies in the cluster environment is nearly twice that of the surrounding field at this redshift and that this overdensity scales with the cluster's dynamical state. The 24um-bright members often appear optically unremarkable and exhibit only moderate [OII] line emission due to severe obscuration. Although their spatial distribution suggests they are an infalling population, a close examination of their spectral properties, morphologies and optical colors indicate they are not simply analogs of the field population that have yet to be quenched. Using stacked DEIMOS spectra, we find the 24um-detected cluster and group galaxies exhibit elevated levels of Balmer absorption compared to galaxies undergoing normal, continuous star formation. A similar excess is not observed in field galaxies with equivalent infrared luminosities, indicating a greater fraction of the detected cluster and group members have experienced a burst of star formation in the recent past compared to their counterparts in the field. Our results suggest that gas-rich galaxies at high redshift experience a temporary increase in their star formation activity as they assemble into denser environments. Using HST ACS imaging we find that disturbed morphologies are common among the obscured starburst population and become more prevalent in regions of higher galaxy density. We conclude that mergers are the dominant triggering mechanism responsible for the enhanced star formation found in the group galaxies, while a mix of harassment and mergers are likely driving the activity of the cluster galaxies. 114.04 The Physical Conditions Of A Lensed Star-forming Galaxy At z=1.7 Jane R. Rigby1, E. Wuyts2, M. Gladders2, K. Sharon2, G. Becker3 1Goddard Space Flight Center, 2University of Chicago, 3Kavli Institute for Cosmology and Institute of Astronomy, United Kingdom. 10:40 AM - 10:50 AM Room 606 We report rest-frame optical Keck/NIRSPEC spectroscopy of the brightest lensed galaxy yet dis- covered, RCSGA 032727-132609 at z=1.7037. From precise measurements of the nebular lines, we infer a number of physical properties: redshift, extinction, star formation rate, ionization parameter, electron density, electron temperature, oxygen abundance, and N/O, Ne/O, and Ar/O abundance ratios. The limit on [O III] 4363 A tightly constrains the oxygen abundance via the “direct” or Te method, for the first time in an average-metallicity galaxy at z?2. We compare this result to several standard “bright-line” O abundance diagnostics, thereby testing these empirically-calibrated diagnostics in situ. Finally, we explore the positions of lensed and unlensed galaxies in standard diagnostic diagrams, to explore the diversity of ionization conditions and mass-metallicity ratios at z=2. 114.05D WiFeS & GOALS: An IFU Study Of Metallicity, Shocks, And More In Nearby U/LIRGS Jeffrey Rich1, L. Kewley1, M. Dopita2 1University Of Hawaii, 2RSAA, Australian National University, Australia. 10:50 AM - 11:10 AM Room 606 Ultraluminous/Luminous Infrared Galaxies (U/LIRGs) are an excellent laboratory for investigating galaxy formation and evolution. They are complex systems, running the gamut of galaxy nuclear types and covering a sequence of massive mergers from isolated starburst galaxies to completely coalesced mergers with post-starburst populations and strong AGN. The detailed relationship between star formation, AGN, the ISM environment, gas motions, and merger evolution in LIRGs remains poorly understood. This talk presents the first results from a survey of nearby U/LIRGs from the GOALS sample. Our data come from WiFeS, a new IFU on the ANU 2.3m at Siding Spring Observatory. WiFeS has proved well suited for observing nearby U/LIRGs given its wide 25"x38" field of view, moderate R~7000 resolution and broad wavelength coverage (370-700 nm). We investigate galactic winds, extended emission power sources, metallicity distributions and stellar populations in our sample of U/LIRGs, many of which are merging systems. Our early results indicate extended LINER emission driven by slow shocks in some of our observed systems, which could have important implications for similar composite and LINER sources. We provide new slow shock models which provide an excellent fit to the observed line ratios. I will also discuss the observations of the least IR luminous galaxy in our sample, NGC 839, which seems to be a precursor E+A galaxy. Our work has shown that IFU data is incredibly useful for understanding key features of U/LIRGs and disentangling the composite nature of these complex systems. 114.06 The Crystalline Fraction Of Interstellar Silicates In Starburst Galaxies Francisca Kemper1, A. J. Markwick1, P. M. Woods1 1Univ. of Manchester, United Kingdom. 11:10 AM - 11:20 AM Room 606 We present a model using the evolution of the stellar population in a starburst galaxy to predict the crystallinity of the silicates in the interstellar medium of this galaxy. We take into account dust production in stellar ejecta, and amorphization and destruction in the interstellar medium and find that a detectable amount of crystalline silicates may be formed using relatively extreme input parameters. We discuss the effect of dust destruction and amorphisation of supernovae, and the relatively low dust-production efficiency of supernovae, and find that when taking this into account, crystallinity in the interstellar medium becomes hard to detect. Levels of 6.5-13% crystallinity in the interstellar medium of Ultraluminous Infrared Galaxies have been observed (Spoon et al. 2006, ApJ 638, 759). We conclude that not all these crystalline silicates can be of stellar (e.g. starburst related) origin, and additional crystallisation must be asociated with AGN activity. 114.07 The New Chandra View of M82 K. D. Kuntz1, D. K. Strickland1, T. M. Heckman1, L. Armus2, R. E. Kilgard3, A. Ptak1, T. P. Roberts4, R. K. Smith5, M. J. Ward4, A. Zezas5 1Johns Hopkins Univ., 2California Institute of Technology, 3Wesleyen Univ., 4Durham University, United Kingdom, 5SAO. 11:20 AM - 11:30 AM Room 606 M82 is the closest classical staruburst galaxy without a complicating AGN, showing a strong wind that extends more than 10 kpc out into the halo. As such it has been an important laboratory for studying both the sources powering the wind and the physical conditions within the wind itself. We have obtained a deep (497 ks) image of M82 with the Chandra ACIS-S which provides unprecedented detail about the wind structure within the central 5 kpc, and reveals large discontinuous emission regions at 5 and 7 kpc as well as the "cap" at 10.5 kpc (which are only partially correlated with structures seen in the UV and optical). We will present a preliminary hardness map and spatially resolved spectroscopic analysis. 115 Evolution of Galaxies I Oral Session Room 607 115.01D The Impact of Ram Pressure Stripping on Virgo Cluster Spirals Anne Abramson1, J. D. P. Kenney1 1Yale University. 10:00 AM - 10:20 AM Room 607 In recent years, both observations and simulations have shown that ICM-ISM stripping is likely an important driver of galaxy evolution. In order to understand the impact of stripping on galaxy evolution, it is vital to determine how the multi-phase ISM behaves during stripping, how long it takes to strip a galaxy, and how stripping influences star formation. We present multi-wavelength studies of three Virgo Cluster spirals undergoing active ram pressure stripping, including two with HST imaging. We estimate timescales for various stripping-related processes in the galaxies and identify signatures of stripping in the galaxies’ ISM and star formation distributions. All three have undisturbed old stellar disks and show one-sided extraplanar ISM distributions. This extraplanar ISM hosts regions of ongoing and recent star formation that has taken place within the past few hundred Myr, with some regions significantly younger. The galaxy NGC 4330 has distinct leading and trailing sides, including a striking ISM “upturn” feature at the leading edge. There are significant differences between the galaxy’s optical, UV, H ?, and HI morphologies, and we use stellar population models to estimate that it has taken 200-400 Myr to strip the ISM from a radius of >8 to 5 kpc on the galaxy’s leading side. HST imaging reveals that NGC 4522 and NGC 4402 have GMC-mass dust clouds located outside of their main ISM truncation radii, showing that the most massive clouds can decouple from the rest of the ISM during stripping. Dust features with linear morphologies in both galaxies reveal the projected ICM wind direction. By identifying morphological characteristics related to the ram pressure stripping process, we constrain the physics of interactions between the ICM and the complex multi-phase ISM, and we provide a foundation for future observational and theoretical studies investigating the extent to which ICM-ISM interactions drive galaxy evolution. 115.02D Growth and Evolution of the M81 Group of Galaxies Mihoko Yukita1, D. Swartz2 1Univ. of Alabama, 2USRA. 10:20 AM - 10:40 AM Room 607 The goal of this study is to investigate the cycle of the star formation focusing on the young massive star-forming regions and their interaction with their surroundings on the local scales in galaxies in the M81 group. The X-ray data are analyzed to understand the hot phase of the interstellar medium as characterized by the X-ray properties of the hot gas, separately treating supernovae remnants, Hii regions, and diffuse residual emission. The observed hot gas temperature of the events related to star-forming activities do not change dramatically over the recent star-formation time scale, about 100 Myr, but the density of the hot gas and hence pressure may decrease over time. The physical properties of the star-forming events on local scales are derived by comparing the broadband spectra using GALEX and Spitzer data to the stellar population synthesis models convolved with the dust reprocessing model. The mechanical luminosity from stars via stellar winds and supernovae is estimated based on the derived physical properties and compared to the X-ray luminosity of star-forming regions to estimate the amount of radiative losses of the hot gas. A very low ratio of the X-ray luminosity to mechanical luminosity suggests that most of the released energy goes into thermalization and is only slowly radiated over a very long period of time. 115.03 The Impact of Environment on Galaxy Group Evolution in the Coma-A1367 Supercluster Kelley M. Hess1, E. M. Wilcots1, M. P. Haynes2, R. Giovanelli2, ALFALFA Team 1Univ. Of Wisconsin-Madison, 2Cornell University. 10:40 AM - 10:50 AM Room 607 We present the HI content of galaxies and galaxy groups in the Coma-Abell 1367 Supercluster derived from a 180 square degree strip of the ALFALFA survey between +24d and +28d from 11h to 14h. We use this data to present a complete view of the neutral gas content in galaxy groups as a function of the large scale environment and derive a group HI mass function. The galaxy groups, derived from SDSS, span a range of global environments from the highest density sub-clumps falling into the center of the Coma cluster, to groups that make up the filament between the Coma and Abell 1367, to poor groups that exist on the edges of voids. Using the results from ALFALFA as well as widefield imaging and GALEX UV data we test the idea that the majority of galaxy evolution happens in groups prior to their in-fall into a galaxy cluster. In addition we correlate the frequency of low luminosity AGN activities with the HI properties of the environment. Together these multi-wavelength observations show how the HI content, the star formation rate and the AGN frequency change as a function of local galaxy density and distance from the cluster center and show how the role of environment affects galaxy evolution. 115.04 The Impact Of Radio-jet Driven Outflows On The Molecular Gas In Powerful Radio-galaxies Pierre Guillard1, P. Ogle1, B. Emonts2, R. Morganti3, P. Appleton4, C. Tadhunter5, T. Oosterloo3, A. Evans6 1Spitzer Science Center, Caltech, 2Australia Telescope National Facility, CSIRO, Australia, 3Netherlands Foundation for Research in Astronomy, Netherlands, 4NASA Herschel Science Center, IPAC, 5Department of Physics and Astronomy, University of Sheffield, United Kingdom, 6University of Virginia. 10:50 AM - 11:00 AM Room 607 Observations of ionized and neutral gas outflows in radio-galaxies (RG) suggest that AGN feedback has a galaxy-scale impact on the host ISM, but it is still unclear how the molecular gas is affected. Thus it is crucial to determine the physical conditions of the molecular gas in powerful RG to understand how radio sources may regulate the star formation in their host galaxies. We present deep Spitzer IRS high-resolution spectroscopy of 8 nearby RG that show fast HI outflows. Strikingly, all of these RG have extremely bright H2 mid-IR lines that cannot be accounted for by UV or X-ray heating. This strongly suggests that the radio jet, which drives the HI outflow, is also responsible for the shock-excitation of the warm H2 gas. In addition, the warm H2 gas does not share the kinematics of the ionized/neutral gas. In most of the sources, the mid-IR H2 lines are unresolved by the IRS, whereas ionized gas lines (e.g. NeII, NeIII) have FWHM up to 1200 km/s. If the dissipation of a small fraction (<10%) of the jet kinetic energy can explain the heating of the molecular gas, our data do not show that a significant fraction of the total molecular mass is expelled from these galaxies. 115.05 Galaxy Build-up And Evolution At z>=7: Results From The Ultra-deep Wfc3/ir Observations Over The Hudf From The Hudf09 Program Rychard Bouwens1, HUDF09 Team 1UC Santa Cruz / Leiden. 11:00 AM - 11:10 AM Room 607 The new WFC3/IR camera aboard HST enables us to survey the sky in the near-IR data 40x more efficiently than ever before -- permitting us to make enormous strides in our searches for z>=7 galaxies. Already in the 15 months of observations, we have deep and ultra-deep observation over 52+ arcmin**2 over legacy fields like the HUDF and GOODS. With these data, we have been able to select 80+ z~7 galaxies, 50+ z~8 galaxies, and even a candidate z~10 galaxy. These new selections have allowed us to quantify the evolution of the UV LF and faint-end slope from z~10, significantly constrain the stellar populations and dust properties of z~7-10 galaxies, and construct a general picture of how galaxies build up early in the universe. In this presentation, I highlight a few of our results. 116 Computation: Learning, Simulating, Data Reduction Oral Session Room 401 116.01 Automatic QSO Selection Algorithm Using Time Series Analysis and Machine Learning Dae-Won Kim1, P. Protopapas1, C. Alcock1, Y. Byun2, R. Khardon3 1Harvard-Smithsonian Center for Astrophysics, 2Yonsei University, Korea, Republic of, 3Tufts University. 10:00 AM - 10:10 AM Room 401 We present a new QSO selection algorithm using time series analysis and supervised machine learning. To characterize the lightcurves, we extracted multiple times series features such as period, amplitude, color and autocorrelation value. We then used Support Vector Machine (SVM), a supervised machine learning algorithm, to separate QSOs from other types of variable stars, microlensing events and non-variable stars. In order to train the QSO SVM model, we used 58 known QSOs, 1,629 variable stars and 4,288 non-variable stars from the MAssive Compact Halo Objects (MACHO) database. Cross-validation test shows that the model identifies 80% of known QSOs and have 25% false positive rate. Most of the false positives during the cross-validation are Be stars, known to show similar variability characteristic with QSOs. We applied the trained QSO SVM model to the MACHO Large Magellanic Cloud (LMC) dataset, which consists of 40million lightcurves, and found 1,097 QSO candidates. We crossmatched the candidates with several astronomical catalogs including the Spizter SAGE (Surveying the Agents of a Galaxy's Evolution) LMC catalog and various X-ray catalogs. The results suggest that the most of the candidates are likely true QSOs. 116.02 Combining Eulerian and Lagrangian Schemes to Investigate Outflows from AGN and their Effect on Star-Forming Galaxies Mark L. A. Richardson1, E. Scannapieco1 1Arizona State University. 10:10 AM - 10:20 AM Room 401 Issues with simulating astrophysical phenomenon have arisen lately with the appropriateness of the two dominant methods: Adaptive Mesh Refinement (AMR), which is well suited for mixing of media, turbulent flow, shocks, and shear layers, and Smoothed Particle Hydrodynamics (SPH), which is less complex, and more easily able to cover length scales spanning several orders of magnitude. For problems including the dynamics of stellar interactions, galactic formation, galactic feedback, and cosmological evolution, both these capabilities are essential. To address these issues, we created a tool to convert SPH datasets from codes such as SNSPH and Hydra into initial conditions for the AMR code FLASH, allowing efficient simulation of the initial conditions on large scales, and further simulation of the small scale regions of interest. As a test case we modeled colliding white dwarfs as possible SNIa progenitors to illuminate different mechanisms of Ni56 production. Our approach was then applied to cosmological datasets to allow for large-scale cosmological simulations with sufficient resolution to model AGN feedback and its effect on gas accretion and star formation in z = 2 galaxies. We would like to thank the Natural Sciences and Engineering Research Council of Canada for their support of this research. 116.03D Structure Formation in the Early Universe Andrew J. Davis1, P. Natarajan1 1Yale University. 10:20 AM - 10:40 AM Room 401 We present results from simulations of dark matter halos at high redshifts that likely host the some of the earliest stars and galaxies in the Universe. We present measurements of the halos' angular momentum, shape, and density profile for halos from z=15 to 6. We find that high spin haloes have stronger clustering strengths, and are found preferentially in high density environments and have closer neighbors than their low spin counterparts. High redshift spherical haloes are also up to 50 per cent more clustered than extremely aspherical haloes. We also present the results of simulations including baryons at high redshift, high spin halos to study the relation between the halo and baryonic structural properties at these early times. 116.04 Improving the Background Subtraction for X-Ray Observations of Galaxy Clusters Wenhao Liu1, D. Buote1, P. Humphrey1 1University of California, Irvine. 10:40 AM - 10:50 AM Room 401 The use of clusters as cosmological probes requires accurate measurements of global cluster properties, such as the virial mass. Since the X-ray emission rapidly decreases with radius, characterization of the background is a critical factor limiting the accuracy of such global mass measurements. We propose a method to improve background subtraction of Chandra ACIS observations that involves detailed modeling of the background components and the use of multiple apertures that contain both cluster emission and background. Preliminary results applying this method to a sample of nearby clusters will be presented. 116.05 MegaPipe: the MegaCam Image Stacking Pipeline Stephen Gwyn1 1Canadian Astronomy Data Centre, Canada. 10:50 AM - 11:00 AM Room 401 This presentation describes the MegaPipe image processing pipeline at the Canadian Astronomical Data Centre (CADC). The pipeline takes multiple images from the MegaCam mosaic camera on CFHT and combines them into a single output image. MegaPipe takes as input detrended MegaCam images and does a careful astrometric and photometric calibration on them. The calibrated images are then resampled and combined into image stacks. MegaPipe is run on PI data by request, data from large surveys (the CFHT Legacy Survey and the Next Generation Virgo Survey) and all non-proprietary MegaCam data in the CFHT archive. The stacked images and catalogs derived from these images are available through the CADC website. Currently, 2000 square degrees have been processed. 116.06 Is the k Coefficient Constant? Elise Weaver1, D. Caton1, A. B. Smith1 1Appalachian State University. 11:00 AM - 11:10 AM Room 401 Stored in the archives at Appalachian State University’s Dark Sky Observatory (DSO), there are approximately 30 years (starting in 1981) of variable star observations made with the observatory’s 18-inch telescope. These observations either come in the form of CCD images or older photomultiplier measurements of brightness. Both types of files contain brightness information on variable stars, and comparison stars. Looking at the comparison stars, we can calculate the extinction coefficient, k, by plotting how the magnitude of the star changes with airmass. The slope of the linear fit is k. Since k is the factor by which light is attenuated by the atmosphere, we hypothesize that if find any trends in k over the 30 year span of data, we can infer something about how the Earth’s atmosphere has changed. We have processed observation runs during the spring and fall (the times of the year with the best viewing conditions at DSO) that occurred in the latest seven years of the telescope's operation. Additionally, the ten years of photomultiplier data has an accompanying k measurement, which was calculated along side the light curve. Using these preliminary data, we cannot see any trends, but we need to fill in this middle regime before we can draw any conclusions. The approximately 15 years of intervening data needs to be processed, but that process is slowed by the disorganization of the data, which we are currently sorting. This research is currently being funded by the North Carolina Space Grant and Appalachian State University. 116.07 Subtraction Of Point Sources From Interferometric Radio Images Through An Algebraic Forward Modeling Scheme Gianni Bernardi1, D. Mitchell1, S. Ord1, L. Greenhill1, B. Pindor2, R. Wayth3, S. Wyithe2 1Harvard-Smithsonian Center for Astrophysics, 2University of Melbourne, School of Physics, Australia, 3ICRAR/Curtin Institute of Radioastronomy, Australia. 11:10 AM - 11:20 AM Room 401 Cutting edge cosmological investigations of the Epoch of Reionization (EoR) are driving a renovated effort in building low frequency radio interferometers. In order to detect the tiny EoR signal, high dynamic range (DR) imaging at frequencies below 200~MHz is required. High DR images are traditionally obtained by subtraction of bright sources from the ungridded visibilities, however, future generations of large-N radiotelescopes will generate such high volume data stream that the cost of storing the raw ungridded visibilities will be prohibitive. The DR will therefore be limited by well known pixelization effects. Further challenges for an image based deconvolution at low frequencies are a point spread function which varies significantly across the field of view, a time and frequency variable receptor response and ionospheric variability. In this presentation, we introduce a deconvolution algorithm which makes use of forward modeling to mitigate against the limitations of image-based deconvolution. Through forward modeling it is possible to generate a spatially variable point spread function and relate the sky brightness distribution to astrophysical parameters which are then retrieved through a non linear least squares minimization. We applied the method to the deconvolution of point sources on simulated observations of the Murchison Wide-field Array (MWA). MWA is the array with the largest number of correlated elements currently under construction (512 final elements) and will not have the option of storing the raw visibility data over long time integrations. We find that the accuracy to which point sources can be deconvolved/subtracted is only limited by their signal to noise ratio, not by their number or positions, therefore the DR increases with integration time. These results indicate this method to be promising for applications that require high DR imaging, like the detection of the EoR signal. This work was supported by the U.S. National Science Foundation. 116.08 Automatic Recommendation of Astronomy Literature Edwin A. Henneken1, M. J. Kurtz1, A. Accomazzi1, C. S. Grant1, D. Thompson1, E. Bohlen1, G. Di Milia1, J. Luker1, S. S. Murray1 1Smithsonian Astrophysical Observatory. 11:20 AM - 11:30 AM Room 401 Authors publish because they want to transfer information. An essential ingredient for this transfer is being able to find this information. As the Literature Universe is expanding rapidly, finding your way in this deluge of information can be a daunting task. How do you find what you are looking for in a reasonable amount of time and more importantly, information you could not have found using the normal information discovery model? When you have some prior information (like author names and/or subject keywords), you can use your favorite search engine and apply that information as filters. There are also more sophisticated services like the myADS service of the SAO/NASA Astrophysics Data System (ADS), that do intelligent filtering for you and provide you with customized suggestions. Alternatively, you can ask somebody you consider to be an expert. On this poster we describe a method (the "recommender system") that mimics this information "ask the export" discovery model, argue that it is practically feasible to incorporate this method as a useful addition to the existing ADS service and show that it is able to produce meaningful results. The ADS is funded by NASA Grant NNX09AB39G. Monday, January 10, 2011, 11:40 AM - 12:30 PM 117 Chandra's First Decade (Plus) of Discovery Invited Session Ballroom 6AB 117.01 Chandra's First Decade (Plus) of Discovery Harvey Tananbaum1 1Harvard-Smithsonian, CfA. Ballroom 6AB NASA's Chandra X-ray Observatory has provided an unprecedented view of the Universe at x-ray wavelengths since its launch in July 1999. Chandra's spectacular images and detailed spectra of astrophysical systems ranging from solar system objects to distant galaxies and clusters shed (x-ray) light on diverse topics such as stellar formation and demise, black hole-galaxy-cluster interactions, and properties of dark matter and dark energy. After a brief overview and status report on the Observatory, the focus of the talk will be on selected scientific highlights with emphasis on recent Chandra results. Monday, January 10, 2011, 2:00 PM - 3:30 PM 121 Super-Earths and Terrestrial Planets: Latest Results from the Kepler Mission Special Session Ballroom 6C 121.01 Kepler Mission Overview William J. Borucki1, D. G. Koch1, T. N. Gautier, III2, E. W. Dunham3, Kepler Science Team 1NASA Ames Research Center, 2Jet Propulsion Laboratory, 3Lowell Observatory. 2:00 PM - 2:30 PM Ballroom 6C Early Kepler observations show the presence of over 750 candidate planets, 1800 eclipsing binary stars, and variable stars of amazing variety. Many of the planetary candidates are smaller than Neptune. Discoveries of seven new exoplanets are shown including one of with two confirmed transiting planets. The candidate- and the announced-planets are compared with known exoplanets with respect to mass, size, density, and orbital period. Support by the NASA Astrophysics Division is gratefully acknowledged. 121.02 Physical Properties of Kepler's Super-Earths Dimitar D. Sasselov1, Kepler Science Team 1Harvard-Smithsonian CfA. 2:30 PM - 2:45 PM Ballroom 6C Planets in the radius range from about 1.25 to 2 Re, referred to as Super-Earth-sized planets, do not exist in our Solar System. Their physical properties as determined by theoretical modeling are expected to differ in many ways from our Solar System experience. The Kepler Mission is going to discover many such planets and determine their orbits and radii. For some of them follow-up observations may determine masses, and for a few of them asteroseismology of their stars from the Kepler light curve may determine an age. I will discuss theoretical models for such planets and how they could be constrained by the anticipated Kepler Mission observations. 121.03 Transit Timing Variations of Kepler Planets Matthew J. Holman1, D. C. Fabrycky1, D. Ragozzine1, E. B. Ford2, J. H. Steffen3, W. F. Welsh4, J. J. Lissauer5, Kepler Science Team 1Harvard-Smithsonian, CfA, 2University of Florida, 3Fermilab Center for Particle Astrophysics, 4San Diego State University, 5NASA Ames Research Center. 2:45 PM - 3:00 PM Ballroom 6C For a transiting planet following a fixed Keplerian ellipse, observers would measure a constant interval between successive transits. Orbital precession induced by general relativity, a planetary tidal bulge, or stellar oblateness could result in a variation of the transit interval for a planet with an eccentric or inclined orbit. Furthermore, tidal dissipation should alter the orbital period of the planet. These slow effects can only be detected over several years. However, the gravitational influence of other planets in the system can yield a detectable change in the transit interval over much shorter time scales. With the precision and continuous monitoring provided by Kepler photometry, the presence of sub-Earth mass planets in resonance, as well as larger planets at a wide range of orbital periods could, in principle, be readily detected. With the detection of transit timing variations in systems with multiple transiting bodies, such as Kepler-9, it is possible to establish from the transit observations alone that these bodies have planetary masses. But the combination of Kepler photometry with high-precision radial velocity observations is particularly powerful in establishing the orbital and physical properties of such systems. We will present the results of the analyses of transit timing variations in exoplanet systems observed by Kepler to date. Kepler was selected as the 10th mission of the Discovery Program. Funding for this mission is provided by NASA, Science Mission Directorate. 121.04 The Kepler Asteroseismic Investigation Hans Kjeldsen1 1University of Aarhus, Denmark. 3:00 PM - 3:15 PM Ballroom 6C The aim of asteroseismology is to probe the interiors of stars and quantify their properties, such as radius, mass, rotation and age, through observations of oscillation modes. Using the ultrahigh photometric precision and the extended length of the time series from Kepler one can perform asteroseismology which is orders of magnitudes more accurate than one could do just a few years ago. The Kepler asteroseismic programme is being conducted through the Kepler Asteroseismic Science Consortium (KASC), whose 400 members are organized into 13 working groups (KASC WGs) by type of variable star. The KASC WGs are established to ensure an efficient and structured work within KASC focusing on data analysis, stellar modelling and publication of data. The goals of the asteroseismic part of the Kepler project are to perform detailed studies of stellar interiors and to support the exoplanet investigation by measuring accurate stellar properties, especially the radius of planet host stars. The first results of the asteroseismic analysis indicate how the future analysis of Kepler data for many types of stars will impact our general understanding of stellar structure and evolution. A series of the most fascinating results from the asteroseismic analysis of Kepler data will be presented. 121.05 Stellar and Galactic Astrophysics with Kepler: Results from the Guest Observer Program Michael N. Fanelli1 1NASA Ames Research Center. 3:15 PM - 3:30 PM Ballroom 6C Kepler was launched in March, 2009 with a primary mission of determining the statistics of Earth-sized planets in the habitable zones of Sun-like stars. Each quarter Kepler continuously observes on order ~160,000 stars at a 30 minute cadence, and 500 stars at a 1-minute cadence. These light curves define a unique dataset for astrophysics, beyond the primary exoplanet mission. A broad range of topics are addressed, including stellar parameters from eclipsing binary modeling, asteroseismology, stellar activity cycles and pulsation modes across the HR diagram, episodic variability such as flares and accretion physics, and variability in galactic nuclei. In this talk, we will present a sampling of results derived from the Kepler data, selected to represent the efforts of Guest Observers and the general astronomical community. As the Kepler program proceeds, the growing archive of precision light curves will provide unparalled opportunities to explore many puzzles in the field of time domain astronomy. 122 Community Science with LSST Special Session Ballroom 6A 122.01 LSST System Overview Donald Sweeney1 1LSSTC. 2:00 PM - 2:15 PM Ballroom 6A The Large Synoptic Survey Telescope Corporation was formed to design, build, and operate the LSST. Currently 34 institutions have joined. The proposed observatory is funded as a private/federal partnership with federal support from the NSF and DOE. The LSST has a guiding principle of open-data and open-source for everyone in the US and Chile without any proprietary period. The total cost of the LSST Observatory in 2010 USD is approximately 465 million. Full science operations will begin six years after federal construction funding begins. The LSST will be located on Cerro Pachón Ridge near Gemini-South and SOAR. The telescope will survey the entire available sky every few nights using six bands 350nm to 1100nm ugrizy, covering 20,000 square degrees deeply in all six filters 1000 times in ten years. The optical design has an effective collecting aperture of 6.5 meters and a field of view of 9.6 square degrees. Currently, all three of the large mirrors are in construction using private funding. The site architecture and site preparation are in process. All Chilean environmental studies are approved and permits awarded. The 3.2 GigaPixel camera is the primary deliverable of the DOE under the leadership of SLAC. Prototype sensors have been delivered from two commercial suppliers. The Observatory will produce 18TB of data each night. Over the planned ten year survey the survey will produce 100PB of data and catalogs that will be processed and stored at NCSA. Transient events will be announced within 60 seconds world-wide; Static sky catalogs will be updated on various time scales; Data Releases with full provenance will occur once a year and include reprocessing of all prior data. Data Access Centers will be strategically located for serving the data to the scientific community and the general public. 122.02 LSST Science Collaborations Michael A. Strauss1 1Princeton Univ.. 2:15 PM - 2:30 PM Ballroom 6A The LSST will have enormous scientific impact on areas ranging from Earth-crossing asteroids to the most distant quasars, from the structure of the Milky Way halo to the distribution of dark matter on the largest scales and the nature of dark energy. To maximize the scientific potential of the survey, we have formed 11 so-called "Science Collaborations," with membership from LSST member institutions and the broader scientific community, which are preparing the tools needed to carry out their science once LSST data start to flow. They also represent advocates for their science areas, giving input to decisions about filter design, survey cadence, image processing algorithms, and database structure. Finally, they are playing a key role in testing the LSST software, and in planning for commissioning the telescope and system. Outside LSST member institutions, membership in the science collaborations is via application; there is a annual call for applications from the astronomy and physics community administered by NOAO. There is also the opportunity to propose new science collaborations. 122.03 Galactic Science With LSST Beth Willman1 1Haverford College. 2:30 PM - 2:45 PM Ballroom 6A LSST will yield revolutionary, multi-dimensional maps of the Milky Way (MW) galaxy and its neighbors. Over its 10-year survey period, LSST will catalog 10 billion MW stars (including photometric metallicities for 200 million F/G stars within 100 kpc) and map their tangential velocity field to at least 10 kpc (at 10 km/s precision) and as far as 25 kpc (at 60 km/s precision). Parallax data will allow a complete census of stars above the hydrogen-burning limit that are closer than 500 pc, and RR Lyrae stars will be detectable through their variability to a distance limit of 400 kpc. The star formation and hierarchical merging history of the MW to be facilitated by these deep maps will complement LSST’s observational cosmology based on billions of distant galaxies. The census of MW dwarf galaxy satellites and remnants will be complete out to the virial radius within LSST’s footprint, and will provide a detailed window into the spatial distribution and abundance of dark matter halos on sub-galactic scales. In this talk, I will highlight a few specific Galactic science programs and the corresponding simulations and observations we are conducting to prepare for LSST operations. 122.04 Extragalactic Science with LSST Philip J. Marshall1 1Stanford University. 2:45 PM - 3:00 PM Ballroom 6A The LSST survey will provide a very deep mine of data on the extra-galactic universe. The system is designed to enable all four of the probes identified by the Dark Energy task force, measuring cosmological parameters through cataloging 4 billion galaxies in photometric redshift bins for Baryon Acoustic Oscillation measurements, discovering hundreds of thousands of massive galaxy clusters, providing good lightcurves for hundreds of thousands of type Ia supernovae, and mapping the large scale dark matter distribution across half the sky and 10 billion years of cosmic growth with weak gravitational lensing. The high statistical precision will allow us to look for spatial variations in the universal expansion, while the combination and cross-correlation of these measurements will allow us to explore generalized parametrizations of dark energy, and test for non-standard gravity as analternative. The survey data will also allow other cosmological tests, such as cosmography with the thousands of expected strong gravitational lenses. Moreover, the study of galaxies to low surface brightness levels, the supermassive black holes active in their nuclei, and the supernovae they host will be greatly expanded by the enormous samples of objects and images generated. The scale of each of these science projects will require us to think of new ways of exploring and handling such large datasets. 122.05 Transient and Variable Star Science with LSST Lucianne M. Walkowicz1, LSST Transients and Variable Stars Science Collaboration 1UC Berkeley. 3:00 PM - 3:15 PM Ballroom 6A The time resolution and high etendue of LSST will revolutionize studies of a wide variety of astrophysical phenomena. The umbrella of time domain science with LSST encompasses objects both familiar and exotic, from classical variables within our Galaxy to explosive cosmological events. Within our Galaxy, LSST observations of variable stars will allow the mapping of the stellar halo in new detail, determination of the global Galactic cool star flare rate, and detection of rare evolved binary populations. Beyond the Milky Way, LSST will probe the distant Universe for the most luminous events. LSST will make localization for gravity wave events possible, identify counterparts to GRBs and X-ray flashes, and discover new supernovae. Increased sample sizes of known-but-rare observational phenomena will quantify their distributions for the first time, thus challenging existing theory. Perhaps most excitingly, LSST will provide the opportunity to sample previously untouched regions of parameter space, where transient events are expected on theoretical grounds, but have not yet been observed. In this talk, I will highlight some of the interesting scientific possibilities LSST will bring to transient and variable star science, as well as the challenges we face and opportunities for community involvement. 122.06 LSST Resources for the Community R. Lynne Jones1 1Univ. of Washington. 3:15 PM - 3:30 PM Ballroom 6A LSST will generate ~100 petabytes of images and ~20 petabytes of catalogs, covering 18,000-20,000 square degrees of area sampled every few days, throughout a total of ten years of time -- all publicly available and exquisitely calibrated. The primary access to this data will be through Data Access Centers (DACs). DACs will provide access to catalogs of sources (single detections from individual images) and objects (associations of sources from multiple images). Simple user interfaces or direct SQL queries at the DAC can return user-specified portions of data from catalogs or images. More complex manipulations of the data, such as calculating multi-point correlation functions or creating alternative photo-z measurements on terabyte-scale data, can be completed with the DAC's own resources. Even more data-intensive computations requiring access to large numbers of image pixels on petabyte-scale could also be conducted at the DAC, using compute resources allocated in a similar manner to a TAC. DAC resources will be available to all individuals in member countries or institutes and LSST science collaborations. DACs will also assist investigators with requests for allocations at national facilities such as the Petascale Computing Facility, TeraGrid, and Open Science Grid. Using data on this scale requires new approaches to accessibility and analysis which are being developed through interactions with the LSST Science Collaborations. We are producing simulated images (as might be acquired by LSST) based on models of the universe and generating catalogs from these images (as well as from the base model) using the LSST data management framework in a series of data challenges. The resulting images and catalogs are being made available to the science collaborations to verify the algorithms and develop user interfaces. All LSST software is open source and available online, including preliminary catalog formats. We encourage feedback from the community. 123 Science Highlights from NASA's Astrophysics Data Analysis Program I Special Session Ballroom 6B 123.01 Overview and Status of NASA's ADAP Douglas M. Hudgins1 1NASA Headquarters. 2:00 PM - 2:15 PM Ballroom 6B Over the years, NASA has invested heavily in the development and execution of an extensive array of space astrophysics missions. The magnitude and scope of the archival data from those missions enables science that transcends traditional wavelength regimes and allows researchers to answer questions that would be difficult, if not impossible, to address through an individual observing program. To capitalize on this invaluable asset and enhance the scientific return on NASA mission investments, the Astrophysics Data Analysis Program (ADAP) provides support for investigations whose focus is on the analysis of archival data from NASA space astrophysics missions. In this introduction to the scientific session, I will provide a brief introduction to the ADAP including an overview of its scope and content, as well as a synopsis of its current status and funding trajectory in coming years. 123.02 The Abundances of Carbon and Nitrogen in the Photospheres of Active B Stars Geraldine J. Peters1 1Univ. of Southern California. 2:15 PM - 2:30 PM Ballroom 6B Contemporary models for the structure and evolution of rapidly-rotating OB stars predict a photospheric enrichment of nitrogen due to the mixing of the CNO-processed material from the star’s core with the original surface material. The predicted N-enhancement increases as the star approaches its critical rotational velocity. Alternatively the Algol primaries should have N-enriched photospheres if the material currently being transferred is from the mass loser’s original core. To test these predictions, the C and N abundances in selected early Be stars and B-type mass gainers in Algol systems have been determined from spectroscopic data obtained with the IUE and FUSE spacecraft. The abundance analyses, carried through with the Hubeny/Lanz NLTE codes TLUSTY/SYNSPEC, were confronted with some challenges that are not encountered in abundance studies of sharp-lined, non-emission B stars including the treatment of shallow, blended rotationally-broadened lines, the appropriate value for the microturbulence parameter, correction for disk emission and possible shell absorption, and latitudinal variation of Teff and log g. The FUV offers an advantage over the optical region as there is far less influence from disk emission and the N lines are intrinsically stronger. Particularly useful are the features of C II 1324 Å, C III 1176 Å, 1247 Å, N I 1243 Å, and N III 1183,84 Å. Be stars with v sin i < 150 km s-1 were chosen to minimize the effect of latitudinal parameter variation. Given the errors it appears that the N abundance in the Be stars is normal. Expected mixing is apparently suppressed, and this study lends no support for Be star models based upon critical rotation. However, expected N-enhancement and a low C abundance are inferred for the B-type primaries in some interacting binaries. GJP is grateful for support from NASA Grants NNX07AH56G (ADP) and NNX07AF89G (FUSE), and the USC WiSE program. 123.03 Analysis of Archival FUSE Spectra of Accreting White Dwarfs in Cataclysmic Variables Patrick Godon1 1Villanova University. 2:30 PM - 2:45 PM Ballroom 6B We study the accreting white dwarfs (WDs) and accretion disks in Cataclysmic Variables (CVs) by carrying out a systematic analysis of the FUSE spectra of galactic CVs. Using the codes TLUSTY, SYNSPEC and BINSYSN, we generate synthetic spectra of WDs, and accretion disks, and derive the parameters of the systems: the temperature of the WD, its gravity, projected rotational velocity, chemical aundances, and the mass accretion rate. We use these results to probe the evolution of CVs and accretion physics. Our findings confirm that gravitational radiation can account for the WD effective temperature of polars both above and below the gap. Above the gap, the majority of DNs have a temperature lower than expected by the standard theory, and NL VY systems have a temperature higher than expected from the standard theory.Overall, it seems that the standard model does not agree with the nonmagnetic CVs above the period gap. A higher than expected temperature for the NL VY could be accounted for with a higher mass accretion rate. For disk-dominated systems, we find that the basic standard disk model fails almost systematically to fit the data. We find that the disk model must be improved at high accretion rate to include the star-disk boundary layer. As a scientific byproduct of this research we also create a web-based catalog of all the (fully reduced and co-added) FUSE spectra of CVs, including also all the synthetic spectra. This catalog will enable the full exploitation of the tremendous potential of the FUSE data for CVs on a large scale. This will be of invaluable importance for future NASA FUV space missions and it will add much value to the NASA FUSE mission itself. This work is supported by NASA under grant NNX08AJ39G issued though the Office of Astrophysics Data Analysis Program. 123.04 Spin Measurements for a Sample of Eight Stellar-Mass Black Holes Jeffrey E. McClintock1 1Harvard-Smithsonian, CfA. 2:45 PM - 3:00 PM Ballroom 6B Our team has published the spins of six accreting black holes, and I will present our results for two others, XTE J1550-564 and Cygnus X-1. I will discuss the implications of our spin data for models of relativistic jets and black hole formation. We measure spin by fitting the thermal continuum X-ray spectrum of the black hole to the relativistic thin-disk model of Novikov and Thorne, thereby determining the radius of the inner edge of the disk. We identify this disk radius with the black hole's innermost stable circular orbit (ISCO). It is then trivial to deduce the spin, which for a black hole of known mass depends solely on the radius of the ISCO via a standard GR formula. Strong theoretical evidence that the thin accretion disks we study are sharply truncated at the ISCO is provided by our GRMHD simulations. Likewise, strong empirical support for identifying the disk radius we measure with the radius of the ISCO is provided by decades of observational evidence, including our recent and compelling study of LMC X-3. We find for this persistent source, based on an analysis of hundreds of spectra collected over a span of 26 years by eight X-ray satellites, that the inner radius of the accretion disk is stable to approximately 4 percent. Thus, our measurements of spin are supported by both observational and theoretical evidence. 123.05 Black Hole X-ray Sources in Extragalactic Globular Clusters Stephen E. Zepf1 1Michigan State Univ.. 3:00 PM - 3:15 PM Ballroom 6B Whether there are black holes in globular clusters and what the properties of any such black holes might be remained unclear for many years. Advances in both X-ray and optical/near-infrared work have enabled searches for black hole X-ray sources to be extended to extragalactic globular clusters. We combined X-ray and optical observations to identify the first unambiguous black hole in a globular cluster in 2007. Through ADP supported work we have shown that this black hole is very likely to be a stellar mass and not an intermediate mass black hole. We have also used ADP supported archival studies and pointed observations to find two more globular cluster black hole X-ray sources, and two additional objects have been reported in the literature. We discuss these discoveries and their implications for the masses of black holes in globular clusters and for the formation of accreting black hole systems in dense stellar environments. 123.06 Constraining Accreting Binary Populations in Normal Galaxies Bret Lehmer1, A. Hornschemeier2, A. Basu-Zych2, T. Fragos3, L. Jenkins2, V. Kalogera3, A. Ptak2, P. Tzanavaris2, A. Zezas4 1Johns Hopkins University, 2Goddard Space Flight Center, 3Northwestern, 4SAO. 3:15 PM - 3:30 PM Ballroom 6B X-ray emission from accreting binary systems (X-ray binaries) uniquely probe the binary phase of stellar evolution and the formation of compact objects such as neutron stars and black holes. A detailed understanding of X-ray binary systems is needed to provide physical insight into the formation and evolution of the stars involved, as well as the demographics of interesting binary remnants, such as millisecond pulsars and gravitational wave sources. Our program makes wide use of Chandra observations and complementary multiwavelength data sets (through, e.g., the Spitzer Infrared Nearby Galaxies Survey [SINGS] and the Great Observatories Origins Deep Survey [GOODS]), as well as super-computing facilities, to provide: (1) improved calibrations for correlations between X-ray binary emission and physical properties (e.g., star-formation rate and stellar mass) for galaxies in the local Universe; (2) new physical constraints on accreting binary processes (e.g., common-envelope phase and mass transfer) through the fitting of X-ray binary synthesis models to observed local galaxy X-ray binary luminosity functions; (3) observational and model constraints on the X-ray evolution of normal galaxies over the last 90% of cosmic history (since z ~ 4) from the Chandra Deep Field surveys and accreting binary synthesis models; and (4) predictions for deeper observations from forthcoming generations of X-ray telesopes (e.g., IXO, WFXT, and Gen-X) to provide a science driver for these missions. In this talk, we highlight the details of our program and discuss recent results. 124 The Low-Frequency Gravitational Wave Universe: Detection Prospects, Sources, and Astrophysics Special Session Room 611/612 124.01 Low-Frequency Gravitational Wave Detection Using Radio Pulsars: Building a Galactic Scale Gravitational Wave Observatory Fredrick Jenet1 1Univ. of Texas at Brownsville. 2:00 PM - 2:20 PM Room 611/612 Observations of radio pulsars give us unique access to the nano-Hertz regime of the gravitational wave spectrum. This new window to the cosmos will allow us to study some of the most energetic events in the universe including the collision of two supermassive black holes. In this talk, we will review the basic detection techniques and discuss possible gravitational wave sources that may be detectable in the near future. We will also discuss the status of current pulsar timing based gravitational wave detection efforts. 124.02 Radio Pulsars as Gravitational Wave Detectors: Recent Observational Results Paul Demorest1 1National Radio Astronomy Observatory. 2:20 PM - 2:40 PM Room 611/612 The idea of using an array of millisecond radio pulsars as a nanohertz-frequency gravitational wave detector has continued to attract increasing attention over the past several years. Current experimental sensitivities are beginning to probe the upper limits of the predicted signal strength and a detection seems entirely within reach. The North American Nanohertz Observatory for Gravitational Waves (NANOGrav) project has been regularly timing a set of 20 millisecond pulsars over the past 5 years. These observations use the two largest radio telescopes on Earth, Arecibo Observatory and the NRAO Green Bank Telescope. In this talk, I will present newly developed analysis procedures and timing results from the NANOGrav 5-year data set. These are then used to place a new experimental limit on the strength of the stochastic nHz-frequency gravitational wave background. 124.03 Prospects for Gravitational Wave Detection with Pulsar Timing Arrays Alberto Sesana1 1Albert Einstein Institute, Germany. 2:40 PM - 3:00 PM Room 611/612 In the next decade the detection of gravitational waves (GW) will (hopefully) be a reality, opening a completely new window on the Universe. Massive black holes (MBH) binaries (MBHBs) are expected to be among the primary actors on this upcoming stage. Utilizing detailed MBHB population models (based on our current best understanding of galaxy formation and evolution trough mergers, and on our knowledge of the relations between MBHs and their hosts), I describe prospects of detecting GWs with forthcoming pulsar timing arrays (PTAs). A strong GW background, detectable at a level of 10-100ns timing precision, is a robust predictions of all the models. Single bright sources may also be resolvable, providing unique information about MBHB dynamics, and the physics of the processes driving their final coalescence. 124.04 Searching for Gravitational Waves with the EPTA and LEAP Ben Stappers1, M. Kramer2 1University of Manchester, United Kingdom, 2Max Planck Institut fur Radioastronomie, Germany. 3:00 PM - 3:20 PM Room 611/612 The European Pulsar Timing Array (EPTA) is a European effort spanning multiple institutes and multiple telescopes to directly detect gravitational waves by using high-precision pulsar timing. The project, instruments and its members are outlined, and methods and goals are discussed. The results of a the first EPTA upper limit on the stochastic gravitational wave background will be reported. The Large European Array for Pulsars (LEAP) will be introduced. LEAP is a project to coherently combine the signals of the large telescopes in Europe into a tied-array and increase the sensitivity, to that of a 200 m dish, for pulsars and thereby increase the precision of pulsar timing. I will present results from the initial combinations of data and discuss the prospects for the future. The LEAP project is funded through an European Research Council Advanced Grant to Michael Kramer. 125 AGN, QSO, Blazars II Oral Session Room 618/620 125.01 The Hard X-ray Spectra of Swift-BAT AGN Wayne H. Baumgartner1, R. Mushotzky2, J. Tueller3 1UMBC & NASA/GSFC, 2UMCP, 3NASA/GSFC. 2:00 PM - 2:10 PM Room 618/620 We present a composite analysis of the hard X-ray (15 -- 195 keV) spectra of over 500 AGN from the Swift-BAT all sky survey. The AGN observed in over 65 months of the survey are a mixture of Seyfert galaxies (Type I 56%, Type II 43%) with a median redshift of z=0.04, and QSOs and blazars at higher redshifts. It has been shown in high resolution X-ray (1-10 keV) studies of the cosmic X-ray background that the CXB is composed of the combined output of AGN out to high redshifts. The spectrum of the CXB is well measured and peaks in the hard X-ray band. However, the hard X-ray spectra of individual AGN have not been measured at the same level of detail until now. We present the hard X-ray spectra of individual Type I, Type II, and Compton-thick AGN from the Swift-BAT survey as well as an analysis of the stacked spectra of these groups in order to investigate whether the spectral properties (spectral index, cutoff) vary as a class or as a function of luminosity. We then attempt to address the question of how well the hard X-ray spectrum of the CXB can be explained as a composite of the spectra of AGN in the local universe as measured by Swift-BAT. 125.02 Fermi View of the Swift/BAT Seyferts Stacy H. Teng1, R. M. Sambruna2, D. S. Davis3, R. F. Mushotzky1, C. S. Reynolds1 1Univ. of Maryland, 2NASA-HQ, 3NASA-GSFC. 2:10 PM - 2:20 PM Room 618/620 We present the results of our detailed analysis of the first two years of Fermi data on the entire sample of Swift/BAT Seyfert galaxies. Of the 490 objects in the 58-month BAT catalog, three Seyferts have been identified to have Fermi/LAT counterparts. These objects have similar characteristics as flat-spectrum radio quasars, but are borderline radio quiet AGNs. The discovery of gamma-ray emission from Seyfert galaxies represents a new class of objects detectable by Fermi and has the potential to alter our understanding of the accretion process by the central engine. We will discuss the mechanisms for gamma-ray emission in Seyfert galaxies. Using upper limits derived from the Fermi non-detections, we will also examine the implications of these results for the GeV background. This work has been supported by the Fermi General Observers program. 125.03D Studying The Spectral Shape And The X-ray/uv Variability Of Active Galactic Nuclei With Data From Swift And Xmm Archives Sara Turriziani1 1Universita' Degli Studi Di Roma Tor Vergata, Italy. 2:20 PM - 2:40 PM Room 618/620 Many efforts have been made in understanding the underlying origin of variability in Active Galactic Nuclei (AGN), but at present they could give still no conclusive answers. Since a deeper knowledge of variability will enable to understand better the accretion process onto supermassive black holes, I built the first ensemble struction function analysis of the X-ray variability of samples of quasars with data from Swift and XMM-Newton archives in order to study the average properties of their variability. Moreover, it is known that UV and X-ray luminosities of quasars are correlated and recent studies quantified this relation across 5 orders of magnitude. In this context, I presents results on the X-ray/UV ratio from simultaneous observations in UV and X-ray bands of a sample of quasars with data from XMM-Newton archive. Lastly, I will present a complete sample of Swift/SDSS faint blazars and other non-thermal dominated AGNs. I used this sample to calculate the general statistical properties of faint blazars and radio galaxies and in particular their Radio LogN-LogS with fluxes down to 10 mJy, in order to gain knowledge on the contribution to Cosmic Microwave Background (CMB) and gamma-ray background radiation from the faint tail of the radio population. I acknowledge financial support through Grant ASI I/088/06/0. 125.04D Quasar SEDs in XMM-COSMOS: 90% Uniform, 10% Hot-Dust-Poor - Low Covering Factors and Large Accretion Disk Outer Radii Heng Hao1, M. Elvis2, F. Civano2, COSMOS Team 1Harvard Univ., 2Center for Astrophysics. 2:40 PM - 3:00 PM Room 618/620 The spectral energy distributions (SEDs) of AGNs are essential to understand the physics of the supermassive black holes (SMBHs) and their host galaxies. We present a detailed study of AGN SED shapes in the optical-near infrared for 408 X-ray selected type 1 AGNs from the XMM-COSMOS Survey. We define an near-IR/optical index-index ('color-color') diagram to investigate the mixture of AGN continuum, reddening and host galaxy contribution. We found that ~90% of the AGNs lie on mixing curves between the Elvis et al. (1994) mean AGN SED (E94) and a host galaxy, with only the modest reddening [E(B-V)=0.1-0.2]. Lower luminosity and Eddington ratio objects have more host galaxy. The E94 is remarkably good in describing the SED shape in the 0.3-3 micron decade over a range of 3.2 dex in Lopt, 2.7 dex in L/LEdd, and for redshifts up to 3. However, 10% of the AGNs are inconsistent with any AGN+host+reddening mix. These AGNs have weak or non-exist near-IR bumps, suggesting a lack of the hot dust characteristic of AGNs. The fraction of these “hot-dust-poor” AGNs evolves with redshift from 6% at z<2 to 20% at 2 5 mags followed immediately by a long eclipse of duration 38 min and depth ~2 mags. Between eclipses the light curve varies sinusoidally with amplitude ~1 mag. We observe significant changes in the light-curve shape with wavelength, with no short-duration eclipses appearing in the J band. The spectra reveal strong Hydrogen emission lines, and a continuum that varies with light curve phase. No known radio or x-ray source coincides with the new object’s location. 126.05 K-band Observations of Sub-Gap Cataclysmic Variables Ryan T. Hamilton1, T. E. Harrison1, C. Tappert2, S. B. Howell3 1New Mexico State University, 2Universidad de Valparaiso, Chile, 3NOAO. 2:50 PM - 3:00 PM Room 615/617 We present K-band spectroscopy of short period, ``sub-gap'' cataclysmic variable (CV) systems obtained using ISAAC on the VLT. We show the infrared spectra (IR) for nine systems below the 2-3 hour period gap: V2051 Oph, V436 Cen, EX Hya, VW Hyi, Z Cha, WX Hyi, V893 Sco, RZ Leo, and TY PsA. We are able to clearly detect the secondary star in all but WX Hyi, V893 Sco, and TY PsA. We present the first direct detection of the secondary stars of V2051 Oph, 436 Cen, and determine new spectral classifications for EX Hya, VW Hyi, Z Cha, and RZ Leo. We find that the CO band strengths of all but Z Cha appear normal for their spectral types, in contrast to their longer period cousins above the period gap. This brings the total number of CVs with moderate resolution (R ? 2000) IR spectroscopy to forty-eight systems: six pre-CVs, thirty-one non-magnetic systems, and eleven magnetic or partially magnetic systems. We discuss the trends seen in the IR abundance patterns thus far, and highlight a potential link between anomalous abundances seen in the IR with the C IV/N V anomaly seen in the ultraviolet. We present a compilation of all systems with sufficient resolution IR observations to assess the CO band strengths, and, by proxy, obtain an estimate on the C abundance on the secondary star. 126.06 Following the Accreting Pulsating White Dwarfs in GW Lib and V455 And After their Superoutbursts Paula Szkody1, A. S. Mukadam1, B. T. Gaensicke2, E. Bullock1, E. J. Harpe3, A. Henden4, E. M. Sion5, D. M. Townsley6 1University of Washington, 2University of Warwick, United Kingdom, 3Heritage High School, 4AAVSO, 5Villanova University, 6University of Alabama. 3:00 PM - 3:10 PM Room 615/617 Accreting pulsating white dwarfs offer the opportunity to study the effects of mass transfer, rotation and accretion on the internal structure of white dwarfs, as pulsation modes in white dwarfs penetrate deep into the stars. Thirteen of these systems are now known to reside in cataclysmic variables. These objects undergo large amplitude outbursts on 20-30 yr timescales which heat the white dwarfs and move them out of their instability zones for 2-3 yrs. Following the white dwarfs as they re-enter the instability strip thus allows an unprecedented opportunity to glean information about the modes and depth of heating. GW Lib and V455 And are two objects with accreting pulsating white dwarfs that underwent superoutbursts in 2007. We have followed these systems with ultraviolet data from GALEX and HST, and ground-based optical data. These 2 systems show different behavior, with GW Lib remaining hot and lacking pulsations 3 yrs post outburst, while V455 And shows a return of a group of periodicities present at shorter periods than pre-outburst. These differences are being studied on the basis of the masses and rotation rates derived from the COS data. Support for this work was provided by NASA GALEX grants NNX08AU43G, NNX09AF87G, HST grants GO-11638, GO-11639, and NSF grant AST-0607840. 127 Galaxy Clusters: Intracluster Medium and Cosmology Oral Session Room 606 127.01D Sloshing Gas in Galaxy Clusters Ryan Johnson1, M. Markevitch2, C. Jones2, G. Wegner3, W. Forman2 1Dartmouth College / Denison University, 2Harvard Smithsonian - Center for Astrophysics, 3Dartmouth College. 2:00 PM - 2:20 PM Room 606 Despite appearing relaxed and symmetric on large scales, many galaxy clusters exhibit striking asymmetries in their core gas distributions. One mechanism for creating these asymmetries is by the bulk oscillation, or sloshing, of the core gas about the cluster gravitational potential minimum. In X-ray observations, this sloshing gas appears as sharp edges in a cluster's surface brightness distribution, with the edges demarcating the (projected) boundary between the lowest entropy gas near the sloshing core and the higher entropy outer cluster gas. Simulations have demonstrated that this sloshing may be brought about by gravitational interactions with other groups or clusters and that such interactions need not be so energetic as mergers, but that even glancing interactions may initiate this gas sloshing. Since large clusters tend to lie at the intersection of cosmic filaments, where there are potentially many such interactions, we expect that most massive clusters should be undergoing some degree of gas sloshing as a result of previous interactions with infalling groups or clusters. My dissertation explores the nature of this core gas sloshing in clusters and how we may use this phenomena as a pointer to the merger history of the system. 127.02 A Double Lobe Radio Galaxy Between Clusters: Constraints on the Intrafilament Medium Density Louise O. V. Edwards1, D. Fadda1, D. T. Frayer2 1California Institute of Technology, 2National Radio Astronomy Observatory. 2:20 PM - 2:30 PM Room 606 We have found the first bent double lobe radio source (DLRS) in a known cluster filament. This discovery has enabled us to constrain the intrafilament density (IFM) to be between (1-10)x10-29 gm/cm3. The host filament has been observed using extensive multiwavelength photometry and confirmed with hundreds of member redshifts. It stretches from the rich galaxy cluster Abell 1763 to the nearby cluster Abell 1770, ~13Mpc away. Our recent observations from the VLA uncovered the DLRS at a distance of 3.4Mpc from the center of Abell~1763, well outside the virial radius of either cluster. We measure the jet flux and calculate the minimum pressure in the jet. Using geometric arguments to derive the orientation and bend of the jet, and assuming that the bend of the of the jet is due to ram pressure, we are able to constraint the density of the IFM. Our measurements agree with the small number of IFM estimates that currently exist, including results from different approaches such as the direct X-ray observations of Abell 222/223 and related WHIM measurements in Sculptor, as well as theoretical models. Our findings justify future searches for bent double lobe radio sources located several Mpc from cluster cores, as they may be good markers of super cluster filaments. 127.03D On the Origins of H? Emission in the Cool Cores of Galaxy Groups and Clusters Michael McDonald1, S. Veilleux1, R. Mushotzky1 1University of Maryland. 2:30 PM - 2:50 PM Room 606 We present results from a survey of cooling flow clusters and groups covering nearly three orders of magnitude in mass, and 1-2 orders of magnitude in temperature and mass deposition rate, aimed at explaining the presence and morphology of warm, ionized gas in the cool cores of galaxy groups and clusters. Using the Maryland-Magellan tunable filter on the Baade 6.5-m telescope at Magellan we have taken a census of these mysterious Halpha filaments with unprecedented depth and resolution. These data have been supplemented with new and archival X-Ray (Chandra), UV (HST, GALEX, XMM-OM), near-IR (2MASS) and radio (VLA) observations. Armed with the most detailed picture of the warm, ionized gas in cooling flow clusters to date, we investigate the possible mechanisms for producing the observed morphologies (buoyant bubbles, runaway cooling, interaction with satellites, etc) as well as possible ionization mechanisms (young stars, heat conduction from the ICM, collisional heating from cosmic rays, etc). Additionally, we determine the effect of environment on the formation of ionized filaments by considering the correlation of Halpha filaments with the global mass, temperature and gas fraction of the system. Our results offer exciting new constraints, both quantitative and qualitative, for the latest models of cooling flow clusters. 127.04 Mass Function Predictions Beyond LCDM Suman Bhattacharya1, K. Heitmann1, M. White2, Z. Lukic1, C. Wagner3, S. Habib1 1Los Alamos National Laboratory, 2UC Berkeley, 3ICC, Barcelona, Spain. 2:50 PM - 3:00 PM Room 606 The statistics of dark matter halos is an essential component of precision cosmology. The mass distribution of halos, as specified by the halo mass function, is a key input for several cosmological probes. The sizes of N-body simulations are now such that, for the most part, results need no longer be statistics-limited, but are still subject to various systematic uncertainties. Discrepancies in the results of recent simulation campaigns for the halo mass function remain in excess of statistical uncertainties and of roughly the same size as the error limits set by near-future observations; we investigate and discuss some of the reasons for these differences. Quantifying error sources and compensating for them as appropriate, we carry out a high-statistics study of dark matter halos from 67 N-body simulations to investigate the mass function and its evolution for a LCDM cosmology and for a set of wCDM cosmologies. We quantify the breaking of universality in the form of the mass function as a function of redshift, finding an evolution of as much as 10 % away from the universal form between redshifts z=0 and z=2. We provide a fitting formula to our results for the (evolving) LCDM mass function over a mass range of 6e11-3e15 solar-mass to an estimated accuracy of about 2 %. In the case of the wCDM cosmologies, we find that the mass function is described by the same fitting formula at an accuracy level of 5-10 % over widely varying cosmologies. 127.05 Three-Dimensional Structure of the 1367 Abell - Coma Supercluser Jane Kaczmarek1, K. Hess1, E. Wilcots1 1University of Wisconsin-Madison. 3:00 PM - 3:10 PM Room 606 We apply the IR Tully-Fisher relationship, combining measurements of the HI profiles from the ALFALFA survey and near-IR colors from 2MASS for 364 galaxies in the Abell 1367 - Coma supercluster ranging from 6000-8500 km/s. We describe the basic 3-dimensional structure of the supercluster, highlighting the known galaxy groups and compare with model of the density distribution around Coma. 128 Evolution of Galaxies II Oral Session Room 607 128.01D The Formation and Evolution of Massive Black Holes in Cosmological Simulations Jillian M. Bellovary1, F. Governato2, T. Quinn2, M. Volonteri1 1University of Michigan, 2University of Washington. 2:00 PM - 2:20 PM Room 607 Massive black holes (MBHs) are inextricably connected to the formation of massive galaxies, but their formation, evolution, and specific effects on their hosts are not clearly understood. Cosmological simulations of galaxy formation, including prescriptions for MBH formation, mergers, accretion, and feedback, are a unique way to shed light on this issue. We use a suite of simulated galaxies with a range of masses and formation histories to make predictions regarding the distribution of MBHs in galaxies as well as their fueling histories. We predict a population of ``wandering'' MBHs in the halos of massive galaxies, which are the remnant cores of tidally stripped satellite galaxies. These objects may be observed as off-nuclear ultraluminous X-ray sources if the cores retain a gas reservoir and are perturbed in some way, such as a passage near the galactic disk. Additionally, we trace the origins of gas accreted by central black holes to test the standard paradigm that quasars are fueled by major mergers. We find that in addition to major mergers, a high redshift quasar can be fueled through smoothly accreted cold flows; thus, a major merger is not a requirement for quasar activity. Bulge morphology is likely an observational relic of a galaxy's merger history and can be used to test whether a black hole's accretion has been fueled through mergers or more quiescent processes. 128.02D Insight into the Early Evolution of Globular Clusters and Supermassive Black Holes from Panchromatic Observations of Nearby Dwarf Starburst Galaxies Amy E. Reines1 1Univ. of Virginia. 2:20 PM - 2:40 PM Room 607 In the earlier universe, both globular clusters and the seeds of supermassive black holes are believed to have formed in the progenitors of modern massive galaxies, although the details are poorly understood. Direct observations of these low-mass, distant, and hence faint systems are unobtainable with current capabilities. However, gas-rich dwarf starburst galaxies in the local universe, analogous in many ways to protogalaxies at high-redshift, can provide critical insight into the early stages of galaxy evolution including the formation of globular clusters and massive black holes. We present a panchromatic study of nearby dwarf starburst galaxies harboring nascent globular clusters still embedded in their birth material. We also show the first example of a nearby dwarf starburst galaxy simultaneously hosting an actively accreting intermediate-mass central black hole and an extreme burst of star formation. The massive black hole in this dwarf galaxy is unusual in that it is not associated with a bulge, a nuclear star cluster, or any other well-defined nucleus, likely reflecting an early phase of black hole and galaxy evolution that has not been previously observed. 128.03D Application of a New AGN Diagnostic to Infrared Galaxies: Unveiling Obscured AGNs Stephanie Juneau1, M. Dickinson2 1University of Arizona, 2NOAO. 2:40 PM - 3:00 PM Room 607 I will present a new excitation diagnotic that allows us to identify the presence of active galactic nuclei (AGNs) in galaxies out to redshift ~1. Our understanding of galaxy evolution relies on disentangling the roles of star formation and AGN, two phenomena affecting the fate of galaxies. Although it has become increasingly clear that supermassive black holes (SMBHs) are ubiquitous, the details of their connection to their host galaxies remain open questions. For instance, what fraction of SMBHs are actively accreting? How does that fraction relate to the rate of star formation? To address these topics, I will describe a census of AGNs within 70-micron selected galaxies from the Far-Infrared Deep Extragalactic Legacy survey (FIDEL). This population of galaxies includes the main contributors to the star formation rate density at redshift ~ 1. We find that although only ~10-12% of 70-micron galaxies with emission lines host a strong, X-ray detected AGN, the AGN fraction reaches ~40% when including systems with low-level activity. Furthermore, the diagram reveals AGNs that are misidentified in the most sensitive Chandra X-ray observations (reaching 2 Msec in the GOODS-North field). I will show evidence that a large number of these "missed" AGNs are likely Compton-thick. 128.04 High-z Superwinds from Massive Star-forming Clumps Sarah Newman1, R. Genzel2, SINS team 1UC Berkeley, 2MPE, Germany. 3:00 PM - 3:10 PM Room 607 We have observed large-scale galactic outflows from resolved clumps in several z~2 galaxies in emission. The observations were made using SINFONI/VLT integral field spectroscopy with adaptive optics of H?, [NII] and [SII]. We estimate the outflow rate from these H?-bright, rapidly star-forming clumps as several times the SFR. We also estimate the lifetime of these clumps based on the stellar ages, the gas exhaustion timescale, the metal enrichment timescale and the expansion timescale. We can understand these massive outflow rates in the context of superwinds generated by feedback from active star formation. This result is highly significant as this is the first time that outflows have been detected from spatially resolved clumps, and the information gathered on the fate of these clumps will help us to better understand galaxy formation and evolution at the redshifts at which today’s massive galaxies were formed. This work was possible thanks to the National Science Foundation’s Graduate Research Fellowship Program. 128.05 First Results from HIPPIES: Constraint on the Very Bright End of Galaxy Luminosity Function at z >~ 7 Haojing Yan1, HIPPIES Project 1CCAPP, Ohio State University. 3:10 PM - 3:20 PM Room 607 We present the first results from the Hubble Infrared Pure Parallel Imaging Extragalactic Survey (HIPPIES), which utilizes HST pure parallel orbits to do deep imaging along a large number of random sightlines. One of the key goals of HIPPIES is to search for candidate galaxies at z>7 and to address the very bright-end of the luminosity function at these redshifts. We report the Ys-dropouts discovered among the 30 WFC3 fields observed in Cycle 17(program 11700, PI. M. Trenti; and program 11702, PI. H. Yan), and compare to the initial Y-dropout selection results from 8 WFC3 fields recently observed in Cycle 18 (program 12286, PI. H. Yan). We acknowledge the support of NASA grant HST-GO-11702.*. 128.06 Near-infrared Imaging And Z=7 Galaxy Candidates In The GOODS-North Field Nimish P. Hathi1, B. Mobasher2, P. Capak3 1Carnegie Observatories, 2UCR, 3Caltech. 3:20 PM - 3:30 PM Room 607 Near-infrared (NIR) imaging covering the full GOODS-North (GOODS-N) field has been done only from the ground, using the CFHT and the Subaru telescopes. The lack of space-based NIR imaging in this field has increased the importance of these ground-based observations. We present the co-added/combined NIR images in the GOODS-N field obtained using the CFHT/WIRCam and the Subaru/MOIRCS instruments. MOIRCS observations cover approx. 60% of the central GOODS-N field, while WIRCam observations cover a much wider area. These archival imaging data in J and Ks filters were reduced independently and then combined to increase the depth of these observations in the ACS covered GOODS-N region. These combined images cover the GOODS-N area to a depth of about 25 AB mag in both filters. We also examine the feasibility of using (z-J) vs. (J-Ks) color selection in the ACS covered GOODS-N region to identify bright z-band dropouts, which are galaxy candidates at z=7. Our preliminary results indicate a very low surface density (approx. 0.01 objects per sq. arcmin) of bright (< 26 mag) z=7 galaxy candidates in the GOODS-N field. We discuss the importance of these NIR data, and the results obtained from our z-band dropout search. 129 HAD V History of Astronomy Oral Session Room 613/614 129.01 The Legendary Fourth-Century Total Solar Eclipse in Georgia: Fact or Fantasy? Jefferson Sauter1, I. Simonia1, F. Stephenson1, W. Orchiston1 1James Cook University, Australia. 2:00 PM - 2:15 PM Room 613/614 Medieval Georgian accounts of a sudden darkening of the sky are studied in detail. Though aspects of the story were likely embellished or fantastical, specific clues in the written sources suggest a total solar eclipse (TSE) from the 4th century AD. We examine the local circumstances of a likely candidate, the TSE of 6 May 319, using computer simulations and accounting for visibility corrections and constraints on the accumulated clock error (?T). If the accounts do describe this TSE, the value of ?T inferred from the written sources would agree well with the range of values derived from Stephenson (1997). Additional analysis shows why this eclipse may have seemed uniquely remarkable to observers at the presumed location. 129.02 Declinations in the Almagest: An Evaluation and Comments on their Use by Tycho Brahe and Edmond Halley John C. Brandt1, P. Zimmer1, P. B. Jones2 1Univ. of New Mexico, 2Univ. of Arizona. 2:15 PM - 2:30 PM Room 613/614 The Almagest (Book VII, Chapter 3: Toomer 1998) gives 54 stellar declinations attributed to Timocharis, Aristyllus, Hipparchus, and Ptolemy (“As found by us”). We evaluate these declinations (?) by comparing them to precessed modern positions (d) obtained by using U.S. Naval Observatory software. A recent HIPPARCOS catalogue is the source of positions, proper motions, and parallaxes, and radial velocities come from the Yale Bright Star Catalog. The standard deviation (?) is computed for ? = ?-d for a plausible range of years for each observer. The minimum standard deviation, ?min , determines the accuracies and epochs of observation assuming that an observer’s observations were taken at approximately the same time. The results are: Timocharis, ?min = 0.135° and = +0.022° at 295 BC: Aristyllus, ?min = 0.089° and = -0.004° at 258 BC; Hipparchus, ?min = 0.113° and = +0.010° at 128 BC; and Ptolemy, ?min = 0.199° and = +0.005° at 115 AD. The precisions (?min) are remarkable, the mean errors () are small, and the dates are compatible with the historical evidence except for Ptolemy. The ?s for individual observers are approximately Gaussian except Timocharis’s value for Arcturus at 5.6?min which appears to be erroneous; our results are based on 53 declinations. The study of Almagest declinations by Maeyama (1984) uses the same approach and input data from the catalogue by Boss (1910). The results of the two studies are close, but with differences. Our values should be an improvement because of improved input data. We comment on the use of Almagest declinations by Tycho Brahe and Edmond Halley. 129.03 Kepler’s Cosmos And The Lathe Of Heaven Kenneth Brecher1 1Boston University. 2:30 PM - 2:45 PM Room 613/614 Johannes Kepler’s Mysterium Cosmographicum, published in 1596, presented his vision of the geometrical structure of the solar system. Kepler sought to account for the number of planets, thought to be six, as well as their orbital radii. He assigned orbits to the planets in three-dimensional space. Kepler proposed that the planets move on six spheres inscribed within and circumscribed around the five platonic solids. How did he arrive at his model? By his own account reported in the book, the central idea occurred to him while giving a lecture about planetary conjunctions. But was this revelation the origin of the model? In this presentation, we discuss the artistic, scientific and mathematical environment in which Kepler was immersed in late 16th century Europe. Examples will be shown of some of the readily available inscribed polyhedra that he may have seen - printed in widely circulated books, included in well-known paintings and engravings, and displayed as three dimensional ornamentally turned sculptures. It is highly likely that he saw such physical models five years later while in the employ of Rudolf II who was an avid ornamental turner. Layered polyhedral ivory turnings were made by the nobility with what were then fairly common lathes. Kepler himself wanted to have his own celestial model made into a punch bowl! Therefore, it seems plausible that Kepler had seen models of inscribed platonic solids well before 1596. Later in life Kepler reprinted the Mysterium Cosmographicum with very little fundamental change in its outlook, even after having found what we now call Kepler’s three laws of planetary motion. His interest in nested polyhedra may well have preceded any astronomical evidence or geometrical reasoning, arising from artistic and aesthetic encounters that occurred early in his life. Project LITE is supported by the NSF through DUE Grant # 0715975. 129.04 Astronomy with a Difference: China Nathan Sivin1 1University of Pennsylvania. 2:45 PM - 3:30 PM Room 613/614 Chinese astronomy, observational and computational, is the only one of the world’s traditions minutely documented and uninterrupted in its evolution for the last two thousand years. Its independence from Western influence for most of that period, and the fundamental differences in the ways it was thought through and organized, make it valuable for studying astronomical possibilities never explored elsewhere. This short talk will sketch its special character and the nature of the historical research going on in China and elsewhere. 130 Planetary Nebulae and Supernova Remnants Oral Session Room 609 130.01 Infrared Spectroscopy of Late Stage Post-AGB Stars Alexa H. Hart1, J. Hora2, L. Cerrigone3, G. Umana4, C. Trigilio4, M. Cohen5, M. Marengo6 1University of Denver & Harvard-Smithsonian Center for Astrophysics, 2Harvard-Smithsonian Center for Astrophysics, 3Max-Planck-Institut fuer Radioastronomie, Germany, 4INAF-Osservatorio Astrofisico de Catania, Italy, 5University of California at Berkeley, 6Iowa State University. 2:00 PM - 2:10 PM Room 609 During their pilgrimage towards Planetary Nebulae (PNe), dust-enshrouded post-AGB stars undergo a structural and perhaps chemical transformation. Many potentially responsible shaping mechanisms have been proposed, including an axisymmetric super wind, several types of binary interactions and magnetic confinement. During this critical phase, the central star is typically obscured at optical wavelengths; infrared emission from the circumstellar envelope provides a window into the processes occurring in the interior region. I present spectra (from Spitzer’s IRS and MMIRS on the Magellan Clay Telescope) of a sample of late post-AGB stars designed to bracket the transition from post-AGB to PN. These data reveal important clues about conditions in the circumstellar environment during this enigmatic phase. 130.02D Cosmic Ray Acceleration at Supernova Remnant Shocks Daniel Castro1 1Harvard Smithsonian Center for Astrophysics. 2:10 PM - 2:30 PM Room 609 Observational evidence increasingly supports the scenario where cosmic rays are accelerated at supernova remnant (SNR) shocks. Both thermal and non-thermal emission from these objects, in a wide range of wavelengths, indicate the presence of extremely energetic particles in SNRs, and the development of analytical and semi-analytical models of SNR evolution where diffusive shock acceleration (DSA) is efficient allow for constraining the nature of cosmic ray production. The research presented in this talk focuses on the impact of DSA on the evolution and observational properties of SNRs, and it is divided in three main parts. Firstly, an X-ray study of the morphology and spectral properties of SNR G296.1-0.5 is performed, using the XMM-Newtonn X-ray Observatory. Modeling of the observational characteristics of this SNR suggest the remnant is in the adiabatic expansion phase, and is possibly the result of the core collapse of a massive progenitor. The detection of a bursting compact source in the direction of the remnant, and its nature and possible association with the SNR, is also discussed. Secondly, a semi-analytical model is presented, which considers the modifications to the evolution and emission characteristics of SNRs in the Sedov-Taylor phase, imposed by DSA. This study shows how efficient cosmic ray acceleration impacts the analysis of SNRs in this evolution phase, and how the results diverge from the standard model when the acceleration process is efficient. Finally, the gamma-ray observations, with the Fermi LAT, of MeV-GeV emission coincident with four SNRs are analyzed. These SNRs show evidence of interaction with dense molecular clouds, from OH maser studies, and the gamma-ray emission in their directions is explained in this study as the result of pion-decay emission from the dense molecular material interacting with cosmic rays accelerated at the shocks of these remnants. 130.03D Cosmic-ray Acceleration Efficiency of the Supernova Remnants RCW 86 and SNR 0509-67.5 Eveline A. Helder1, J. Vink1 1Utrecht University, Netherlands. 2:30 PM - 2:50 PM Room 609 Since their discovery in 1912, it has been a problem to identify the main sources of Galactic cosmic rays. This is an important issue, as accelerating these particles requires an enormous amount of energy: they contribute one third to the energy density of the inter stellar medium. For decades, the main candidates for accelerating Galactic cosmic rays have been the shocks of supernova remnants. There is plenty evidence for highly energetic cosmic-ray electrons at the shock fronts of supernova remnants. However, 99% of the cosmic-ray energy is contained in cosmic-ray protons. We measured the total cosmic-ray acceleration efficiency by combining shock velocities with proton temperatures behind the shock fronts of the young supernova remnants RCW 86 and SNR 0509-67.5. We show that the temperatures are lower than expected from the shock velocities. From this study, we conclude that over 10% of the pressure behind the shock is contributed by cosmic rays. 130.04D Multi-wavelength Modeling Of SNRs: Implications On Cosmic Ray Acceleration Miguel Araya1 1Purdue University. 2:50 PM - 3:10 PM Room 609 A spectral study of non-thermal filaments is carried out with data from a deep Chandra observation of Cassiopeia A, a young supernova remnant (SNR). The diffusion model applied explains the properties observed, such as the spectral hardening going outward, and allows for an estimation of the magnetic field, level of turbulence and shock obliquity. Using these results, and combining archival data taken at radio and infrared wavelengths with state-of-the-art measurements at X-ray and gamma-ray energies, a spectral energy distribution (SED) is assembled and modeled. The non-thermal SED is explained partly with a two-zone leptonic model. Synchrotron emission from the electrons can account for data from radio to X-ray wavelengths. Much of the GeV-TeV emission can also be explained by a combination of bremsstrahlung emission and inverse Compton scattering of infrared photons. However, the model cannot fit a distinct feature at GeV energies. This feature can be well accounted for by a pion-zero emission component to the model, providing evidence for cosmic ray production in Cas A. A similar SED is assembled for Tycho's SNR. The results do not allow to conclude anything firmly, although the leptonic scenario for this case might be able to explain the data. 130.05 The Origin and Evolution of the Nonthermal Emission in Cassiopeia A Daniel Patnaude1, R. Fesen2, J. Laming3, J. Vink4 1Smithsonian Astrophysical Observatory, 2Dartmouth College, 3NRL, 4University of Utrecht, Netherlands. 3:10 PM - 3:20 PM Room 609 Cassiopeia A is one of only a handful of Galactic supernova remnants to show variations in nonthermal emission on measureable timescales. With 10 years worth of Chandra observations of Cas A, I will show how the nonthermal emission has decreased by ~ 1.5%/yr, or about twice as fast as the decline seen in the radio emission. On smaller scales, I will demonstrate that the nonthermal emission knots and filament are not uniformly distributed across the face of the remnant, with the smallest scale features localized along and interior of the so-called bright ring. This would seem to suggest that the observed short term variations are not occurring at the forward shock, but somewhere in the interior, possibly at the contact discontinuity. 131 YSO's Etc. II Oral Session Room 604 131.01 Fitting Spectral Energy Distributions of Protostars in the Taurus Star-Forming Region Jillian Tromp1, S. Terebey1, D. Padgett2, L. Rebull2, A. Noriega-Crespo2, Taurus Spitzer Legacy Team 1California State University, Los Angeles, 2Caltech, Spitzer Science Center. 2:00 PM - 2:10 PM Room 604 We present data for the brightest far-infrared objects in the Taurus star-forming region comprising a sample of eighty sources. We fit observed spectral energy distributions (SEDs) of the embedded population from the Taurus Spitzer Legacy Survey using a grid of pre-computed model SEDs. Our 70 micron flux-limited sample is above 0.6 Jy, and is comprised of 67 young stellar objects (26 Class I, 12 Flat Spectrum, 26 Class II, 3 Class III), 10 galaxies, and 3 miscellaneous objects (a planetary nebula, carbon star, and background giant). The criterion for this sample is biased toward the selection of protostars since excess emission in the far-infrared is indicative of the dust enshrouding embedded sources. Fainter 70 micron objects in the Taurus Spitzer Legacy data set are predominately background galaxies. The observed SEDs are fit using the YSO model SED grid from Robitaille et al., 2007, computed using a Monte-Carlo radiation transfer code from Whitney et al., 2003. Updated constraints on the parameters involved in low-mass star formation theory are presented. 131.02D The Characterization of Volatiles Associated with Young Stellar Objects Kari A. Wojtkowski1, E. L. Gibb1, B. A. Wilking1, S. S. Shenoy2 1Univ. Of Missouri St. Louis, 2NASA Ames Research Center. 2:10 PM - 2:30 PM Room 604 We present column densities for CO2 and H2O ice toward ~30 Young Stellar Objects (YSOs) in the Rho Ophiuchi dark cloud. We compare abundance ratios with the spatial distribution of the YSOs, their evolutionary state, and their local environment. In addition, we consider similarities and differences between the abundance ratios in Rho Ophiuchi, Taurus, and background objects in order to investigate possible differences due to regions of low mass star formation, low and high mass star formation, and the quiescent interstellar medium. While Taurus and background objects toward three dark clouds have been extensively studied (see, for example, Zasowski et al., 2009 and Whittet et al. 2009), no large study toward Rho Ophiuchi has been completed to date. However, variations in abundance ratios due to the spatial distribution of YSOs in the molecular cloud have been found. For example, Pontoppidan (2006) found an enhancement of CO2 and CO ice toward the Ophiuchus-F core, but with a sample size of five sources. Our study provides more information regarding differences in abundance ratios related to the spatial distribution of the sources by considering YSOs throughout the entire dark cloud rather than a single core. In addition, our large sample size allows a better statistical comparison with YSOs in other environments, as well as the evolutionary state of YSOs within Rho Ophiuchi. 131.03 Mid-Infrared Variability in Protoplanetary Disks with Gaps and Holes Catherine Espaillat1 1Harvard-Smithsonian Center for Astrophysics. 2:30 PM - 2:40 PM Room 604 Forming planets should interact with the surrounding accretion disk, clearing the material around themselves and leaving behind gaps in the disk. Stars with inner holes in their disks have been detected and are labeled as transitional objects. A few years ago, Spitzer identified a new class of "pre-transitional disks" which have gaps rather than holes - they have an inner disk, a gap, and an outer disk. In several cases, millimeter imaging has confirmed the presence of these cavities. Recently, we obtained multi-epoch Spitzer IRS spectra for a number of transitional and pre-transitional disks and find that infrared variability is a common phenomenon in such objects. Using sophisticated irradiated accretion disk models we explore the possible causes for such variability by comparing spectral energy distributions to the observations. The variability observed in transitional and pre-transitional disks has important implications on the structure of protoplanetary disks. 131.04D Morphological Complexity of Protostellar Envelopes: Structure and Kinematics John J. Tobin1 1Univ. Of Michigan Ann Arbor. 2:40 PM - 3:00 PM Room 604 The morphology and kinematics of infalling envelopes around protostars determine the structure of the forming protostellar disk and reflect back on the initial properties of their parent dark clouds. Axisymmetric envelopes are often used in comparison to observations due to simplicity; however, 8 micron shadow images from Spitzer show that the dense envelopes around Class 0 protostars are generally morphologically complex, often filamentary, and frequently non-axisymmetric. The observed envelope structure indicates a likely origin in turbulent cloud structure rather than a quasi-static formation and increase the likelihood of fragmentation during collapse, forming close binaries. This complex complex envelope structure is observed in regions spatially distinct from outflow cavities, and often show no systematic alignment perpendicular to the cavities. To further characterize these systems, I have observed them in the dense gas tracers N2H+, N2D+, and ammonia which closely follow the extinction morphology. The magnitude of the velocity gradients on R ~ 10000 AU scales indicates that the velocity structure, which has historically interpreted as rotation, may really be large-scale infall. Furthermore, several systems show large velocity gradients and/or linewidths near the protostar, as expected for infall or increased rotational velocity in the inner envelope. Comparisons with three-dimensional filamentary and symmetric rotating collapse models indicate that the position-velocity structure seen in many systems is better reproduced by filaments than sheets or spheres. These results strongly show that the structure of the envelope must be considered when interpreting the velocity field. 131.05 Imaged Gaps in Protoplanetary Disks as Probes of Growing Planets Hannah Jang-Condell1 1Univ. of Maryland/NASA-GSFC. 3:00 PM - 3:10 PM Room 604 As planets grow in size, they begin to dynamically clear out gaps in disks. Planets above about 30 Earth masses (0.1 Jupiter masses) can clear about half the material along their orbital paths, but until they grow in size to at least a Jupiter mass (300 Earth masses), these gaps do not significantly affect the spectral energy distribution. However, these gaps are potentially observable in spatially resolved imaging both in scattered light and in thermal continuum emission. Optical to near-infrared images trace out scattered light from the structure of the surface of the gap. Infrared to radio wavelengths trace radiative cooling and heating due shadowing of stellar illumination on the gap. I present observations of gaps in spatially resolved images of protoplanetary disks and compare them to analytical models to constrain the masses of planets that might be creating the gaps. If these gaps are indeed indicative of planet formation, the ages of the disks and locations of the gaps give a direct probe of the planet formation process. As we better understand where and when planets form, the better we can understand the distribution of exoplanet masses and orbital properties. This work was supported by the Michelson Fellowship Program, under contract with JPL and funded by NASA; JPL is managed for NASA by the California Institute of Technology. 131.06D A Search for Low Mass Stars and Substellar Companions and A Study of Circumbinary Gas and Dust Disks David R. Rodriguez1 1University of California, Los Angeles. 3:10 PM - 3:30 PM Room 604 We have searched for nearby low-mass stars and brown dwarfs and have studied the planet-forming environment of binary stars. We have carried out a search for young, low-mass stars in nearby stellar associations using X-ray and UV source catalogs. We discovered a new technique to identify ~10-100 Myr-old low-mass stars within ~100 pc of the Earth using GALEX-optical/near-IR data. We present candidate young stars found by applying this new method in the ~10 Myr old TW Hydrae and Scorpius-Centaurus associations. In addition, we have searched for the coolest brown dwarf class: Y-dwarfs, expected to appear at temperatures <500 K. Using wide-field near infrared imaging with ground (CTIO, Palomar, KPNO) and space (Spitzer, AKARI) observatories, we have looked for companions to nearby, old (2 Gyr or older), high proper motion white dwarfs. We present results for Southern Hemisphere white dwarfs. Additionally, we have characterized how likely planet formation occurs in binary star systems. While ~20% of planets have been discovered around one member of a binary system, these binaries have semi-major axes larger than 20 AU. We have performed an AO and spectroscopic search for binary stars among a sample of known debris disk stars, which allows us to indirectly study planet formation and evolution in binary systems. As a case study, we examined the gas and dust present in the circumbinary disk around V4046 Sagittarii, a 2.4-day spectroscopic binary. Our results demonstrate it is unlikely that planets can form in binaries with stellar semi-major axes of ~10s of AU. This research has been funded by a NASA ADA grant to UCLA and RIT. 132 Interstellar Medium: HII Regions Oral Session Room 608 132.01 The GBT Galactic HII Region Discovery Survey Source Catalog Thomas M. Bania1, L. D. Anderson2, D. S. Balser3, R. T. Rood4 1Boston University, 2Laboratoire d'Astrophysique de Marseille, France, 3NRAO, 4University of Virginia. 2:00 PM - 2:10 PM Room 608 The Green Bank Telescope (GBT) HII Region Discovery Survey (HRDS) has doubled the number of known HII regions in the Galactic zone 343 deg < Lgal < 67 deg with |Bgal| < 1 deg. We detected 603 discrete Hydrogen radio recombination line (RRL) components at 9 GHz (3cm) from 448 targets. Our targets were selected based on spatially coincident mid-infrared and 20 cm radio continuum emission. Such sources are almost invariably HII regions; we detect hydrogen RRL emission from 95% of our target sample. The sensitivity of the GBT and the power of its spectrometer together made this survey possible. Here we report on the HRDS catalog of the measured properties of the RRL and continuum emission from the survey nebulae. The derived survey completeness limit, 180 mJy at 9 GHz, is sufficient to detect all HII regions ionized by single O-stars to a distance of 15 kpc. These recently discovered nebulae share the same distribution on the sky as does the previously known census of Galactic HII regions. On average, however, the new nebulae have fainter continuum fluxes, smaller continuum angular sizes, fainter RRL intensities and smaller RRL line widths. Though small in angular size, many of our new nebulae show little spatial correlation with tracers associated with extremely young HII regions, implying that our sample spans a range of evolutionary states. We discovered 34 first quadrant negative-velocity HII regions, which lie at extreme distances from the Sun and appear to be part of the Outer Arm. We found RRL emission from 211 Spitzer GLIMPSE 8 micron ``bubble'' sources, 65 of which have been catalogued previously. It thus appears that nearly all GLIMPSE bubbles are HII regions and that ~50% of all Galactic HII regions have a bubble morphology at 8 microns. 132.02 Galactic Structure As Probed By The GBT HRDS Loren D. Anderson1, T. M. Bania2, D. S. Balser3, R. T. Rood4 1Laboratoire d'Astrophysique de Marseille, France, 2Boston University, 3NRAO, 4University of Virginia. 2:10 PM - 2:20 PM Room 608 Studies of external galaxies show that HII regions are excellent tracers of galactic structure. They are zero-age objects compared to the age of their host galaxy; they map the current locations of massive star formation, which trace spiral arms. Until recently the number of Milky Way HII regions with known distances was relatively small. The new GBT HII Region Discovery Survey (HRDS) has doubled the number of known first Galactic quadrant HII regions, giving us a much larger sample for Galactic structure studies. Here we report on kinematic distance determinations for HRDS sources located in the Galactic longitude range of 18° to 65°. These first quadrant sources suffer from the well known kinematic distance ambiguity (KDA): each measured recombination line velocity maps to two possible kinematic distances, a "near" and a "far" distance. We resolved the KDA for nearly 200 HRDS sources by making HI emission/absorption experiments using data from the VLA Galactic Plane Survey. The HRDS targets are nearly all at the far kinematic distance, which indicates that their small angular size is due to a large distance from the Sun rather than a small physical size. When combined with kinematic distances for the sample of previously known HII regions, the face-on map of first quadrant star forming regions shows strong evidence for Galactic structure. The map shows two spiral arc features that have mean Galactocentric radii of ~4.5 and ~6.0 kpc. Structures at these locations are generally associated with the Scutum and Sagittarius arms, respectively. The HRDS has also detected a significant number of very distant sources beyond the Solar orbit that show excellent agreement with what has been called the Outer Arm, and agree well with the warp and flaring seen in the CO and HI layers. 132.03 Metallicity Distribution in the Milky Way Disk Dana S. Balser1, R. T. Rood2, T. M. Bania3, L. D. Anderson4 1NRAO, 2University of Virginia, 3Boston University, 4Lab. d Astrophys. de Marseille, France. 2:20 PM - 2:30 PM Room 608 Galactic chemical evolution models are important for understanding how galaxies form and evolve. A key observational constraint for these models is the spatial distribution of abundances in the Galaxy. We use hydrogen radio recombination line and continuum free-free emission observed with the Green Bank Telescope to calculate electron temperatures in 81 Galactic HII regions. Since metals, such as oxygen, are the main coolants in the photo-ionized nebular gas, the electron temperature is directly related to the distribution of heavy elements in the Milky Way. We convert the electron temperatures to metallicity (12 + Log(O/H), based on a sub-sample of objects with both electron temperature and O/H determinations. We find a radial metallicity gradient in the Galactic disk of about -0.03 to -0.06 dex/kpc with no significant discontinuity from 4-18 kpc. This is in contrast to previous studies that found a discontinuity in the gradient at 10 kpc. The radial metallicity gradient varies with azimuth, however, suggesting that the Galactic disk is not uniformly mixed as is often assumed in chemical evolution models. The new GBT HRDS Galactic HII regions will sample a new zone in Galactic azimuth since they are systematically at the far kinematic distance. Electron temperature determinations for the HRDS nebulae may provide direct evidence for local enrichment. Moreover, the negative velocity HRDS sources are not only at the important Galactocentric radius zone of ~9-12 kpc, but also lie at very large distances, > 12 kpc, from the Sun. Electron temperature determinations for these nebulae will probe the metallicity of an entirely new part of the Milky Way. 132.04D What Drives the Expansion of Giant HII Regions?: A Study of Stellar Feedback in 30 Doradus Laura A. Lopez1, M. Krumholz1, A. Bolatto2, J. X. Prochaska1, E. Ramirez-Ruiz1 1UC Santa Cruz, 2University of Maryland College Park. 2:30 PM - 2:50 PM Room 608 Observations demonstrate that star formation is an inefficient and slow process. This result can be attributed to the injection of energy and momentum that prevents free-fall collapse of molecular clouds. The mechanism of this feedback is debated theoretically: possible sources of pressure include the classical warm HII gas, the hot gas generated by shock-heating from stellar winds and supernovae, direct radiation from stars, and the dust-processed radiation field trapped inside the HII shell. In this talk, I present observational measurements of the pressures associated with each component listed above in the giant HII region 30 Doradus in the Large Magellanic Cloud. For this analyses, we have used high resolution, multi-wavelength images (radio, infrared, optical, and X-ray) to map these pressures as a function of position. We find that radiation pressure dominates within 50 pc of the central star cluster, R136, while the HII gas pressure dominates at larger radii. By contrast, the dust-processed radiation pressure and hot gas pressure are generally weak and not dynamically important, although the hot gas pressure may have played a more significant role at early times. I discuss the implications of these results regarding confinement/leakage of the hot gas from the HII shell and the early dynamics of 30 Dor. 132.06 Spatially Resolved 3-micron Spectroscopy of HII Regions Erin C. Smith1, I. S. McLean2 1NASA Ames Research Center, 2UCLA. 3:00 PM - 3:10 PM Room 608 We used narrow band 3 micron emission maps of the Orion Bar, M17 and S-106 to investigate the distribution of 3.3 micron polycyclic aromatic hydrocarbon (PAH) emission with respect to K-band emission. In each HII region the prominent 3.3 micron emission was offset from or displayed a different morphology than the K band emission. In the Orion Bar PAH emission was offset by 2-3 arcseconds, in M17 the 3 micron emission exhibited distinctly shell-like morphology, and in S-106 PAH emission was bar-like in distribution. We also obtained 3-5 micron spectra of the regions with prominent 3 micron emission within each HII region using NIRSPEC at Keck Observatory. By systematically stepping the NIRSPEC slit across the regions’ extent we obtained data cubes with 2 spatial and 1 spectral dimension. Spectra at each spatial position were fitted with a series of Gaussians to measure the central wavelength, FWHM and total flux of each feature. Spatial distribution and spectral variation of the 3.3 micron hydrocarbon emission feature and its associated features at 3.4, 3.46, 3.51 and 3.56 microns were examined and compared to HeII , Pfund-gamma and Pfund-delta (Hydrogen) atomic emission. Hydrocarbon emission exhibited the same morphological variations as seen in the narrow band images. While the distribution of individual hydrocarbon features was similar, there were correlations observed between the 3.4 and 3.51 micron emission features as well as spectral variations in the 3.4 micron feature shape between the ionized and molecular regions in the Orion Bar. 132.07 Ionization Parameter: A Diagnostic of Radiation Pressure Dominated HII Regions Sherry Yeh1, C. D. Matzner1 1University of Toronto, Canada. 3:10 PM - 3:20 PM Room 608 When irradiation is sufficiently intense, the structure of an HII region will be dominated by radiation pressure and stellar winds, rather than ionized gas pressure. This state is of considerable interest because of its role in the formation of massive stars, the disruption of giant molecular clouds, and the evolution of starburst galaxies. We discuss the usefulness of the ionization parameter U, as often derived from observed line ratios between species which exist only in ionized gas, as a diagnostic for the radiation pressure-dominated state. In ionization-bounded directions, U cannot exceed a maximum value Umax determined by equilibrium between radiation and gas pressure forces. Lower values of U will occur, however, when the pressure of shocked stellar winds is significant, or when neutral gas is broken into clumps with sufficiently small radii of curvature. Applying these considerations to a prominent ionized shell around 30 Doradus and to the inner starburst region of M82, along with Cloudy simulations, we conclude that both are dominated by a combination of radiation pressure and shocked winds. 132.08 The Fifth ISM Phase as Revealed by Faraday Rotation Carl E. Heiles1 1UC, Berkeley. 3:20 PM - 3:30 PM Room 608 In the diffuse ISM, phases are classically categorized as largely ionized or neutral. The neutral phases come in two flavors, the Cold and Warm Neutral Media (the CNM and WNM), which have typical temperatures ~50 and ~5000 K. The ionized phases also come in two flavors, again classified by temperature: the Warm and Hot Ionized Media (the WIM and the HIM), which have typical temperatures ~8000 and ~106 K. There lurks a fifth phase, the Warm Partially Ionized Medium (WPIM). This is not widely recognized, mainly because it's presence is hard to establish observationally. It is well represented by the Local Interstellar Cloud (LIC), whose properties are very well specified in a series of papers by Redfield and Linsky. This fifth phase has a relatively high electron column but low emission measure, so it is not easily seen in H alpha. However, if the region is permeated by a typical magnetic field (~6 microGauss), then it can produce a recognizable signature in Faraday rotation. We show a few examples and discuss the potential for large-scale mapping of this fifth ISM phase. Support for this work was provided in part by NSF grant AST-0908572. 133 Star formation in Extragalactic Systems Oral Session Room 4C-4 133.02D The First Stars: Multiplicity, Rotation Speeds, and Feedback Athena Stacy1 1University of Texas at Austin. 2:10 PM - 2:30 PM Room 4C-4 We investigate the formation of metal-free, Population III, stars within a minihalo at z~20 with a smoothed particle hydrodynamics simulation, starting from cosmological initial conditions. Employing a hierarchical, zoom-in procedure, we achieve sufficient numerical resolution to follow the collapsing gas in the center of the minihalo up to number densities of 1012 cm-3. We then study the protostellar accretion onto the initial hydrostatic core, which we represent as a growing sink particle. We continue our simulation for 5000 yearrs after the first sink particle has formed. During this time period, a disk-like configuration is assembled around the first protostar. At the end of the simulation, a small multiple system has formed, dominated by a binary with masses 40 Msol and 10 Msol. If Pop III stars were to form typically in binaries or small multiples, the standard model of primordial star formation, where single, isolated stars are predicted to form in minihalos, would have to be modified. As these sinks grow we furthermore measure the velocities and angular momenta of all particles that fall onto these protostellar regions. This allows us to determine the angular momentum of the sinks and estimate the rotational velocity of the Pop III stars expected to form within them. We find that there is sufficient angular momentum to yield rapidly rotating stars, with velocites close to break-up speed, providing a large enough spin to potentially lead to a GRB. 133.03D Testing the Star Formation Law in Bulgeless Disk Galaxies Linda C. Watson1 1Ohio State University. 2:30 PM - 2:50 PM Room 4C-4 Recent work has provided constraints on the physics that sets the star formation efficiency in varying environments of the interstellar medium. However, a single theory for star formation has yet to stand out among its peers. I will present results from our study of the relation between the surface density of gas and star formation rate in twenty bulgeless disk galaxies using data from the VLA, IRAM 30m, MDM, and Spitzer IRAC. The general motivation for our study is to test the predictive power of current theories with substantially improved observations of late-type and low-mass disks. We specifically study star formation and the properties of the cold and warm interstellar medium above and below a circular velocity of 120 km/s (stellar mass ~ 1010 solar masses), where Dalcanton et al. (2004) found that edge-on galaxies show an abrupt transition in their dust scale heights. I will discuss the location of our low- and high-mass galaxies on the star formation law, with a focus on the scale of physical processes that affect star formation. 133.04D The HERACLES View of Molecular Gas in the Outer Disks of Galaxies Andreas Schruba1, A. K. Leroy2, F. Walter1, HERACLES team 1Max Planck Institute for Astronomy, Germany, 2National Radio Astronomy Observatory. 2:50 PM - 3:10 PM Room 4C-4 For 24 nearby spiral galaxies we combine observations of CO (HERACLES), HI (THINGS), IR (SINGS), and UV (GALEX) to study how the ISM forms stars in regions of low molecular gas surface density. The gas-to-stars conversion appears to be a two step process: 1) the formation of dense (molecular) gas from the (atomic) ISM and 2) the formation of stars from that dense phase. Distinguishing these processes requires obtaining high-significance measurements of molecular gas in low surface brightness, HI-dominated regions. We do this using a novel technique, leveraging HI velocity fields from THINGS and wide area coverage of HERACLES to stack CO spectra out to the optical radius. We find CO to decrease uniformly over all radii and scale remarkably linearly with tracers of star formation (IR and FUV). The H2-SFR relation is linear for individual galaxies and does not appear to depend on local gas surface density. However, we find systematic offsets between galaxies which dominate the scatter of the combined relation. Meanwhile, the H2-to-HI ratio varies by several orders of magnitude with radius and total gas surface density and, therefore, sensitively regulates the supply of star-forming molecular gas. 133.05 The Life and Death of Dense Molecular Clumps Around Massive YSOs in the LMC Jonathan P. Seale1, L. W. Looney2, T. Wong2, J. Ott3 1Space Telescope Science Institute, 2University of Illinois, 3National Radio Astronomy Observaory. 3:10 PM - 3:20 PM Room 4C-4 We present observations of the dense molecular clumps toward active star formation regions N105, N113, N159, and N44 in the LMC. Observations were performed with the Australia Telescope Compact Array in the 3 mm transitions of HCO+ and HCN. The observations reveal that the molecular material is clumpy, with individual clump masses between 102 and 104 solar masses and radii of <1 pc to ~2 pc. While many of the clumps are coincident with tracers of star formation, we find several to be devoid of any star formation signposts. The clumps with on-going star formation are on average 3-5 times more massive than those without, suggesting that the mass of the most massive star a clump forms may be determined by the mass of the natal clump. Moreover, we find a possible correlation between the mass of a clump and the projected distance between the clump’s center and the forming star, suggesting that as a massive star forms, it becomes displaced from the clump’s emission peak as it dissipates a significant fraction (>1/2) of the surrounding clump. We also find a number of YSOs within the imaged regions that are not associated with HCO+ or HCN emission; these YSOs have presumably destroyed their natal clumps to become evolutionarily older than those in clumps. The strength of the 10 micron silicate absorption feature seen in mid-IR spectra of YSOs is correlated with a source’s association with a molecular clump; objects within clumps have deep silicate features, while those outside clumps have features that are weak or non-existent. This correlation suggests the silicate feature is formed by material on clump-sized scales. Using a large sample of LMC massive YSO spectra, we estimate that ~60% of the YSOs detected in the LMC via their mid-IR emission are no longer located in molecular clumps. Monday, January 10, 2011, 3:40 PM - 4:30 PM 134 Pierce Prize: Dark Matter and Black Holes Over Cosmic Time Invited Session Ballroom 6AB 134.01 Dark Matter and Black Holes Over Cosmic Time Tommaso Treu1 1University of California. Ballroom 6AB The standard cosmological model successfully reproduces the properties of the universe on supergalactic scales. However, it is unclear whether it can match the detailed properties of galaxies themselves. In particular, the origin of spheroidal galaxies is currently a point of discord between observation and the standard hierarchical model. For example, the stellar populations properties and sizes of massive galaxies are difficult to reproduce by models. Surprisingly, in the past decade it has become clear that supermassive black holes might be an essential ingredient to solve this puzzle: they are found ubiquitously at the center of spheroidal galaxies and their mass correlates with global properties of the host. Furthermore my work, and that of others, has shown that global properties of spheroidal galaxies also correlate very tightly with those of their dark matter halos. A unified description of dark matter, baryons and black holes seems thus necessary to explain the observed correlations, and could perhaps reconcile the standard model with the conflicting observations. I will present highlights of my observational research program aimed at measuring the evolution over cosmic time of black holes, stars, and dark matter in spheroidal galaxies. Monday, January 10, 2011, 4:30 PM - 5:20 PM 135 Exoplanets: Misaligned, Migratory, Metallic, and Mini Invited Session Ballroom 6AB 135.01 Exoplanets: Misaligned, Migratory, Metallic, and Mini Geoffrey W. Marcy1 1UC, Berkeley. Ballroom 6AB The past year saw paradigms challenged and long-sought domains detected from Doppler, transit, microlensing, and direct imaging observations of exoplanets. The tilt of orbital planes with respect to stellar equators has been studied in over 30 planetary systems. Shockingly, they are not generally aligned, including some orbits quite tilted relative to the star's equator and a few even retrograde. These misalignments utterly contradict the accepted theory of planet migration in a gaseous protoplanetary disk, and they differ from the co-planar orbits in our own solar system. Equally puzzling, many close-in gas giants display grossly inflated radii, temperature inversions of mysterious origin, and non-equilibrium abundances of CO and methane. Meanwhile, Doppler-detected exoplanets reveal, for the first time, a rapidly rising mass function toward lower masses - all the way to 3 Earth-masses, pointing to the occurrence frequency of Earth-mass planets. The NASA Kepler Mission has discovered over 700 candidate planets, with most having diameters less than 5 times that of Earth and some as small as that of Earth. One planet has a radius, mass, and density in a new domain having no counterpart in our Solar System, opening a new chapter in planetary science. The mutual inclinations and gravitational interactions among planets measured by Kepler provide key information on the formation and evolution of planetary systems. The diversity of exoplanets continues to confound, delight, and inform us about planetary systems in general, with our Solar System being just one example. Tuesday, January 11, 2011, 8:30 AM - 9:20 AM 200 The Virgo Cluster: New Results from New Surveys Invited Session Ballroom 6AB 200.01 The Virgo Cluster: New Results from New Surveys Laura Ferrarese1 1Herzberg Institute of Astrophysics, Canada. Ballroom 6AB The Virgo Cluster contains about two thousand of cataloged galaxies orbiting within a dark halo of roughly 400 trillion solar masses. It is the most thoroughly studied cluster in the universe and has long played a key role in our understanding of how galaxies form and evolve in dense environments. At a distance of 16.5 Mpc, it also occupies a unique position in galaxy and cluster research, offering a local counterpart to the massive clusters studied at high redshift, while at the same time allowing astronomers to study analogs of the faint, low surface brightness galaxies of the Local Group in a different environment, and in far greater numbers. During recent years, several new surveys of the Virgo Cluster have been undertaken at wavelengths ranging from the x-ray to the radio. In this talk, I will briefly review these surveys and summarize some of their scientific highlights, focusing closely on what observations of the Virgo Cluster have taught us about the role of environment in galaxy evolution. Tuesday, January 11, 2011, 9:00 AM - 6:30 PM 239 Dark Energy Survey Poster Session Exhibit Hall 239.01 DECam Prototype Observations for Calibration of the Dark Energy Survey Kyler Kuehn1, Dark Energy Survey Collaboration 1Argonne National Laboratory. Exhibit Hall The Dark Energy Survey (DES) makes use of the Dark Energy Camera (DECam) to survey approximately 1/4 of the southern sky in order to observe supernovae, galaxy clusters, baryon acoustic oscillations, and weak gravitational lensing, with the ultimate goal of obtaining unprecedented constraints on the Dark Energy Equation of State. A Prototype Dark Energy Camera (PreCam) has been fully operational since September 2010, more than a year prior to the start of DES. It serves not only as a testbed for DECam hardware and software, but also as a means to make standard star calibration measurements throughout the proposed DES footprint. We describe the current status of the PreCam observations, as well as its calibration goals and expected contribution to the overall scientific output of DES. 239.02 The Dark Energy Survey Camera (DECam) and Upgrade (DESpec) H. Thomas Diehl1 1Fermi National Accelerator Laboratory. Exhibit Hall The Dark Energy Survey (DES) is a next generation optical survey aimed at understanding the expansion rate of the universe using four complementary methods: weak gravitational lensing, galaxy cluster counts, baryon acoustic oscillations, and Type Ia supernovae. To perform the survey, the DES Collaboration is building the Dark Energy Camera (DECam), a 3 square degree, 520 Megapixel CCD camera that will be mounted at the prime focus of the Blanco 4-meter telescope at the Cerro Tololo Inter-American Observatory. CCD production has finished, yielding roughly twice the required 62 2kx4k detectors. The construction of DECam is nearly finished; some components have already been received at CTIO. In addition, the DES Collaboration has been evaluating the physics prospects and design options of the Dark Energy Survey Upgrade, for which the instrument is a multi-fiber spectrometer, called DESpec. This poster will concentrate on the present status of DECam and the expected start of survey operations and show initial concepts for DESpec. 239.03 The Dark Energy Camera Data Acquisition and Control System Elizabeth J. Buckley-Geer1, J. Annis1, M. Bonati2, J. Eiting3, A. Elliot3, M. Haney4, W. Hanlon4, K. Honscheid3, I. Karliner4, K. W. Kuehn5, S. E. Kuhlmann5, S. Marshall6, A. J. Roodman6, T. Schalk7, G. Schumacher2, J. Thaler4, W. Wester1 1Fermi Nat'l Accelerator Laboratory, 2Cerro Tololo Inter-American Observatory, Chile, 3The Ohio State University, 4University of Illinois (Urbana-Champaign), 5Argonne National Laboratory, 6SLAC National Accelerator Laboratory, 7University of California, Santa Cruz. Exhibit Hall The Dark Energy Camera (DECam) data acquisition and control system is called the Survey Image System Process Integration (SISPI). Implemented as a distributed multi-processor system, SISPI consists of a set of processes that will coordinate and perform image acquisition and deliver images to the data management system for processing. Separate processes for instrument control, image building and analysis, image acquisition and observatory control are built on top of an infrastructure layer that provides message passing and communications. Additional system components include a flexible configuration system and the facility database. The command protocol is implemented in Python using a client-server design pattern derived from the SML and SCLN communications software developed at CTIO. A publish-subscribe model has been added to support the distribution of telemetry data and alarm messages. The design of the graphical user interfaces follows the Model-View-Controller approach to distinguish between the actual information and the graphical representation of the data. We will present the software architecture of the SISPI system and report on the current status of the project. 239.04 Calibration Of The Dark Energy Survey Camera: Measurements Of Focal Plane Flatness And Crosstalk Among CCDs Marcelle Soares-Santos1, J. Hao1, J. Estrada1, E. Buckley-Geer1, H. Cease1, G. Derylo1, H. T. Diehl1, B. Flaugher1, R. Flores1, K. Honscheid2, I. Karliner3, D. Kubik1, K. Kuk1, N. Kuropatkin1, H. Lin1, A. Lathrop1, J. Montes1, V. Scarpine1, K. Schultz1, L. Scott1, T. Shaw1, W. Stuermer1, W. Wester1, Dark Energy Survey 1Fermi National Accelerator Laboratory, 2Ohio State University, 3University of Illinois. Exhibit Hall DECam is an extremely red sensitive 520 Megapixel camera designed for the incoming Dark Energy Survey (DES). It is consist of sixty two 4k x 2k and twelve 2k x 2k 250-micron thick fully-depleted CCDs, with a focal plane of 44 cm in diameter and a field of view of 2.2 square degree. It will be attached to the Blanco 4-meter telescope at CTIO. The DES will cover 5000 square-degrees of the southern galactic cap in 5 color bands (g, r, i, z, Y) in 5 years starting from 2011. We present our techniques for measuring the flatness of the focal plane and the crosstalk among CCDs for theDECam. We developed an image based technique to measure the flatness by moving and matching a projected grid pattern across the focal plane. The flatness is then determined by the variation of the grid pattern. We measure the crosstalk by shotting laser spots on every CCD and look at the crosstalk on other CCDs. The results show the crosstalk are well within the DES specification. 240 Radio Sky Surveys Project with the Allen Telescope Array Poster Session Exhibit Hall 240.01 Spectropolarimetry with the Allen Telescope Array: Revealing a New Dimension Casey J. Law1, B. M. Gaensler2, G. C. Bower1, Allen Telescope Array Team 1Radio Astronomy Lab, UC Berkeley, 2University of Sydney, Australia. Exhibit Hall We present a novel analysis of the Faraday rotation properties of 37 bright, polarized radio sources. Observations with the Allen Telescope Array (ATA) cover frequencies from 1 to 2 GHz, which is sensitive to a range of Faraday rotation effects. We use RM synthesis to make the first detection of multiple RM components towards individual sources. Typically, these complexities in Faraday rotation have been treated as anomalies, but this technique reveals the true complexity of this process. Roughly a quarter of the sources studied have extra RM components with high confidence (brighter than ? 40 mJy), when observing with a RM resolution of roughly 100 rad m-2. We show that the peak RM cannot be determined more precisely than the RM beam size, but that the RMs from this work are consistent with that of earlier, narrow-bandwidth, all-sky surveys. This work also describes the polarimetry calibration procedure and that on-axis ATA observations of linear polarization can be calibrated to an accuracy of 0.2% of Stokes I. Future research directions include studying the time-dependent RM structure in Active Galactic Nuclei (AGNs) and enabling accurate, wide-area RM surveys to test models of Galactic and extragalactic magnetic fields. 240.02 The Variable Radio Sky from the Allen Telescope Array Steve Croft1, G. C. Bower1, Allen Telescope Array Team 1UC Berkeley. Exhibit Hall The Allen Telescope Array (ATA) is, among other projects, undertaking large surveys of the radio sky at 1.4 and 3.14 GHz. With its wide field of view (about 5 square degrees at 1.4 GHz), the ATA is one of the most powerful radio survey telescopes in the world. As well as quantifying variability of radio sources using many epochs of imaging, and exploring new areas of area -- depth -- cadence parameter space in the search for radio transients, we are undertaking multi-wavelength studies (e.g. simultaneous optical observations of nearby galaxy nuclei using the Kepler satellite) to better probe the physical processes driving variability. 240.03 Search for Electrostatic Discharges on Mars Imke de Pater1, M. Anderson1, A. Siemion1, D. Wertheimer1, G. C. Bower1, W. C. Barott1, Allen Telescope Array Team 1UC, Berkeley. Exhibit Hall The Allen Telescope Array was used to monitor Mars between March 8 and June 1, 2010 over a total of approximately 42 hours, for signals indicative of electrostatic discharge using a wideband signal processor developed at the Center for Astronomy Signal Processing and Electronics Research (CASPER), following the report by Ruf et al., 2009, of the possible detection of electrostatic discharge on Mars. In conjunction with the ATA, simultaneous observations were done by JPL on the Deep Space Network antenna. The 1024-channel spectrometer receives complex-baseband voltage data from the ATA beamformer, from which it computes power and spectral kurtosis of the input signal in real-time. For this experiment, the ATA beamformers, each of which delivers a 104.8 MHz bandwidth, were tuned to 3.2 and 8.0 GHz. The spectral kurtosis is calculated using the method suggested in Nita et al., 2007, using a ratio between power and power squared. Variations in the kurtosis are indicative of non-Gaussianity in the signal, which can be used to detect variable cosmic signals as well as radio frequency interference -- in particular, lightning discharge in the Martian atmosphere measurable as a variation in the kurtosis corresponding to Mars' Schumann resonance. In the presence of a Gaussian signal, the kurtosis takes on a constant value. Interference, and the non-thermal emission associated with electrostatic discharge, are non-Gaussian, and thus cause the kurtosis to deviate from the Gaussian value. The instrument and analysis were tested on a variety of known sources of non-Gaussian emission, including the Crab pulsar and a number of terrestrial sources, such as satellites, which showed appropriate deviations in power and kurtosis corresponding to radio interference, and in the case of the Crab pulsar, giant pulses. 240.04 Pulsar Observations with the Allen Telescope Array Gregory Desvignes1, Allen Telescope Array Team 1University of California Berkeley. Exhibit Hall The detection of the gravitational wave background from massive black holes mergers requires to precisely monitor an array of millisecond pulsars spread throughout the Galaxy. To achieve high precision pulsar timing of millisecond pulsars, high time resolution and wide bandwidth are required. The effects of the interstellar medium have also to be taken into account. We report here the installation of a new real-time coherent dedispersion backend at the Allen Telescope Array (ATA) in the aim of monitoring a set of strong millisecond pulsar. Currently three beamformers can provide a 72 MHz bandwidth, among two of them have independent and tunable Intermediate Frequency bands. The unique capability of the ATA to simultaneously observe pulsars at two widely spaced frequencies will contribute to a better understanding of the effects of the interstellar medium on pulsar timing. 240.05 setiQuest: Leaving the Cathedral and Embracing the Bazaar Jill C. Tarter1, A. Agrawal1, ATA SonATA Team 1SETI Inst.. Exhibit Hall We are building the setiQuest open community to involve the world in five different threads of a SETI program on the ATA. setiObs are the routine observations at the ATA, that will be the beneficiary of the other four setiQuest threads, with the resultant improvement in search speed and expansion of the classes of signals that can be detected during targeted star searches and surveys. setiCode involves publishing and improving our current SonATA code base as an open source project. setiData is a weekly program to capture, and make available through Amazon Web Services, several hours of raw data recorded from the output of one of the beamformers at the ATA. These data can be used by the community for analyses and testing of new signal processing algorithms for complex, noise-like signals with a large number of degrees of freedom, or improved algorithms for the types of narrowband, continuous or pulsed signals already identified by SonATA. setiCloud is a stack built by Cloudant, Inc. that allows access to computational and storage resources available in the Amazon Cloud for setiQuest use. setiCitizen is our attempt to use the pattern recognition capabilities of the human brain coupled with visual (and perhaps auditory) sensors to quickly find signals in noise. The intent of this citizen science project is to allow crowdsourcing signal detection in certain portions of the terrestrial microwave window that contain so many signals that SonATA cannot now complete its detection and classification tasks within the required near-real-time constraint. Patterns indicating signals that have been validated and screened against known interference will be scheduled for automatic follow up observations. The setiQuest community is being encouraged to help with the development of the tools needed for these five threads as well as utilizing the end products. 240.06 Results from the Fly’s Eye Fast Radio Transient Search at the Allen Telescope Array Andrew Siemion1, G. Bower1, M. Dexter1, G. Foster2, W. Mallard1, P. McMahon3, M. Wagner1, D. Werthimer1, Allen Telescope Array Team 1University of California, Berkeley, 2Oxford University, United Kingdom, 3Stanford University. Exhibit Hall The relatively unexplored fast radio transient parameter space is known to be home to a variety of interesting sources, including rotating radio transients (RRATs), ?-ray burst (GRB) afterglows and pulsar giant pulses. In addition, a variety of hypothesized but as yet unobserved phenomena, such as primordial black hole evap- oration (Rees, 1977), prompt emission associated with coalescing massive objects (Hansen & Lyutikov, 2008) and hyper-flares from magnetars (Popov & Postnov, 2007) have been suggested. The announcement by Lorimer et al. of the detection of a powerful (?30 Jy) and highly dispersed (DM ? 375 pc cm?3) radio pulse in Parkes multi-beam survey data (Lorimer et al., 2007), and subsequent consternation, have demonstrated both the potential utility of bright radio pulses as probes of the ISM and IGM, as well as the need for wide-field surveys characterizing the fast radio transient population. We present results from the 450-hour Fly’s Eye survey for powerful dispersed radio pulses at the Allen Telescope Array (ATA). The Fly’s Eye spectrometer processes 44 independent signal paths, each with a bandwidth of 209 MHz centered at 1420 MHz, and produces 128-channel power spectra accumulated for 0.6ms. Independent antenna-pointings of the extant 42-dish ATA yields a maximum total field-of-view of approximately 198 square degrees. 240.07 Coordinated Radio and High-Energy Observations of Cygnus X-3 with the Allen Telescope Array Peter K. G. Williams1, G. C. Bower1, J. A. Tomsick1, Allen Telescope Array Team 1UC Berkeley. Exhibit Hall The microquasar Cygnus X-3 is one of the few Galactic sources known to produce relativistic jets and can be one of the brightest radio sources in the Galaxy when flaring. In late 2009 it became the first such system to be seen in the gamma-ray regime with detections by both AGILE and Fermi. We have observed Cyg X-3 at 3 GHz every ~5 days for the past six months with the Allen Telescope Array in conjunction with space-based X-ray (INTEGRAL, RXTE) and gamma-ray (Fermi) observations. We present results from both the long-term dataset and intensive observing sessions in which we obtain the radio lightcurve of Cyg X-3 on ~10-minute timescales. We focus particularly on a May 2010 minor flare event for which we have coverage in all three bands.The first phase of the ATA was funded through generous grants from the Paul G. Allen Family Foundation. UC Berkeley, the SETI Institute, the National Science Foundation (Grant No. 0540599), Sun Microsystems, Xilinx, Nathan Myhrvold, Greg Papadopoulos, and other corporations and individual donors contributed additional funding. 241 The Milky Way, The Galactic Center Poster Session Exhibit Hall 241.01 The GALFA-HI Survey: Feeding the Disk via Stellar Feedback Mary E. Putman1, J. Peek1, D. Saul1, J. Grcevich1, A. Begum2, K. Douglas3, S. Gibson4, C. Heiles5, E. Korpela5, M. Lee2, S. Stanimirovic2 1Columbia University, 2UW-Madison, 3University of Exeter, United Kingdom, 4Western Kentucky University, 5UC-Berkeley. Exhibit Hall The contribution of future star formation fuel to a galaxy from evolved stars remains uncertain. We present a correlation of discrete clouds of HI gas with evolved variable stars and find a number of cases where stellar mass-loss is likely to have created the cloud. The results of this study impact our understanding of both stellar outflows and galactic gas recycling. This research was partially funded by NSF grant AST-0917810. 241.02 The GALFA-HI Survey: Transition from HI to H2 Caught in Action in the Perseus Molecular Cloud Min-Young Lee1, S. Stanimirovic1, A. Leroy2, K. Douglas3, J. Di Francesco4, S. Gibson5, L. Knee6, R. Plume7, A. Begum1, J. Grcevich8, C. Heiles9, E. Korpela9, J. Peek8, N. Pingel1, M. Putman8, D. Saul8 1University of Wisconsin-Madison, 2NRAO, 3University of Exeter, United Kingdom, 4Herzberg Institute of Astrophysics, Canada, 5Western Kentucky University, 6Atacama Large Millimeter Array, Chile, 7University of Calgary, Canada, 8Columbia University, 9University of California-Berkeley. Exhibit Hall The conversion of atomic gas into molecular gas is a critical process for star formation. Yet, a deep understanding of fundamental agents that control the ratio of atomic to molecular gas in molecular clouds has not been achieved. Recently, Krumholz et al. (2009) provided theoretical predictions for the ratio of atomic to molecular gas in galaxies as a function of galactic properties (total gas column density and metallicity). We test the Krumholz's predictions on sub-parsec scales by investigating the ratio of atomic to molecular gas across the Perseus molecular cloud. We estimate the dust column density using the IRIS 60 and 100 micron maps and derive the H2 column density from the excess of infrared emission relative to the HI column density. Using the HI data from the GALFA-HI Survey, we derive the map of RH2 (H2 surface density / HI surface density) for Perseus. Our comparison of observational data with the Krumholz's predictions shows that the model reasonably well describes RH2 as a function of total gas column density even at sub-parsec scales. We compare RH2 for several star-forming and dark clouds in Perseus to investigate the role of interstellar radiation field in molecule formation. This research was partially funded by the NSF grant AST-0707679 and the Research Corporation for Science Advancement. 241.03 The GALFA-HI Survey: Extracting New Clouds From a Complex Medium Destry R. Saul1, J. E. G. Peek1, J. Grcevich1, M. E. Putman1, C. Heiles2, S. Stanimrovic3, E. J. Korpela4, K. A. Douglas5, M. Lee3, S. J. Gibson6, A. Begum3, A. R. H. Brown1, B. Burkhart3, E. T. Hamden1, N. M. Pingel3, S. Tonnesen1 1Columbia University, 2UC Berkeley, 3University of Wisconsin, 4Space Sciences Laboratory, UC Berkeley, 5University of Exeter, United Kingdom, 6Western Kentucky University. Exhibit Hall We present a new catalog of compact, isolated neutral hydrogen clouds extracted from the first GALFA-HI data release. With ~4' spatial resolution, 0.18 km/s spectral resolution, and a 80mK noise level per 1 km/s channel, the GALFA-HI survey provides a new view of neutral Galactic hydrogen. To identify isolated clouds, we developed a new algorithm based on a difference of gaussians wavelet. Our algorithm was tuned to specifically search for clouds smaller than 20', velocity widths of less than 20 km/s, and with absolute velocities less than 700 km/s. Thousands of clouds were detected. These may be new dwarf galaxies, high velocity clouds, disk-halo clouds, or some other exotic object. We will highlight the distribution and other properties of this new population and explain our methods in detail. This research was partially funded by NSF grant AST-0917810. 241.04 The GALFA-HI Survey: From Pretty Images To Quantifying Interstellar Inhomogeneities Snezana Stanimirovic1, A. Begum1, K. A. Douglas2, S. J. Gibson3, J. Grcevich4, C. Heiles5, M. Lee1, E. J. Korpela5, J. Peek4, M. Putman4, N. M. Pingel1, D. Saul4 1UW-Madison, 2Univ. of Exeter, United Kingdom, 3Western Kentucky University, 4Columbia University, 5UC-Berkeley. Exhibit Hall Understanding the origin and nature of interstellar inhomogeneities in galaxies is a crucial step toward inclusion of realistic high-density regions in numerical simulations. Yet, driving sources and modes of interstellar turbulence -- an important ingredient for formation and evolution of interstellar structure -- have largely been unexplored even in the Galaxy. We use data products from the GALFA-HI survey in conjunction with results from recent numerical simulations to study the level of interstellar turbulence and make connections with the dominant underlying energy sources across different Galactic environments. The GALFA-HI survey has been mapping the Galactic neutral hydrogen (HI) distribution using the the Arecibo Observatory, the largest single-dish radio telescope in the world. The unsurpassed combination of sensitivity, resolution, and mapping speed of this survey result in stunning images of the Galaxy with high spatial and velocity dynamic range perfectly suited for studying the origin and nature of interstellar inhomogeneities. This research was partially funded by the NSF grant AST-0707679 and the Research Corporation for Science Advancement. 241.05 The GALFA-HI Survey: Probing the Anatomy of Galactic Neutral Hydrogen Nickolas Pingel1 1University of Wisconsin-Madison. Exhibit Hall The Galactic HI survey with the Arecibo L-band Feed Array (GALFA-HI) is observing the whole Arecibo sky (about 13,000 square degrees), with high angular (3.5 arcmin) and velocity resolution (0.2 km s-1). The unprecedented angular and velocity resolution allow studies of the Galactic gaseous disk, halo, and the flow of material between them. The survey operates mainly commensally with other ALFA surveys, saving thousands of hours of telescope time. The 7-beam feed array ALFA is tuned to the hyperfine transition of HI at 1420.405 MHz, and a specially developed method the Least-Squares Frequency Switching is used for bandpass fitting. The survey uses a combination of basket-weave and drift observing modes, and the final data products are in the form of RA x Dec x Velocity data cubes. From these cubes we can create detailed images of the Galactic HI, and other galaxies. The reduced data are released publicly at http://sites.google.com/site/galfahi/data. We present the current survey and data release status and examples of GALFA-HI images in different visualization modes. This research was partially funded by the NSF grant[[Unsupported Character - 
]]AST-0707679 and the Research Corporation for Science Advancement. ---------------------- N. Pingel1, S. Stanimirovic, A. Begum1, K. A. Douglas2, S. J. Gibson3, J. Grcevich4, C. Heiles5, M. Lee1, E. J. Korpela5, J. Peek4, M. Putman4, D. Saul4 1UW-Madison, 2Univ. of Exeter, United Kingdom, 3Western Kentucky University, 4Columbia University, 5UC-Berkeley. 241.06 The GALFA-HI Survey: Searching for Undiscovered Local Group Dwarf Galaxies with HI Jana Grcevich1, D. Saul1, J. E. G. Peek1, M. Putman1, A. Begum2, K. Douglas3, S. J. Gibson4, C. Heiles5, E. J. Korpela5, M. Lee2, S. Stanimirovic2 1Columbia University, 2University of Wisconsin, 3University of Exeter, United Kingdom, 4Western Kentucky University, 5University of California. Exhibit Hall We present a list of candidates for previously undiscovered dwarf galaxies selected from a catalog of compact, isolated neutral hydrogen clouds identified in the GALFA-HI survey (Saul et al. 2010, in prep.). Clouds were scored based on how well their observational characteristics matched those of known Local Group dwarf galaxies, and in particular the characteristics of the only known ultra-faint galaxy to contain HI, Leo T. Follow-up observations will be conducted for the highest scoring dwarf candidates to determine if an associated stellar population exists. This research was partially funded by NSF grants AST-0917810 and AST-0904059. 241.07 Multiwavelength Observations of the Most Massive Stellar Clusters in the Galaxy Emily Richards1, C. C. Lang1, C. Trombley2, D. F. Figer2, HST/NICMOS GC Paschen Alpha Team 1University of Iowa, 2Rochester Institute of Technology. Exhibit Hall The Galactic Center Arches and Quintuplet stellar clusters are two of the most luminous clusters in the Galaxy. These massive clusters produce high rates of ionizing photons and powerful winds which sculpt the surrounding interstellar medium (ISM) and form the Sickle and Arched Filaments HII regions. Recently, these clusters and HII regions have been studied in high resolution by Spitzer, Chandra and HST/NICMOS. Here we present a multiwavelength analysis of the interaction between the clusters and the ISM. Throughout the Galaxy, only a handful of similarly luminous and massive clusters are known. It is likely that other such clusters reside in our Galaxy but are obscured from optical detection. Using data from infrared and radio surveys, 40 candidate massive clusters have been identified. We have followed up on the interstellar environment of six candidate clusters using the VLA at 8.5 and 4.9 GHz. Parameters such as the Lyman continuum flux, electron density, and total ionized mass can be determined from these radio observations and can provide estimates of the stellar content in the candidate clusters. Finally, comparison between the radio and infrared (Spitzer) data will lead to a more complete understanding of the interaction between the stellar clusters and the ISM. This material is based upon work supported by the National Science Foundation under Grant Number 0907934. The authors also acknowledge support from the University of Iowa. 241.08 Small Scale Filamentation in the Galactic Center at 5 GHz: A VLA Survey Jared Moon1, C. C. Lang1, J. Lazio2 1University of Iowa, 2Jet Propulsion Lab. Exhibit Hall We present a survey of the central 200 pc of the Galactic Center made with the VLA at 5 GHz in total and polarized intensity. A catalog of extended and compact sources is presented. The main scientific aim is to determine whether numerous linear radio filamentary structures detected both here and previously (by Nord et al. 2004 and Yusef-Zadeh et al. 2004) are in fact non-thermal in nature. Detections of filaments in polarized intensity are shown as well as spectral indicies based on multifrequency data (a recent 1.4 GHz survey of this region by Lang et al. (2010)). Better understanding the nature of these non-thermal filaments provides important insight into the nature of the magnetic field in the Galactic Center. Finally, we compare some of our 5 GHz sources to counterparts discovered in the HST/NICMOS Paschen Alpha Survey of the Galactic Center. This material is based upon work supported by the National Science Foundation under Grant No. 0907934. 241.09 The Shape and Profile of the Galactic Halo as Seen by CFHT LS/b> Branimir Sesar1, M. Juric2, Z. Ivezic3 1Caltech, 2Harvard Smithsonian Center for Astrophysics, 3University of Washington. Exhibit Hall One of the key goals of Galactic structure studies is to map the distribution of stars in the Galaxy. We use Canada-France-Hawaii Telescope Legacy Survey (CFHTLS) data, recalibrated and transformed to the Sloan Digital Sky Survey ugri photometric system, to study the distribution of near-turnoff main sequence stars in the Galactic halo along four lines of sight and to distances of ~35 kpc from the Sun. We find that the halo number density profile becomes steeper at Galactocentric distances greater than Rgal ~ 28 kpc, with the power law index changing from ninner = -2.6 to nouter = -3.8. The oblateness of the halo is q = 0.70 and shows no evidence of change across the range of probed distances. The Sagittarius stream is detected in the l = 173 deg and b = -62 deg direction as an overdensity of [Fe/H] ~ -1.5 dex stars at Rgal ~ 32 kpc, and provides a new constraint for the Sagittarius stream and dark matter halo models. The Monoceros stream is also detected, as an overdensity of [Fe/H] > -1.5 dex stars in the l=232 deg and b = 26 deg direction with Rgal < 25 kpc. In two sightlines where we do not detect significant substructure, the median metallicity is found to be independent of distance within systematic uncertainties ([Fe/H] ~ -1.5 with 0.2 dex of uncertainty). 241.10 A Kinematic Asymmetry and Interaction with the Galactic Bar Roberta M. Humphreys1, T. C. Beers2, J. E. Cabanela3, S. Grammer1, J. A. Larsen4, Y. Lee2 1Univ. of Minnesota, 2Michigan State University, 3Minnesota State University Moorhead, 4U.S. Naval Academy. Exhibit Hall The Thick Disk and Inner Halo stars in Quadrant I (Q1) have a significant over-density or star count excess compared to similar stars in the complementary fields in Quadrant 4 which extend to 5 kpc along the line of sight. The Thick Disk stars in Q1 have a much slower effective rotation rate compared to the corresponding Q4 stars (Parker et al 2004). We have greatly expanded the kinematic data with radial velocities and derived metallicity parameters for over 4000 stars. We confirm the corresponding kinematic asymmetry, extended to greater distances and with more spatial coverage. The Thick Disk stars in Q1 have a rotational lag of 60 -- 70 km/s relative to circular rotation, and the Metal-Weak Thick Disk stars have an even greater lag of 100 km s. Both lag their corresponding populations in Q4 by approximately 30 km/s. Interestingly, the Disk stars in Q1 also appear to participate in the rotational lag by about 30 km/s. The enhanced rotational lag for the Thick Disk in Q1 extends to 4 kpc or more from the Sun. At 3 to 4 kpc, our sight lines extend above the density contours on the near side of the bar, and as our lines of sight pass directly over the bar the rotational lag appears to decrease. This is consistent with a ``gravitational wake''induced by the rotating bar in the Disk which would trap and pile up stars behind it. We conclude that a dynamical interaction with the stellar bar is the most probable explanation for the observed kinematic and spatial asymmetries. This work was supported by the National Science Foundation. 241.11 The Genesis of the Milky Way's Thick Disk via Stellar Migration Sarah Loebman1, R. Roskar1, V. P. Debattista2, Z. Ivezic1, T. R. Quinn1, J. Wadsley3 1University of Washington, 2Jeremiah Horrocks Institute, University of Lancashire, United Kingdom, 3McMaster University, Canada. Exhibit Hall The separation of the Milky Way disk into a thin and thick component is supported by differences in kinematics and metallicity. These differences have lead to the predominant view that the thick disk formed early via a cataclysmic event and constitutes fossil evidence of the hierarchical growth of the Milky Way. We show here, using N-body simulations, how a double vertical structure, with stellar populations displaying similar dichotomies can arise purely through internal evolution. Stars migrate radially, while retaining nearly circular orbits, as described by Sellwood & Binney (2002). As stars move outwards their vertical motions carry them to larger heights above the mid-plane, populating a thickened component. Such stars found at present time in the solar neighborhood formed early in the disk’s history at smaller radii where stars are more metal-poor and ?-enhanced, leading to exactly the properties observed for thick disk stars. Classifying stars as members of the thin or thick disk by either velocity or metallicity leads to an apparent separation in the other property as observed. This scenario is supported by the SDSS observation that stars in the transition region do not show any correlation between rotation and metallicity. Such a correlation is present in young stars and arises because of epicyclic motions but migration radially mixes stars, washing out the correlation. Using the Geneva Copenhagen Survey, we indeed find a velocity-metallicity correlation in the younger stars and none in the older stars. We predict a similar result when separating stars by [?/Fe]. The good qualitative agreement between our simulation and observations are remarkable because the simulation was not tuned to reproduce the Milky Way, hinting that the thick disk may be dominated by stellar migration. Nonetheless, we cannot exclude that some fraction of the thick disk is a fossil of a past more violent history. 241.12 The Bulge Radial Velocity Assay: New Observations and Results Andrea M. Kunder1, R. de Propris1, M. Rich2, A. Koch3, C. Howard4, C. I. Johnson2, W. Clarkson2, R. Mallery2, J. Kormendy5, A. C. Robin6, R. Fux7, R. B. David2, H. Zhao8, K. Kuijken9, A. Pipino10, J. Shen5 1Cerro Tololo Inter-American Observatory, Chile, 2UCLA, 3Cerro Tololo Inter-American Observatory, Netherlands, 4NASA Ames Research Center, 5University of Texas at Austin, 6Observatoire de Besancon, Institut Utinam, France, 7Observatoire de Geneve, Universite de Geneve, Switzerland, 8University of St. Andrews, United Kingdom, 9University of Leicester, Netherlands, 10ETH Zurich, Switzerland. Exhibit Hall The Bulge Radial Velocity Assay (BRAVA) is a large scale spectroscopic survey of the stellar radial velocities of M-type giants whose population membership in the bulge is well established. To date, ~4500 radial velocities from the CTIO 4m Hydra multi-object spectrograph have been obtained. Here we discuss ~4500 additional radial velocity observations taken to sample the kinematics the bulge major axis at -10 1 Gyr) and young stars (~ 6 Myr). Recently, using laser guide star adaptive optics in conjunction with integral-field spectroscopy, it has been possible to distinguish between two populations to study their distribution and kinematics separately. The radial profile for the old stars was found to be significantly flatter than predicted by theories of stellar cusp formation around massive black holes. Based on number counts alone, it is unclear whether there is a ‘hole’ in the distribution of old stars at the center or if the space density of stars is constant. Distinguishing between these two scenarios will be important to constrain the range of models of cusp depletion. Here, we report on the results of a radial extension of our previous spectroscopic survey out to ~0.5 pc from Sgr A*, doubling the number of spectroscopically identified late-type giants. With the addition of astrometry, we are able to obtain 3D velocities for these stars, and in some cases, acceleration measurements. We are able to place better constraints on the three-dimensional profile of the cluster core than is possible with number counts alone. This survey also results in newly detected young, faint, B-stars along the plane of the young stellar disk at the Galactic center; significantly more stars were found than expected based on the previously observed luminosity function in this region. We also find that the radial profile of the surface density of young stars along the disk plane is flatter than was found in previous studies that sample largely perpendicularly to the disk plane. 241.19 Gamma-ray Constraints on Cosmic Rays in Galactic Winds Kaiqi Hu1, J. E. Everett1, E. G. Zweibel1 1University of Wisconsin-Madison. Exhibit Hall Our group is constructing a hybrid thermal gas and cosmic-ray pressure driven wind model. This model is built on past work by Breitschwerdt et al. (1991) and Zirakashvili et al. (1996), and was motivated by unexplained high latitude Galactic X-ray emission observed by ROSAT, and further tested with radio synchrotron observations. In this poster, the role of cosmic-ray protons in generating gamma-ray emission in a Galactic wind is explored. In interacting with the wind plasma, cosmic-ray protons have three mechanisms to generate gamma-rays (pion production, Bremsstrahlung, and inverse Compton scattering), which can be detected by the Fermi Gamma-ray Space Telescope. To test the model, we have calculated the gamma-ray intensity from the wind model of Everett et al (2010), and we compare these predictions to the observed emission in the central Milky Way. Also, we have recently developed a new wind model which includes an azimuthal magnetic field and galactic rotation; we compare the driving in this improved model to the previous one, and report on the gamma-ray emissivity of this model as well. In the future we will apply this model to other galaxies which are observed to have a large scale wind, such as M82 and NGC 253. Understanding the high latitude gamma-ray emission from relativistic particles in galactic winds may help to constrain dark-matter models as well. This work has been supported by NASA through grant NNX10AO50G, and by the NSF through grants NSF AST-0907837 and NSF PHY-0821899 (to the Center for Magnetic Self-Organization in Laboratory and Astrophysical Plasmas). 242 Stars, Cool Dwarfs, Brown Dwarfs Poster Session Exhibit Hall 242.01 Abundances of Stars with Planets- Trends with Condensation Temperature Simon C. Schuler1, J. R. King2, L. Ghezzi3, K. Cunha1, V. V. Smith1 1NOAO, 2Clemson University, 3Observatório Nacional, Brazil. Exhibit Hall We present the abundances of 18 elements for 10 stars with Jovian-mass planets based on high-resolution, high-S/N spectroscopy obtained with the 9.2-m Hobby-Eberly Telescope (HET) and the 2.2-m MPG/ESO telescope at La Silla observatory. Stellar parameters have been derived spectroscopically and are in good agreement with previous determinations. The abundances are compared to condensation temperatures (Tc) of the elements, and the possible connection between Tc-dependent abundance trends and the presence of planets is discussed. 242.02 ACCOLADES: Astrometric Changes in Column Overlaps for Low-mass Archaic Dwarfs Espied in SDSS Andrew A. West1, J. J. Bochanski2, A. J. Burgasser3, J. K. Faherty4 1Boston University, 2Penn State, 3U.C. San Diego, 4AMNH. Exhibit Hall We present preliminary results from ACCOLADES, a study of high proper motion, low-mass dwarfs, identified from two-epoch photometric observations in SDSS. The chip gap geometry in the SDSS photometric camera required that a small amount of each CCD column be imaged twice to ensure full spatial coverage in a given SDSS stripe. Occasionally, these overlapping regions were imaged months or years apart. Therefore, a subset of the SDSS catalog can be mined to produce accurate proper motions for stars that fall within these overlap regions. We selected a sample of late-M and L type dwarfs identified in these regions with time baselines longer than 1 year and conducted a spectroscopic follow-up campaign to compute 3D space motions. We present the spectroscopic analysis of our ACCOLADES sample and examine the utility of using this data mining method to identify low-mass components of the Galactic stellar halo. 242.03 Sizing Up the Stars Tabetha S. Boyajian1, K. von Braun2, G. van Belle3, H. McAlister1, M. López-Morales4, T. Henry1, G. Schaefer1, R. White1, S. T. Ridgway5, D. Ciardi2, T. ten Brummelaar1, L. Sturmann1, J. Sturmann1, N. Turner1, C. Farrington1, P. Goldfinger1 1Georgia State University / CHARA, 2NexScI/Caltech, 3ESO, Germany, 4Carnegie / DTM, 5NOAO. Exhibit Hall This work focuses on determining the fundamental properties of nearby, main sequence, A, F, G, K, and M-type stars. We present the results of angular diameters (average error ~1.5%) obtained via interferometric observations made with the CHARA Array. These measurements combined with HIPPARCOS and ground-based parallaxes and bolometric fluxes provide an empirical determination of their effective temperatures, linear radii, and absolute luminosities. We derive empirically based relations for the stellar effective temperature for these types of stars, which are accurate to the 1% level. Additionally, the masses and ages of the A, F, and G stars are determined by fitting the CHARA-determined temperatures, radii, and luminosities to Yonsei-Yale model isochrones, and we compare these results to those obtained by indirect methods. We show that for most cases the theoretical stellar radii for stars >1.3 Msun and <0.65 Msun are too small compared to observed radii by 5% and 15%, respectively (and temperatures too hot by 2% and 7%, respectively). For the early-type stars, these overestimated temperatures and underestimated radii appear to cause an additional offset in the star’s surface gravity measurements, which consequently yield higher masses and younger ages. Furthermore, we elaborate on these discrepancies seen for the late-type stars where the onset of convection plays a significant role in determining the model radii for these stars. 242.04 Discerning Spectral Features in L Dwarfs Alejandro Nunez1, K. Cruz2, A. J. Burgasser3, J. D. Kirkpatrick4, I. N. Reid5 1CUNY Hunter College, 2CUNY Hunter College & AMNH, 3University of California at San Diego, 4Caltech/IPAC, 5STScI. Exhibit Hall Brown dwarfs are star-like objects that, due to their very low masses (less than 75 Jupiter masses,) never reach the main sequence, and instead cool with time. This cooling leads to a breakdown of the relationship between temperature and mass that exists for stars. Therefore, brown dwarfs with similar temperatures (as indicated by spectral type) could have very different masses and ages. We are investigating the near-infrared spectra of L dwarfs with the same optically derived spectral types (implying similar effective temperatures) with the goal of distinguishing subtle differences, patterns, and/or correlations among absorption features that could reveal information about their ages and masses. Our sample consists of 43 L0-L8 dwarfs with both optical and near-infrared spectra, thus covering the 0.65 to 2.4-micron range. Our analysis included objects with either “typical” or peculiar spectra. Some of the objects with peculiar spectra are suspected low-gravity/young and blue/low-metallicity dwarfs. For each optical type, we normalized and overplotted the spectra in four bands separately: Optical, J, H, and K band. Each resulting plot was examined by eye to look for subtle differences in spectral absorption features, likely due to age and mass. We present the preliminary results from this detailed spectral analysis. In particular, our analysis reveals the major spectral differences in the near infrared of both “red” and “blue” L dwarfs. This work was funded by the RISE Grant GM R25 6066, and we acknowledge the hospitality of the American Museum of Natural History. 242.05 RECONS Reaches to 25 Parsecs Todd J. Henry1, M. R. Boyd2, S. B. Dieterich3, C. T. Finch4, P. A. Ianna5, W. Jao3, A. R. Riedel3, J. P. Subsavage6, A. M. Tanner3, J. G. Winters3 1RECONS, 2RECONS / GaTech, 3RECONS / GSU, 4RECONS / USNO, 5RECONS / U. Virginia, 6RECONS /CTIO. Exhibit Hall RECONS (Research Consortium on Nearby Stars, www.recons.org) is expanding its careful reconnaissance of the solar neighborhood from the original 10 parsec core sample to 25 parsecs. The resulting RECONS Database will expand the number of stellar systems for which we have detailed observations (astrometry, photometry, spectroscopy) and derived information (metallicity, multiplicity, exoplanets) from about 250 systems to 4000-6000 systems. Here we outline the new-and-improved 25 parsec sample, significantly updated from the NStars effort of a decade ago. To date, only 2000 systems have trigonometric parallaxes placing them within 25 parsecs, with more than 10% contributed by the RECONS effort at CTIO. In fact, an accurate estimate of the expected population is elusive, as new systems are being found as close as 4 parsecs, making extrapolations to 25 parsecs highly uncertain. We look forward to upcoming contributions made to the census by RECONS, SkyMapper, Pan-STARRS, LSST, and Gaia, and discuss how each of these efforts will play a role. During the next decade, census work is important because of surging interest in the nearest stars --- our stellar neighbors will offer the best answers to such fundamental questions as "What types of stars really populate the Galaxy?", "How many planets orbit nearby stars?", and "Is there life on any of those planets?" This work is currently supported by the NSF under AST 09-08402. 242.06 Stellar Diameters and Limb-Darkening with Extreme Precision: Coherent Integration with the Navy Prototype Optical Interferometer Anders M. Jorgensen1, T. Hall1, D. Paiton1, H. R. Schmitt2, J. T. Armstrong2, D. Mozurkewich3, E. K. Baines2, R. B. Hindsley2, D. Hutter4, S. R. Restaino2, B. Curtis1, M. Brown1 1New Mexico Tech, 2Naval Research Laboratory, 3Seabrook Engineering, 4Naval Observatory, Flagstaff Station. Exhibit Hall We will present three stellar diameters measurements in which we use coherent integration of data from the Navy Prototype Optical Interferometer. Coherent integration is a post-processing technique which corrects for atmospheric optical-path-difference shifts in interferometric data and allows, effectively, to increase the integration time of optical interferometric data indefinitely by summing many short exposures suitably shifted. This is significant because coherent integration, which allows the complex visibilities to be summed in phase, greatly improves the signal-to-noise ratio over traditional techniques which average squared visibilities. The improvement is particularly dramatic for faint targets, and/or when the visibility amplitude is very small. This is important when measuring stellar diameters on resolving baselines that include visibility nulls. Those baselines best constrain the diameters. However in order to take full advantage of the null as a diameter measure it is necessary to obtain high-SNR measurements around the null, which is possible with coherent integration. We will present observations of three stars for which coherent integration has been used to measure the visibility near the null very precisely. We will then fit these visibilities to uniform disk and limb-darkened visibility models to obtain extremely high precision diameters (1:500 to 1:1000) and limb-darkening parameters. 242.07 Measuring the Masses of the Most Massive Stars Philip Massey1, K. Neugent1, N. Morrell2, L. Penny3, D. R. Gies4, K. Eastwood5 1Lowell Obs., 2Las Campanas Observatory, Chile, 3College of Charleston, 4Georgia State Univ., 5Northern Arizona University. Exhibit Hall The relationship between mass and luminosity is poorly determined for high mass stars, with stellar atmosphere analysis often yielding lower estimates of the masses than stellar evolutionary models predict. For the hottest massive stars in the Magellanic Clouds such differences can be as much as a factor of two. This "mass discrepancy" problem has been known for 15 years. During this time the physics of both the stellar atmosphere and stellar evolutionary models has improved considerably, but the problem still remains with us. We've concluded that resolving this discrepancy requires an observational approach. We have been determining the masses of the highest mass stars directly from Kepler's 3rd law using massive eclipsing binaries, and comparing these to what is predicted by stellar evolutionary tracks. To identify the sample, we have used four years of intensive queue observations on the SMARTS Yale and LCO Swope 1.0-m telescope. This photometry has allowed us to pick out appropriate systems, whose light-curves and periods indicate a good chance that the components are not interacting, and that the results will be representative of single stars. Follow-up spectroscopy has been carried out on the Magellan 6.5-m Baade and Clay telescopes using IMACS and MagE, respectively. We present our preliminary results here. This work has been funded in part through the National Science Foundation (AST-0506577) and NASA (HST GO-10612). 242.08 The Young Solar Analogs Project Christopher J. Corbally1, R. O. Gray2, J. M. Saken2 1Vatican Observatory, 2Appalachian State Univ.. Exhibit Hall Since 2007 we have been monitoring the Ca II K chromospheric emission of a set of 23 young solar analogs (YSA). These stars, carefully selected from the Nearby Stars database (Gray et al. 2003, 2006), have spectral types between F8 and K2, and ages between 300 Myr and 1.5 Gyr. The goal of this project is to learn more about the sun-earth environment at a time, about 3.8 billion years ago, when life was gaining a foothold on the young earth. Of particular interest are the characterization of long-term stellar activity cycles, the determination of rotational periods, and the detection of short-term phenomena such as stellar flares. Spectroscopic observations began in 2007, and just recently we have added a simultaneous multi-band photometric component to the project. We will present preliminary results from the project, and discuss future developments to the program. 242.09 Searching for Wide Low-Mass Tertiary Companions to Binary Star Systems Stephanie Douglas1, P. Allen1 1Frankin & Marshall College. Exhibit Hall We will present the results from common proper motion searches for wide low-mass stellar and sub-stellar companions to known tight binary systems. Observations were made with the 4m telescope at KPNO and the 31" NURO telescope at Lowell Observatory. The binary systems observed at KPNO are spectroscopic binaries, while the systems targeted at NURO are unresolved or partially resolved white dwarf-M dwarf binaries. We are testing recent simulations of star formation that predict that tight binary systems form by transferring angular momentum to a lower mass third companion. Any genuine companions will be able to serve as 'benchmark' low-mass stars and brown dwarfs. The central binary, particularly the white dwarfs, will allow us to estimate independent values of age and metallicity for the wide, low-mass companion. The candidates are primarily selected using astrometry, and then the list is refined with photometry. We present the candidate companions we have found to date and the future plans for this project. 242.10 A Photometric Survey of Ori OB1b Allison T. Merritt1, W. Sherry2 1University of California, Berkeley, 2University of Arizona. Exhibit Hall Several mechanisms have been suggested to describe the formation of sub-stellar mass objects (SSMOs), specifically brown dwarfs. Each proposed mechanism predicts a unique spatial distribution of the brown dwarfs relative to the O and B stars of the association. We have 9 square degrees of optical (VRI) data and 7 square degrees of NIR (JHK) data of Orion OB1b. The purpose of the survey is to obtain the photometric data that will allow us to determine the spatial distribution of brown dwarfs in this region and constrain the various formation theories. We present an overview of the survey, with an emphasis on the NIR data, as well as color-magnitude diagrams. This research was supported by the NOAO/KPNO Research Experiences for Undergraduates (REU) Program which is funded by the National Science Foundation Research Experiences for Undergraduates Program and the Department of Defense ASSURE program through Scientific Program Order No. 13 (AST-0754223) of the Cooperative Agreement No. AST-0132798 between the Association of Universities for Research in Astronomy (AURA) and the NSF. 242.11 Spectroscopic Classification of 3,717 Nearby M Stars Naomi Alpert1, S. Lepine2 1Vassar College, 2American Museum of Natural History. Exhibit Hall Collected spectra of nearby stars are used to identify and classify M-Dwarfs according to temperature and metallicity. The stars examined are all located within approximately 50 parsecs of our Sun and were selected from the LSPM-north proper motion catalog. The spectra were collected over dozens of observing runs from telescopes at MDM, Lick and KPNO. We find the spectral classification to be sensitive to radial velocity shifts and variations in instrument sensitivity so in order to obtain a uniform classification, we must correct the spectra to account for these potential effects. In some cases, these effects were great enough that the original classification needed to be adjusted. A final classification was obtained for 3717 M-Dwarfs and 245 K-Dwarfs. The final distribution of these classifications shows objects with subtypes M3 and M4 to be the most common in our sample (over 1,800 spectra). Within the sample of spectra, 9% were classified as metal-poor subdwarfs (181 stars), extreme subdwarfs (100 stars), or ultrasubdwarfs (64 stars). 242.12 The Chemical Abundances of Stars in the Halo (CASH) Project. II. New Extremely Metal-poor Stars Julie A. Krugler1, A. Frebel2, I. U. Roederer3, C. Sneden1, M. Shetrone1, T. Beers4, N. Christlieb5 1University of Texas, 2Harvard-Smithsonian Center for Astrophysics, 3Carnegie Observatories, 4Michigan State University, 5University of Heidelberg, Germany. Exhibit Hall We present new abundance results from the Chemical Abundances of Stars in the Halo (CASH) project. The ~500 CASH spectra were observed using the Hobby-Eberly Telescope in "snapshot" mode and are analyzed using an automated stellar parameter and abundance pipeline called CASHCODE. For the 20 most metal-poor stars of the CASH sample we have obtained high resolution spectra using the Magellan Telescope in order to test the uncertainties and systematic errors associated with the snapshot quality (i.e., R~15,000 and S/N~65) HET spectra and to calibrate the newly developed CASHCODE by making a detailed comparison between the stellar parameters and abundances determined from the high resolution and snapshot spectra. We find that the CASHCODE stellar parameters (effective temperature, surface gravity, metallicity, and microturbulence) agree well with the results of the manual analysis of the high resolution spectra. We present the abundances of three newly discovered stars with [Fe/H] < -3.5. For the entire pilot sample, we find typical halo abundance ratios with alpha-enhancement and Fe-peak depletion and a range of n-capture elements. The full CASH sample will be used to derive statistically robust abundance trends and frequencies (e.g. carbon and n-capture), as well as placing constraints on nucleosynthetic processes that occurred in the early universe. 242.13 Extending M Dwarf Variability Studies to Longer Wavelengths James R. A. Davenport1, A. Becker1, A. F. Kowalski1, E. J. Hilton1, S. L. Hawley1 1University of Washington. Exhibit Hall Flares on M dwarfs occur stochastically, and the statistical frequency of such events is well characterized in the optical. Flares and stellar variability are a source of confusion for large time-domain surveys, and a unified physical model of these magnetically driven events across all spectral types still awaits discovery. To correctly predict the occurrence rate of M dwarf variability in future astronomical surveys, we must understand the full SED of these events as completely as possible. We have constructed a sample of ~4000 M dwarfs with a broad range of properties, each with thousands of epochs of observation. This matched data set comes from the SDSS Stripe 82 and LINEAR databases in the optical, and 2MASS Calibration Scan database in the NIR. We present preliminary results that extend the flaring rate and variability signature to longer wavelengths, where many future scientific missions such as LSST, JWST, and others will operate. 242.14 The CNO Bi-cycle in the Open Cluster NGC 752 Keith Hawkins1, S. Schuler2, J. King3, L. The3 1Ohio University, 2NOAO, 3Clemson University. Exhibit Hall The CNO bi-cycle is the primary energy source for main sequence stars more massive than the sun. To test our understanding of stellar evolution models using the CNO bi-cycle, we have undertaken light-element (CNO) abundance analysis of three main sequence dwarf stars and three red giant stars in the open cluster NGC 752 utilizing high resolution (R ~ 50,000) spectroscopy from the Keck Observatory. Preliminary results indicate, as expected, there is a depletion of carbon in the giants relative to the dwarfs. Additional analysis is needed to determine if the amount of depletion is in line with model predictions, as seen in the Hyades open cluster. Oxygen abundances are derived from the high-excitation O I triplet, and there is a 0.19 dex offset in the [O/H] abundances between the giants and dwarfs which may be explained by non-local thermodynamic equilibrium (NLTE), although further analysis is needed to verify this. The standard procedure for spectroscopically determining stellar parameters used here allows for a measurement of the cluster metallicity, [Fe/H] = 0.04 ± 0.02. In addition to the Fe abundances we have determined Na, Mg, and Al abundances to determine the status of other nucleosynthesis processes. The Na, Mg and Al abundances of the giants are enhanced relative to the dwarfs, which is consistent with similar findings in giants of other open clusters. Support for K. Hawkins was provided by the NOAO/KPNO Research Experiences for Undergraduates (REU) Program which is funded by the National Science Foundation Research Experiences for Undergraduates Program and the Department of Defense ASSURE program through Scientific Program Order No. 13 (AST-0754223) of the Cooperative Agreement No. AST-0132798 between the Association of Universities for Research in Astronomy (AURA) and the NSF. 242.16 Nearby Motionless Stars Adric R. Riedel1, T. J. Henry1, R. J. White2, I. Song3, E. N. Jensen4, RECONS 1Georgia State Univ./RECONS, 2Georgia State Univ., 3University of Georgia, 4Swarthmore College. Exhibit Hall Almost 15% of all systems within 25 parsecs should be moving slower than 0.18 arcseconds per year, but traditional proper motion searches for nearby systems will miss them. Apart from USNO-B1, work by Lepine and Deacon, and stars bright enough to be seen by Hipparcos, the proper motion regime is almost completely unexplored. We have made a photometric search of the SuperCOSMOS database (Hambly 2002) to locate new nearby systems. The most promising targets moving slower than 0.18”/yr are being followed up with low resolution spectroscopy, CCD photometry, and trigonometric parallaxes from the CTIOPI program. Our first results have revealed nearby nearly-motionless systems like SCR2049-4012 (9.2 pc, 0.06”/yr), and a large number of apparent binary and young systems (a few perhaps as young as TW Hydra) of great astrophysical interest. This research is supported by NSF grant AST 09-08402 242.17 Youth Indicators of Late-M Dwarfs Daniel Feldman1, K. Cruz2, S. Lépine3, N. Alpert4 1CUNY College of Staten Island, 2CUNY Hunter College & AMNH, 3AMNH, 4Vassar College. Exhibit Hall We present a study in which we searched for a correlation between weak Na absorption doublet (8183Å, 8194Å) and strong H-Alpha emission (6563Å) in late-M dwarf stars (M6-M9), as both are indicative of youth. Our sample consists of late-M Dwarfs from the LSPM Survey (Lépine and Shara, 2005), which contain stars with measured proper motions of mu > 40 mas/yr. Measurements for emission and absorption strength were made using spectral indices. Our preliminary results are presented; future work will include a similar analysis of early type M Dwarfs, as well as kinematics. This work was funded by the CUNY Summer Undergraduate Research Program, as well as the CUNY Macaulay Honors College, and we acknowledge the hospitality of the American Museum of Natural History. 242.18 X-ray and Radio Observations of LP349-25 Sarah J. Schmidt1, R. A. Osten2, S. L. Hawley1, P. Ngoc3, N. Reid2 1University of Washington, 2Space Telescope Science Institute, 3Academia Sinica Institute for Astronomy & Astrophysics, Taiwan. Exhibit Hall For a long time ultracool dwarfs (stellar objects with spectral types later than M7) were not thought to display any of the characteristics associated with the presence and action of strong magnetic fields, but surprisingly, recent observations have demonstrated the continuation of chromospheric and coronal indicators into this regime. The radio and X-ray behavior of ultracool dwarfs in particular show strikingly different behaviors when compared to what is seen in higher mass stars: objects detected at X-ray wavelengths show the decline of plasma heating with effective temperature but with examples of flare-like behavior which suggest some continuation in behavior from early-mid M dwarf stars. Radio detections of ultracool dwarfs are characterized by variability which occurs on timescales associated with the rotation period, and the dominant emission mechanism may switch from the incoherent gyrosynchrotron seen on earlier M stars to a coherent maser process. There is a discontinuity between radio-detected ultracool dwarfs (which tend to be X-ray weak or undetected) and X-ray detected ultracool dwarfs, which tend to be radio weak or undetected. The young brown dwarf binary LP 349-25 is a peculiar radio emitter due to its lack of radio variability on both long and short timescales. The lack of rotational modulation presents difficulties for the generation of radio emission in strong large scale magnetic fields. To further investigate the conditions of LP349-25, we present simultaneous radio and x-ray observations of LP349-25. Initial analysis of the data shows that the radio emission continues to be constant and that LP349-25 additionally shows quiescent x-ray emission. This allows us to place additional constraints on the mechanism for radio emission in LP349-25 and explore the conditions which cause disparate high energy behaviors in ultracool dwarfs. 242.19 NEMESIS: Near Encounters with M-dwarfs from an Enormous Sample and Integrated Simulations John J. Bochanski1, R. E. Sanderson2, A. A. West3, A. J. Burgasser4 1Penn State, 2Massachusetts Institute of Technology, 3Boston University, 4UC, San Diego. Exhibit Hall The latest spectroscopic catalog of M dwarfs identified in the Sloan Digital Sky Survey provides radial velocities, proper motions and distances for nearly 40,000 low-mass stars. Using the full 6D phase space coverage and a realistic Galactic potential, we calculated orbits for each star in the sample. The sample consists of stars from both the thin and thick disks, and the orbital properties between the two groups are compared. We also examine trends in orbital properties with spectroscopic features, such as Balmer emission and molecular bands, that should correlate with age. In addition, we have identified a number of stars that will pass very close to the Sun within the next 1000 Myrs. These stars form the "Nemesis" family of orbits. Potential encounters with these stars could have a significant impact on orbits of Oort Cloud and Kuiper Belt members as well as the planets. We comment on the probability of a catastrophic encounter within the next 1000 Myrs. 242.20 M Dwarf Atomic and Molecular Features in SDSS DR7 Spectra Meghin Spencer1, J. R. A. Davenport1, A. A. West2, S. L. Hawley1 1University of Washington, 2Boston University. Exhibit Hall Large, homogenous spectroscopic datasets offer the opportunity to investigate the behavior of stellar atmospheres as a function of various stellar parameters with unprecedented statistical accuracy. We use the SDSS DR7 spectroscopic catalog of 70,000 low mass stars to investigate the changes in atomic and molecular features that occur with differing mass, temperature, metallicity, and level of magnetic activity. 242.21 The Differential Rotation of Very Low-Mass Stars Matthew K. Browning1 1Canadian Institute for Theoretical Astrophysics, Canada. Exhibit Hall We present 3-D MHD simulations of fully convective stars rotating at various rates. We report here in particular on the zonal flows (differential rotation) realized in these simulations, and on how magnetic fields generated by dynamo action act to partly quench those flows. In general, the simulations establish surface differential rotation profiles that are solar-like (with a fast equator and slow poles) whenever rotation is sufficiently strong; when the simulated stars rotate very slowly, however, the differential rotation is typically anti-solar (with a retrograde equator). This change in behavior may be observable through photometric monitoring with, e.g., Kepler. We analyze the maintenance of these flows and compare the angular momentum transport realized here with that in more massive stars, giant planets, and accretion disks. 242.22 Magnetic Cycles in a Wreath-Building Dynamo Simulation of a Young Solar-type Star Benjamin Brown1, M. S. Miesch2, M. K. Browning3, A. S. Brun4, N. J. Nelson5, J. Toomre5 1Univ. of Wisconsin - Madison, 2High Altitude Observatory, 3Canadian Institute for Theoretical Astrophysics, Canada, 4DSM/IRFU/SAp, CEA-Saclay and UMR AIM, CEA-CNRS-Université Paris, France, 5JILA and Dept. Astrophysics & Planetary Sciences, Univ. of Colorado at Boulder. Exhibit Hall Stars like the Sun build global-scale magnetic fields though dynamo processes in their convection zones. There, global-scale plasma motions couple with rotation and likely drive cycles of magnetic activity, though the exact processes at work in solar and stellar dynamos remain elusive. Observations of younger suns indicate that they rotate quite rapidly, have strong magnetic fields at their surfaces, and show signs of cyclic activity. Here we explore recent 3-D MHD simulations of younger, more rapidly rotating solar-type stars conducted with the anelastic spherical harmonic (ASH) code. These simulations of global-scale convection and dynamo action produce strikingly organized magnetic structures in the bulk of their convection zones. Wreaths of magnetic field fill the convection zone and can undergo regular cycles of polarity reversal. Indeed, we find that cyclic behavior is a common feature throughout the parameter space we have explored. Though these magnetic wreaths can coexist with tachoclines of penetration and shear, they do not rely on that internal boundary layer for their formation or persistence. Tachoclines may play a less critical role in the stellar dynamos of younger Suns than has been supposed in solar dynamo theory. 242.23 Distances to Eclipsing M-Dwarf Binary Systems Gail Schaefer1, G. T. van Belle2, K. von Braun3, T. S. Boyajian1, D. R. Ciardi3, M. Lopez-Morales4 1Georgia State University, 2European Southern Observatory, Germany, 3Caltech, 4Institut de Ciencies de L'Espai, Spain. Exhibit Hall We present preliminary trigonometric parallax measurements of five nearby M-dwarf eclipsing binary systems obtained using the Fine Guidance Sensors (FGS) on board the Hubble Space Telescope. We also obtained photometric and spectroscopic observations to classify the background astrometric reference stars in order to convert the parallaxes from relative to absolute. Based on the distance measurements, we can calculate model-independent luminosities for these M-dwarf binaries. Combined with their dynamical masses, these measurements provide anchor points for the low-mass end of the mass-luminosity diagram. 242.24 Making The Most Of Flaring M Dwarfs Nicholas Hunt-Walker1, E. Hilton1, A. Kowalski1, S. Hawley1, J. Matthews2, J. Holtzman3 1University of Washington, 2University of British Columbia, Canada, 3New Mexico State University. Exhibit Hall We present observations of flare activity using the Microvariability and Oscillations of Stars (MOST) satellite in conjunction with simultaneous spectroscopic and photometric observations from the ARC 3.5-meter, NMSU 1.0-meter, and ARCSAT 0.5-meter telescopes at the Apache Point Observatory. The MOST observations enable unprecedented completeness with regard to observing frequent, low-energy flares on the well-known dMe flare star AD Leo with broadband photometry. The observations span approximately one week with a 60-second cadence and are sensitive to flares as small as 0.01-magnitudes. The time-resolved, ground-based spectroscopy gives measurements of H? and other important chromospheric emission lines, whereas the Johnson U-, SDSS u-, and SDSS g-band photometry provide color information during the flare events and allow us to relate the MOST observations to decades of previous broadband observations. Understanding the rates and energetics of flare events on M dwarfs will help characterize this source of variability in large time-domain surveys such as LSST and Pan-STARRS. Flare rates are also of interest to astrobiology, since flares affect the habitability of exoplanets orbiting M dwarfs. 242.25 HST/FGS Parallaxes of Metal-Poor Main Sequence Stars: An Update Brian C. Chaboyer1, G. F. Benedict2, B. E. McArthur2, A. McWilliam3, E. Nelan4, R. J. Patterson5, A. Sarajedini6, G. Feiden1 1Dartmouth College, 2University of Texas at Austin, 3Observatories of the Carnegie Institution of Washington, 4Space Telescope Science Institute, 5The University of Virginia, 6University of Florida. Exhibit Hall We are using the Fine Guidance Sensors (FGS) on HST to obtain parallaxes of 9 metal-poor ([Fe/H] < -1.5) main sequence stars. The HST parallaxes are expected to have an accuracy of 0.2 mas (millisecond of arc), leading to absolute magnitude uncertainties of +/-0.05 mag for a given star. These stars will be used to test metal-poor stellar evolution models and to determine main sequence fitting distances to a large number of low metallicity globular clusters. FGS data has been obtained successfully for all stars during cycle 17 and will be complete at the end of cycle 18. ACS observations with the the F606W and F814W filters have been obtained for each star. ACS and ground based photometry is presented for the 9 stars. We are currently obtaining ground based high resolution spectra of all target stars which will be used to determine the composition of each star. A new grid of stellar evolution models and isochrones, which incorporate a range of different assumptions regarding the physics of stellar evolution, are currently being computed. 242.26 Finding Friends for Red Dwarfs Jennifer G. Winters1, T. J. Henry1, M. R. Boyd2, N. C. Hambly3, RECONS 1Georgia State University, 2Georgia Institute of Technology, 3Royal Observatory, University of Edinburgh, United Kingdom. Exhibit Hall Stellar multiplicity provides fundamental clues about the nature of star formation, the distribution of baryonic mass in the Universe, and the evolution of stellar systems over time. How stars are parceled into singles, doubles, and higher order multiples also provides clues about the angular momentum distribution in stellar systems and constraints on whether planets may be found. Because of their large numbers, arguably the best sample that can be studied to understand stellar multiplicity are the nearby M-dwarfs. Companion searches have been done for M-dwarfs during the past few decades, but all of the surveys have had on the order of 100 targets. With samples of this size, our statistical understanding of the distribution of companions is quite weak. We are currently systematically surveying ~1200 red dwarfs that have trigonometric parallaxes placing them within 25 pc of the Sun for stellar companions at separations of 1" to 10'. By obtaining I-band images using the CTIO 0.9m in the south and the Lowell 42in in the north, we are probing the environs of these systems for companions at separations of 1" to 3'. Because the systems all have accurate parallaxes, biases inherent to photometrically-selected samples are eliminated. A complementary reconnaissance of wider companions out to 10' is also being done via blinking of SuperCOSMOS BRI images. The results will allow statistical analyses of the nearby M-dwarf population, refinement of the solar neighborhood membership roster, and improvement of the mass function for these objects at the end of the main sequence. This is the largest, most comprehensive study ever done of the multiplicity of the most common stars in the Galaxy, one that will hopefully reveal those hidden friends lurking in the darkness. This work is supported by NSF grant AST 09-08402, the SMARTS Consortium, and Georgia State University. 242.27 Calculating Luminosities for a Large Sample of Brown Dwarfs Frank Stabile1, K. Allers2 1Fordham University, 2Bucknell University. Exhibit Hall We set out to expand the number of brown dwarfs with calculated luminosities and bolometric corrections. We chose our sample by collecting published near infrared spectra of brown dwarfs from the Spex Prism Library. The sample is predominantly L and T type dwarfs, although some M dwarfs have been included. These spectral energy distributions were extended to optical wavelengths using SDSS photometry or published optical spectra. Similarly, the spectra were extended out to longer wavelengths using Spitzer photometry and published spectra. The spectrum for each object covers a range from roughly 0.6 microns to 15 microns. In the cases where the photometry was not available, we developed a robust method to approximate missing data utilizing both the published spectral types of the objects as well as their NIR colors. Our initial results with an expanded sample fit well with previously published work. 242.28 Ultraviolet Spectral Synthesis of HgMn Stars Ronald-Louis Ballouz1, E. L. Fitzpatrick1 1Villanova University. Exhibit Hall We present a detailed analysis of the ultraviolet spectrum of HgMn stars. Using the SPECTRUM code of Gray and Corbally (1994) we perform a high resolution, order by order, analysis of archival spectroscopic data from the International Ultraviolet Explorer (IUE). The data set used here consists of IUE spectrophotmetry obtained using the high-resolution echelle observing mode with both the short-wavelength (1150-2000 Angstroms) and the long-wavelength (1900-3200 Angstroms) cameras. This study builds upon detailed spectral synthesis work of the A0V star Vega by Fitzpatrick (2010) and the analysis of HgMn star IUE spectra by Smith (1993) . Through a chi2 minimization routine the analysis yields detailed abundances, effective temperatures, radial velocities, surface gravities, and microturbulence velocities. Thusly, we improve on the parameter determinations for HgMn and comment on the abundance patterns of these chemically peculiar B-stars. This work is supported by the Villanova University Research for Undergraduates Awards Program and NASA programs. 242.29 Brown Dwarfs from SDSS-III Marvels: A Look At The Population Of The Desert Nathan M. De Lee1, J. Ge1, S. Gaudi2, B. Lee1, S. Fleming1, B. Ma1, K. Stassun3, J. Pepper3, D. Nguyen1, L. Hebb3, J. Wisniewski4, S. Mahadevan5, C. Reyle6 1Univ. of Florida, 2Ohio State University, 3Vanderbilt University, 4Univ. of Washington, 5Penn State University, 6Besançon Observatory, France. Exhibit Hall The SDSS-III MARVELS survey is a comprehensive radial velocity survey of 10,000 nearby F through K stars, between magnitudes 7.6 < V < 12.0. The primary goal of this survey is to search for planets among a homogeneous set of stars, which will be used to put constraints on formation and evolution models. This survey is also very sensitive to more massive companions such as brown dwarfs (BDs) and low mass binaries. We will discuss an ongoing project aimed at characterizing the properties of these massive companions. As part of the first two years of the six year MARVELS project, approximately 2,000 stars were searched for BDs from 1 to 180 days using a modified Lomb-Scargle periodogram, yielding roughly a dozen candidates. The completeness of this BD dataset will be determined from Monte Carlo simulations, and the completeness corrected dataset will be used to compute the fraction of solar-like stars that host short- to intermediate-period BD companions. Several of these BD have host stars characterized allowing us to explore in detail their place in the BD desert and how parameters like spectral type and metallicity play a role. Finally, this large homegeneous radial velocity survey will be placed in the larger context of our current knowledge about BD statistics. 244 Cosmic Microwave Background Poster Session Exhibit Hall 244.01 Stacking Catalog Sources in WMAP Data Kasey Schultz1, K. M. Huffenberger1 1University of Miami. Exhibit Hall Following Sawangwit & Shanks (2010), we stack WMAP 7-year data around extragalactic point sources to probe deviations in the source profiles from the Jupiter-modeled WMAP beams. Like them, we find that the stacked source profiles are broader than the WMAP model beam. Subtracting a foreground model changes the stacked profiles significantly, particularly at Q-band, but even after subtraction, the profiles appear significantly wider than the WMAP models in the Q-, V-, and W-bands, and have much heavier tails. While ground-based CMB measurements and cross-correlations with WMAP data mean that serious problems with the WMAP beam models are unlikely, the too-broad source profiles still require explanation. We explore several possibilities with parametric fits to the stacked profiles, probing the source frequency spectrum and positional uncertainty. These explanations appear to be unlikely candidates. Finally, we explore the selection bias at the faint end of the WMAP catalog, where sources lying along the same line of sight as a positive CMB fluctuation may be boosted above the WMAP catalog threshold. 244.02 Measurement Of The Null In The Sunyaev-zel'dovich Effect With Z-spec Michael B. Zemcov1, J. Aguirre2, J. Bock3, M. Bradford3, J. Glenn4, R. Lupu2, H. Nguyen3 1California Insitute of Technology, 2University of Pennsylvania, 3Jet Propulsion Laboratory, 4University of Colorado, Boulder. Exhibit Hall The (thermal) Sunyaev-Zel'dovich (SZ) effect is a decrement in the brightness of the cosmic microwave background (CMB) as seen through galaxy clusters at mm wavelengths and an increment at sub-mm wavelengths which passes though a null at 217 GHz when the scatttering plasma is cold. To correctly describe the SZ distortion when relativisitic electrons are present or the cluster is moving with respect to the CMB requires the addition of correction terms usually called the `non-thermal' and `kinetic' SZ effects. These corrections change both the shape and null frequency of the SZ spectral distortion and should be detectable using suitable instruments. We have measured the SZ effect in the bright galaxy cluster RXJ 1347-1145 using Z-Spec, a spectro-photometer which has uniquely high spectral resolution and continuous coverage between 180 and 300 GHz. This paper presents preliminary results of this measurement, cluster parameters derived from it, and the outlook for future measurements of the SZ effect using mm-wave spectro-photometers. 244.03 Expected Circular Polarization Detection by the Primordial Inflation Polarization Explorer (PIPER) Wenli Mo1, A. Kogut2 1Johns Hopkins University, 2Goddard Space Flight Center. Exhibit Hall The Primordial Inflation Polarization Explorer (PIPER) is a balloon-borne mission searching for the polarization of the cosmic microwave background (CMB) created during the inflationary epoch of the early universe. Instruments will detect both linear and circular polarization (CP) with high precision. Though CP is not predicted in the CMB, it does exist in extragalactic radio sources. The objective of this study is to determine PIPER’s expected CP detection from extragalactic radio sources. We will discuss the collection of CP detection from fifty-eight different sources and the expected flux when scaled using the PIPER beam and observing frequency. Also, we will present a CP sky map, which provides a sample of the intensity and location of these sources. 245 Starburst Galaxies Poster Session Exhibit Hall 245.01 The Extended Hot Halo of NGC3079 Ralf-Juergen Dettmar1, M. Wezgowiec1, D. J. Bomans1 1Ruhr-University, Germany. Exhibit Hall NGC3079 is a nearby edge-on galaxy harboring a composite starburst-AGN nucleus and a disk with a high starformation rate. Earlier observations showed an expanding bubble in the nucleus and some hot gas above the disk. Using XMM-NEWTON data we now trace the hot halo of NGC 3079 to much larger distances and show that the global structure is X-shaped, a configuration similar to the one observed for cosmic ray halos of several galaxies in the radio-continuum (e.g. in NGC 5775).This large scale distribution of the X-ray halo is discussed in comparison to radio-continuum and Halpha data. The X-ray observations have sufficient statistics to allow for spectral analysis at different radial distances from the disk and to search for temperature differences. We also investigate the interaction of the hot halo gas with companion galaxies. This work is supported by DLR Verbundforschung "Extraterrestrik". 245.02 Diffuse Far-UV Line Emission from Circumgalactic Gas Nicholas Nell1, K. France1, J. C. Green1, C. Leitherer2 1CASA, 2Space Telescope Science Institute. Exhibit Hall We present new ultraviolet (UV) observations of the luminous compact blue galaxy KISSR242, obtained with the Hubble Space Telescope-Cosmic Origins Spectrograph (HST-COS). We identify multiple resolved sub-arcsecond near-UV sources within the COS aperture. The far-UV spectroscopic data show strong outflow absorption lines, consistent with feedback processes related to an episode of massive star formation. O I, C II, and Si II-Si IV are observed with a mean outflow velocity langv outrang = -60 km s?¹. We also detect faint fine-structure emission lines of singly ionized silicon for the first time in a low-redshift starburst galaxy. These emissions have been seen previously in deep Lyman break galaxy surveys at z ? 3. The Si II* lines are at the galaxy rest velocity, and they exhibit a quantitatively different line profile from the absorption features. These lines have a width of ? 75 km s?¹, too broad for point-like emission sources such as the H II regions surrounding individual star clusters. The size of the Si II* emitting region is estimated to be ? 250 pc. We discuss the possibility of this emission arising in overlapping super star cluster H II regions, but find this explanation to be unlikely in light of existing far-UV observations of local star-forming galaxies. We suggest that the observed Si II* emission originates in a diffuse warm halo populated by interstellar gas driven out by intense star formation and/or accreted during a recent interaction that may be fueling the present starburst episode in KISSR242. Based on observations made with the NASA/ESA Hubble Space Telescope, obtained from the data archive at the Space Telescope Science Institute. STScI is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS 5-26555. 245.03 Large-scale Shock-ionized and Photoionized Gas in M83: The Impact of Star Formation Sungryong Hong1, D. Calzetti1, M. A. Dopita2, WFC3 SOC 1University of Massachusetts at Amherst, 2Research School of Astronomy & Astrophysics, The Australian National University, Australia. Exhibit Hall We investigate the ionization structure of nebular gas in M83 using the line diagnostic diagram, [SII](6716+6731A)/H? vs. [OIII](5007A)/H? with the newly available narrowband images from the Wide Field Camera 3(WFC3) of the Hubble Space Telescope(HST). We produce the diagnostic diagram on a pixel-by-pixel (0.2??×0.2??) basis and compare it with several photo- and shock-ionization models. We select four regions from the center to the outer spiral arm and compare them in the diagnostic diagram. For the photo-ionized gas, we observe a gradual increase of the log([OIII]/H?) ratios from the center to the spiral arm, consistent with the metallicity gradient from the center to the spiral arm, as the HII regions go from super solar abundance to roughly solar abundance. Using the diagnostic diagram, we separate the photo-ionized from the shock-ionized component of the gas. We find that the shock-ionized H? emission ranges from ?2% to about 15-20% of the total, depending on the separation criteria used. An interesting feature in the diagnostic diagram is an horizontal distribution around log([OIII]/H?) ? 0. This shows a good fit with a shock-ionization model at 2.0 Z? metallicity and shock velocities in the range of 300 km/s to 400 km/s. A low velocity shock component, < 200 km/s, is also detected, and is located at the boundary between the outer ring and the spiral arm. The low velocity shock component can be due to 1) supernova remnants located nearby, 2) dynamical interaction between the outer ring and the spiral arm, 3) abnormal line ratios from extreme local dust extinction. This paper is based on Early Release Science observations made by the WFC3 Scientific Oversight Committee. We are grateful to the Director of the Space Telescope Science Institute for awarding Director's Discretionary time for this program. 245.04 The Physics of the Calorimeter Model in M82 Tova Yoast-Hull1, J. Everett1, J. S. Gallagher III1, E. Zweibel1 1University of Wisconsin-Madison. Exhibit Hall The striking correlation between far-infrared and radio emission found in disk galaxies has led to a calorimetric model for galaxies. In this calorimeter model, all the energy input from supernovae is expended within the galaxy, so both the far-infrared and radio synchrotron emission from cosmic rays are proportional to the supernova rate. To determine how broadly the calorimeter model applies, we examine the energy balance in the starburst galaxy M82: this galaxy's hyperactive star formation rate per unit area (100 times the Milky Way's mean value) provides a severe test of the calorimeter model. Using an empirical model for the M82 starburst zone, we determine confinement times of cosmic rays in the galaxy and the energy losses of primary and secondary cosmic rays, specifically accounting for pair production, ionization losses, and synchrotron emission. We also consider the role of a wind in the propagation and transport of the cosmic rays. The results are tested against the observed multi-wavelength characteristics of M82. 245.05 Molecular Hydrogen in the Galactic Wind of M82 Joshua Fuchs1, D. Rupke1 1Institute for Astronomy, University of Hawai’i ; Rhodes College. Exhibit Hall A more complete understanding of the multiphase nature of galactic winds is necessary to constrain the dominant carriers of mass and energy. Recent studies of near-infrared lines of molecular hydrogen in the galactic wind of M82 have revealed that the warm H2 is extended more than 3 kpc from the nucleus of the galaxy. This project used Gemini NIR spectroscopy to study the velocity structure of the warm molecular hydrogen, which in turn provides information on the dynamical importance of this newly-discovered, extended phase. We also present near-infrared shock diagnostics of the M82 wind. This work was conducted by a Research Experience for Undergraduates (REU) position at the University of Hawai'i's Institute for Astronomy and funded by the NSF. 245.06 Densitometry and Thermometry of Starburst Galaxies Meredith A. MacGregor1, J. G. Mangum2 1Harvard University & NRAO, 2NRAO. Exhibit Hall The conditions that lead to the development of starburst regions within galaxies are not well understood. By combining observations of formaldehyde (H2CO) and ammonia (NH3), we present a more complete picture of the physical conditions within several known starburst galaxies. Observations of the 110-111 and 211-212 K-doublet transitions of H2CO and the (1,1), (2,2), (4,4), and (2,1) transitions of NH3 were taken using the Green Bank 100-m telescope. The ratio of the integrated intensities of the observed metastable levels of NH3 was used to determine probable values of the kinetic temperatures in the starburst regions. Using these calculated kinetic temperature values to restrict Large Velocity Gradient modeling of the H2CO lines allowed us to determine the best fit spatial and molecular column densities for a sample of six starburst galaxies. The variations among starburst galaxies are discussed in the context of the physical parameters determined in this study and available from the literature. This project was supported by the NSF/REU grant AST-0223851 and the National Radio Astronomy Observatory. 245.07 Mini-Spirals: Signatures of Galaxy Transformation John S. Gallagher1, K. Dellenbusch2, A. Parker3 1Univ. of Wisconsin, 2Bowling Green State University, 3Indiana University. Exhibit Hall Dissipative processes play a major role in controlling the growth of galaxies, particularly in producing their dense baryon dominated central regions. Observations exploring how baryons lose energy and angular momentum to allow gas to flow into the centers of galaxies therefore provide important windows into galaxy evolution. One such pathway is associated with the presence of small, gas-rich disks. These features can be especially prominent in lower mass starburst galaxies, where they sometimes appear as remarkable miniature spirals. The compact starburst galaxies NGC 3928 (MB = -18.6) and II Zw 168 (MB = -21.4) are examples of this phenomenon, hosting high surface brightness inner disks with diameters of approximately 3 kpc and 5 kpc, respectively. Both disks display well developed spiral structure, and are embedded in larger diffuse stellar envelopes. Using a combination of data from the archives and our observations, we present basic physical characteristics of these two systems, which include spiral arms with widths of only ~100 pc, and utilize this information to investigate their unusual evolutionary states. This research has been supported in part by grant NSF AST-0708967 and made use of the WIYN Observatory 0.9-m and 3.5-m telescopes. 245.08 GBT HI Observations Of The GOALS Luminous Infrared Galaxies Diana Windemuth1, D. T. Frayer2, R. Maddalena2 1Barnard College of Columbia University, 2NRAO. Exhibit Hall The Great Observatories All-sky LIRG Survey (GOALS) represents a sample of the most luminous infrared galaxies (LIRGs, L(IR)>1e11 L(Sun)) in the local Universe. LIRGs show enhanced starburst and AGN activity, typically related to interacting galaxies and merger events. We report on a new deep Green Bank Telescope (GBT) HI survey of all of the GOALS galaxies above a declination of -35 degrees (167 LIRGs in total). The observations were carried out in 2010 and were recently just completed. We discuss the preliminary analyses of the HI masses and the ratios of HI to stellar mass as a function of infrared luminosity and merger stage. This research was carried out at National Radio Astronomy Observatory (NRAO) Green Bank facility as part of the National Science Foundation (NSF) Research for Undergraduates (REU) program. The NRAO is a facility of the NSF operated under cooperative agreement by Associated Universities, Inc. 245.09 The Kinetic Temperature of Molecular Gas in Arp 220: Ammonia Observations with the ATCA and GBT Juergen Ott1, C. Henkel2, J. A. Braatz1, A. Weiss2 1National Radio Astronomy Observatory, 2Max-Planck-Institut fuer Radioastronomie, Germany. Exhibit Hall Using the ATCA and GBT telescopes, we observed ammonia (NH3) in Arp 220, the nearest ultraluminous infrared galaxy merger. We detect all the inversion transitions from (1,1) through (6,6) in absorption against the bright radio continuum. The velocities indicate that the absorption emerges from the gas that encompasses both starburst nuclei. Ammonia is a very good thermometer for the molecular gas and we derive a kinetic temperature of 186+/-55 K. The profile of the ammonia (1,1) emission is unusually weak compared to the other inversion transitions, which may indicate an additional cold component that is masking the line profile. 245.10 VLBI Imaging of OH Satellite Lines in Arp220 Derek Felli1, C. J. Salter2, T. Ghosh2, E. Momjian3 1BYU, 2NAIC-Arecibo Observatory, Puerto Rico, 3NRAO. Exhibit Hall Arecibo single-dish spectra of Arp220 taken in 2003 revealed complex emission and absorption features in the OH satellite lines at 1612 and 1720 MHz. From these spectra, two velocity ranges are found where these lines are conjugate, while in a third both lines are in emission, with both being seen in absorption in a fourth. For a fuller understanding of the physical conditions leading to such behaviour in this prototype ULIRG, the precise locations and structures of these individual features need to be know in order that detailed comparison can be made with existing high-resolution line and continuum studies of the object. Accordingly, VLBI observations with the EVN (including the Arecibo telescope) were taken of both satellite lines, and have recently been imaged. In this poster, we will present these images and the results and conclusions derived from them. 245.11 An All-stokes, All-line Survey Of OH Megamasers in Luminous Infrared Galaxies James McBride1, C. Heiles1 1UC Berkeley. Exhibit Hall We present recent results from a survey of all known OH megamasers accessible to the Arecibo 300-m telescope. The survey is an extension of the work presented in Robishaw, Quataert, and Heiles (2008), measuring all four Stokes parameters for the main OH maser lines at 1667 and 1665 MHz and the satellite lines at 1612 and 1720 MHz. We compare the original observations of the sources presented in Robishaw et al. to reobservations of the same sources a few years later, and discuss evidence for variability. The linear polarization data may be used to place limits on and in some cases measure the Faraday rotation for the continuum synchrotron emission. We use the circular polarization data to measure the Zeeman splitting of maser lines. The Zeeman splitting is then used to measure the magnetic field in the masing regions. We connect the measured magnetic fields with the large scale properties of the Luminous Infrared Galaxies that play host to OH megamasers. Support for this work was provided in part by NSF grant AST-0908572. 245.12 Spitzer Spectroscopy of Two Lensed Star-forming Galaxies Ross Fadely1, S. S. Allam2, A. J. Baker3, H. Lin2, D. Lutz4, A. E. Shapley5, M. Shin6, J. Allyn Smith7, M. A. Strauss8, D. L. Tucker2 1Haverford College, 2Fermi National Accelerator Laboratory:, 3Rutgers University, 4Max-Planck-Institut fur extraterrestrische Physik, Germany, 5University of California, Los Angeles, 6University of Michigan, 7Austin Peay State University, 8Princeton University. Exhibit Hall Presented are Spitzer/IRS spectra of two lensed UV-bright z~2 star-forming galaxies, SDSS J120602.09+514229.5 and SDSS J090122.37+181432.3. With the magnification provided by lensing, we study the rest-frame ~ 5 - 12 micron emission of the galaxies in greater detail than otherwise possible. We infer both targets are undergoing intense star-formation through the strong PAH emission seen at 6.2, 7.7, and 11.3 microns. In J1206, we detect rising continuum and significant [SIV] emission, indicating a moderately hard radiation field is powering the mid-IR luminosity. We use the strength of the [SIV] emission to infer a metallicity of Z ~ 0.5*Zsun in J1206, confirming existing measurements at optical wavelengths. For J0901, we find the strength of the PAH emission, shallow slope of the continuum, and the strength of optical [OIII] emission imply AGN energetics provide only a small fraction of the infrared luminosity. Through the ratio of [Ar III]/[Ar II], we also imply a metallicity of Z > 1.3 Zsun for J0901. We highlight the importance of both optical and mid-IR spectroscopy in understanding the properties of high-redshift galaxies. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through two awards issued by JPL/Caltech. 245.13 Redshift Determination and 12CO Line Excitation Modeling for the Multiply-Lensed Submillimeter Galaxy SMM 1057+5730 Kimberly S. Scott1, Z-Spec team, HerMES Consortium, IRAM PdBI team, CARMA team 1Univ. Of Pennsylvania. Exhibit Hall We report a redshift of z=2.956 for SMM 1057+5730, a multiply-lensed sub-millimeter galaxy detected with Herschel/SPIRE in the HerMES Lockman-SWIRE field. With the 100 GHz instantaneous bandwidth of the Z-Spec instrument on the Caltech Submillimeter Observatory, we robustly identify the redshift of this source from the simultaneous detection of four 12CO emission lines (J = 7-6, J = 8-7, J = 9-8, and J = 10-9). Combining the measured line fluxes for these high-J transitions with the J = 3-2 and J = 5-4 line fluxes measured with CARMA and the IRAM PdBI, respectively, we model the physical properties of the molecular gas in this galaxy. We find that the full 12CO spectral line energy distribution is best described by warm, low-density gas (T ? 400 K, n ? 102.7 cm-3). However, it is possible that the highest J transitions are radiatively excited by warm gas (potentially close to an AGN), or alternatively are tracing a small fraction of very dense gas in molecular cloud cores, which in either case a single gas component model would not describe the full SLED. Future observations of lower J transitions for this source will aid in distinguishing between these scenarios. 245.14 Z-Spec Measurements of CO Redshifts for Lensed Submillimeter Galaxies Discovered in the H-ATLAS Survey Roxana E. Lupu1, Z-Spec Team, ATLAS Consortium 1Univ. of Pennsylvania. Exhibit Hall We present new observations from Z-Spec, a broadband 200 - 300 GHz spectrometer, of sub-millimeter bright lensed sources recently detected by the Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS). Four out of five sources observed were detected in CO, and their redshifts measured using a new redshift finding algorithm that uses combinations of the signal-to-noise of all the lines falling in the Z-Spec bandpass to determine redshifts with high confidence, even in cases where the signal-to-noise in individual lines is low. Lower limits for the dust masses (~a few 108 M?) and spatial extents (~1 kpc equivalent radius) are derived from the continuum spectral energy distributions, corresponding to dust temperatures between 54 and 69 K. The dust and gas properties, as determined by the CO line luminosities, are characteristic of dusty starburst galaxies, with star formation rates of 102-103 M?/yr. In the LTE approximation, we derive relatively low CO excitation temperatures (< 100 K) and optical depths (tau<1). Using a maximum likelihood technique, we perform a non-LTE excitation analysis of the detected CO lines in each galaxy to further constrain the bulk molecular gas properties. We find that the mid-J CO lines measured by Z-Spec localize the best solutions to either a high-temperature / low-density region, or a low-temperature / high-density region near the LTE solution, with the optical depth varying accordingly. Future observations of CO(1-0) or other molecular lines should help distinguish these scenarios and further illuminate the star-formation history of these galaxies. 245.15 Selecting 1 0.5. 246.17 Resolved Stellar Populations In 50 Regions In M83 Hwihyun Kim1, B. C. Whitmore2, R. Chandar3, C. C. Kaleida1, A. Saha4, R. A. Windhorst1, WFC3 SOC 1Arizona State University, 2STScI, 3Univ. of Toledo, 4NOAO. Exhibit Hall Color-magnitude diagrams (CMDs) of resolved stars are the most powerful diagnostic tool to understand stellar evolution and star formation history of a galaxy in detail. By comparing stellar evolution models to observations in CMDs, we are able to determine approximate ages of individual stellar populations in galaxies. However, in some regions with recent star-forming activity, stellar populations are partially obscured by dust. Applying a single extinction correction value often results in either over- or under-estimate of the ages of individual stars. We present a multi-wavelength photometric study of resolved stars in M83 from the HST WFC3/UVIS observations using four filters - F336W, F438W, F555W, and F814W - to measure colors and, given the known distance (4.5 Mpc) to M83, intrinsic luminosities of ?10,000 stars. We selected 50 regions in a spiral arm and inter-arm areas of M83, and categorized them based on their H? morphology. To determine ages of stellar populations, we combined the CMDs and the color-color diagrams with the Padova isochrones and also constrain the spatial variation of dust extinction in each region. We correct for Galactic foreground extinction and for the extinction towards each individual star internal to M83, resulting in improved stellar age estimates from isochrone fitting on CMDs. We find that age distributions of resolved stellar populations in 50 regions agree with blue-to-red star ratios, and with ages of clusters in their vicinity. This work is based on Early Release Science observations made by the WFC3 Scientific Oversight Committee. We are grateful to the Director of the Space Telescope Science Institute for awarding Director's Discretionary time for this program. 246.18 The Arecibo Zone of Avoidance Survey Travis P. McIntyre1, P. A. Henning2, R. Minchin3, E. Momjian4 1Arecibo Observatory, The University of New Mexico, 2The University of New Mexico, 3Arecibo Observatory, 4NRAO. Exhibit Hall The Arecibo Zone of Avoidance survey is searching for 21cm emission from neutral hydrogen in galaxies located behind the plane of the Milky Way. The goal of the survey is to discover nearby galaxies which are undetectable at optical and infrared wavelengths because of high Galactic extinction and confusion. The survey will map out the nearby mass distribution and connect large scale structure across the zone of avoidance. It will also contribute to our understanding of the neutral hydrogen mass function. This poster will present the status of the survey. Observations, data reduction, and analysis are ongoing. The majority of the detections have been newly discovered sources. 246.19 The WSRT HALOGAS survey George H. Heald1, HALOGAS Team 1ASTRON, Netherlands. Exhibit Hall We present the HALOGAS (Hydrogen Accretion in LOcal GAlaxieS) survey. This is the first systematic investigation of cold gas accretion in nearby spiral galaxies to date. It consists of deep (120 hours) WSRT observations of 22 edge-on and moderately-inclined nearby galaxies. Using these data we are able to detect neutral hydrogen down to a column density of about 1019 cm-2, and characterise the faint extra-planar and anomalous-velocity neutral gas with excellent spatial and velocity resolution. HALOGAS data also allow us to study the disc structure and dynamics in unprecedented detail for a sample of this size. Observations carried out so far show a variety of HI properties, ranging from accretion of (and interaction with) satellite galaxies to filaments possibly caused by star formation in the disc. The detected amount of anomalous gas indicative of accretion episodes varies significantly from galaxy to galaxy. This suggests that accretion of neutral gas from the ambient medium is a rather episodic process. A number of companion posters present first results on the modelling of some of the observed galaxies and on observations at other wavelengths which complement our 21 cm data. 246.20 The Halogas Project: HI Observations Of NGC 1003 Richard J. Rand1, J. Allan2, G. Heald3, G. Jozsa3 1Univ. of New Mexico, 2Macalester College, 3ASTRON, Netherlands. Exhibit Hall We present deep neutral hydrogen observations of the nearby spiral galaxy NGC 1003, obtained as part of the Westerbork Hydrogen Accretion in LOcal GAlaxieS (HALOGAS) Survey currently being performed with the Westerbork Synthesis Radio Telescope (WSRT). Our data are sensitive enough to detect and study both faint diffuse neutral hydrogen gas, as well as discrete accreting gas clouds. We have performed careful tilted-ring modeling of NGC 1003, which shows that it is nearly edge-on, and has a significant warp. The HI disk is both thick (scale height ~ 1 kpc) and radially extended (4-5 times larger than the optical disk). We also present the results of our analysis of the extraplanar gas cloud population in this galaxy. We detect two discrete clouds in the halo of NGC 1003, both with HI masses of about two hundred thousand solar masses, and a larger extraplanar gas complex with an HI mass of about two million solar masses. These extraplanar gas features are analogous to high- and intermediate-velocity clouds around the Milky Way. We discuss the implications of these features for the accretion history of NGC 1003. 246.21 Kinematics of Ionized Gas in Edge-on HALOGAS Galaxies Catharine J. Wu1, R. Walterbos1, R. Rand2, R. Benjamin3, G. Heald4, HALOGAS Team 1New Mexico State University, 2University of New Mexico, 3University of Wisconsin - Whitewater, 4Netherlands Institute for Radio Astronomy, Netherlands. Exhibit Hall Extra-planar gas generally shows a decrease in rotational velocity with increasing height above the disk. It can originate from disk-halo cycling driven by star formation in the disk or from infalling gas clouds. Studies at optical and radio wavelengths suggest that a combination of the two is the most likely scenario. Our goal is to measure velocity gradients of the ionized gas in a large number of halos, which can then be used as a constraint for models of the origin of halo gas. Because we are observing in optical, our measurements are likely not affected by warps which generally occur further out in radial distance. Our targets are drawn from a well-defined sample and are also a subset of the HALOGAS survey, which is investigating cold gas accretion in spiral galaxies with deep WSRT observations. We restrict our targets to edge-on galaxies, and our data provide an optical complement to HALOGAS data. We perform our observations using a multi-slit spectroscopic setup on the ARC 3.5m telescope. Arranging the slits parallel to the minor axis allows us to measure velocities of H-alpha emitting gas as a function of height above the plane in 11 radial distance bins in a single exposure. Our field of view is 3.75' x 4', and our total exposure time for a typical field is 6-8 hours. We present our ionized halo gas velocities for three nearby, edge-on galaxies and show a comparison with HI data. 246.22 The HALOGAS Project: HI Observations Of NGC 5055 Maria Patterson1, R. Walterbos1, G. Heald2, G. Jozsa2, L. Zschaechner3, R. Rand3, D. Thilker4, HALOGAS Team 1New Mexico State University, 2Netherlands Institute for Radio Astronomy (ASTRON), Netherlands, 3University of New Mexico, 4Johns Hopkins University. Exhibit Hall We present deep neutral hydrogen observations of the nearby spiral galaxy NGC 5055 as part of the Westerbork Hydrogen Accretion in LOcal GAlaxieS (HALOGAS) survey currently being performed with the Westerbork Synthesis Radio Telescope (WSRT). The HALOGAS survey aims to investigate cold gas accretion in a sample of 22 neutrally-selected nearby spiral galaxies with 120 hours of integrated observation time for each target. The data are sensitive enough to study faint neutral hydrogen in the galaxy outskirts and to search for halogas and possible accreting gas clouds. The galaxy NGC 5055 is a moderately-inclined SAbc galaxy in the sample with a large pronounced warp of the extended gaseous disk and a declining rotation curve outside of the optical radius. We present an analysis of the new HI observations of this galaxy based on a tilted ring analysis and on more detailed modeling and visualization of the 3-D HI distribution and kinematics. We also discuss the relation between star formation in the faint outer disk spiral arms by comparison of the HI with GALEX and other star formation tracers. 246.23 The HALOGAS Project: HI Observations Of NGC 4244 And NGC 4565 Laura Zschaechner1, R. J. Rand1, G. H. Heald2, G. Gentile3, HALOGAS Team 1University of New Mexico, 2ASTRON, Netherlands, 3Universiteit Gent, Belgium. Exhibit Hall We present models of the distribution and kinematics of HI in NGC 4244 and NGC 4565, two nearby spiral galaxies observed as part of the Westerbork Hydrogen Accretion in LOcal GAlaxieS (HALOGAS) survey. These models focus on the potential existence of extraplanar gas in the form of a halo as well as the presence of a negative gradient in rotational velocity upward from the plane of the disk (a lag). Insight concerning such information may help to better understand the prevalence as well as origins of halos in spiral galaxies, specifically whether they are a result of outflow from the disk, accretion from external sources, or a combination of the two. Models of NGC 4244 yield strong evidence against the presence of a halo and instead favor a warp along the line of sight as an explanation for the observed thickening of the disk. We do detect a lag which decreases in magnitude radially outward from the center of the disk such that the lag in the outermost parts of the disk is substantially shallower than that near the center. These models are based on deeper observations as well as improved modeling techniques and thus differ somewhat from past models of NGC 4244. Previous efforts to model NGC 4565 from data taken prior to the HALOGAS survey indicate a flare as well as a potential lag. We will refine these models using our deeper observations. 247 The Center for Astronomy Education (CAE) Collaboration of Astronomy Teaching Scholars (CATS) Program: A Year-Three Update Poster Session Exhibit Hall 247.01 The Center for Astronomy Education (CAE) and Our NSF CCLI Phase-III Collaboration of Astronomy Teaching Scholars (CATS) Program: A Year-Three Update on Our Community-Based Model for Astronomy Education Research Gina Brissenden1, C. D. Impey2, E. E. Prather1, K. M. Lee3, Collaboration of Astronomy Teaching Scholars (CATS) 1Center for Astronomy Education (CAE), Steward Observatory, Univ. of Arizona, 2Steward Observatory, Univ. of Arizona, 3Univ. of Nebraska, Lincoln. Exhibit Hall The Center for Astronomy Education (CAE) has been devoted to improving teaching & learning in Astro 101 by creating research-validated curriculum & assessment instruments for use in Astro 101 & by providing Astro 101 instructors professional development opportunities to increase their pedagogical content knowledge & instructional skills at implementing these curricula & assessment materials. To create sustainability and further expand this work, CAE, in collaboration with other national leaders in astronomy education & research, developed the Collaboration of Astronomy Teaching Scholars (CATS) Program. The primary goals of CATS are to: 1) increase the number of Astro 101 instructors conducting fundamental research in astronomy education; 2) increase the amount of research-validated curriculum and assessment instruments available for use in Astro 101; and 3) increase the number of people prepared to develop and conduct their own CAE Teaching Excellence Workshops. Our year-three research updates include a longitudinal look at professional development and expanded professional development opportunities; new instructional tools and curriculum; learning gains related to Citizen Science and cosmology; and an expanded look at our LSCI study. To learn more about our CAE/CATS project, visit this and the other posters in our session. This material is based upon work supported by the National Science Foundation under Grant No. 0715517, a CCLI Phase III Grant for the Collaboration of Astronomy Teaching Scholars (CATS). Any opinions, findings, and conclusions or recommendations expressed in this material are those of the authors and do not necessarily reflect the views of the National Science Foundation. In addition, we would like to thank Michael Greene and JPL's NASA Exoplanet Public Engagement Program (EXEP) for their continued support. 247.02 Using Classical Test Theory and Item Response Theory to Evaluate the LSCI Wayne M. Schlingman1, E. E. Prather1, Collaboration of Astronomy Teaching Scholars (CATS) 1Center for Astronomy Education (CAE), Steward Observatory, Univ. of Arizona. Exhibit Hall Analyzing the data from the recent national study using the Light and Spectroscopy Concept Inventory (LSCI), this project uses both Classical Test Theory (CTT) and Item Response Theory (IRT) to investigate the LSCI itself in order to better understand what it is actually measuring. We use Classical Test Theory to form a framework of results that can be used to evaluate the effectiveness of individual questions at measuring differences in student understanding and provide further insight into the prior results presented from this data set. In the second phase of this research, we use Item Response Theory to form a theoretical model that generates parameters accounting for a student’s ability, a question’s difficulty, and estimate the level of guessing. The combined results from our investigations using both CTT and IRT are used to better understand the learning that is taking place in classrooms across the country. The analysis will also allow us to evaluate the effectiveness of individual questions and determine whether the item difficulties are appropriately matched to the abilities of the students in our data set. These results may require that some questions be revised, motivating the need for further development of the LSCI. This material is based upon work supported by the National Science Foundation under Grant No. 0715517, a CCLI Phase III Grant for the Collaboration of Astronomy Teaching Scholars (CATS). Any opinions, findings, and conclusions or recommendations expressed in this material are those of the authors and do not necessarily reflect the views of the National Science Foundation. 247.03 Improvements in Students' Understanding from Increased Implementation of Active Learning Strategies Melissa N. Hayes-Gehrke1, E. E. Prather2, A. L. Rudolph3, Collaboration of Astronomy Teaching Scholars (CATS) 1Univ. of Maryland, 2Center for Astronomy Education (CAE), Steward Observatory, Univ. of Arizona, 3California State Polytechnic Univ. Exhibit Hall Many instructors are hesitant to implement active learning strategies in their introductory astronomy classrooms because they are not sure which techniques they should use, how to implement those techniques, and question whether the investment in changing their course will really bring the advertised learning gains. We present an example illustrating how thoughtful and systematic implementation of active learning strategies into a traditionally taught Astro 101 class can translate into significant increases in students' understanding. We detail the journey of one instructor, over several years, as she changes the instruction and design of her course from one that focuses almost exclusively on lecture to a course that provides an integrated use of several active learning techniques such as Lecture-Tutorials and Think-Pair-Share questions. The students in the initial lecture-only course achieved a low normalized gain score of only 0.2 on the Light and Spectroscopy Concept Inventory (LSCI), while the students in the re-designed learner-centered course achieved a significantly better normalized gain of 0.43. This material is based upon work supported by the National Science Foundation under Grant No. 0715517, a CCLI Phase III Grant for the Collaboration of Astronomy Teaching Scholars (CATS), and Grant No. 0847170, a PAARE Grant for the Calfornia-Arizona Minority Partnership for Astronomy Research and Education (CAMPARE). Any opinions, findings, and conclusions or recommendations expressed in this material are those of the authors and do not necessarily reflect the views of the National Science Foundation. 247.04 Overcoming Common Conceptual and Reasoning Difficulties in Cosmology: A Lecture-Tutorial Approach Edward E. Prather1, C. S. Wallace2, D. Duncan2 1Center for Astronomy Education (CAE), Steward Observatory, Univ. of Arizona, 2Dept. of Astrophysical & Planetary Sciences, Univ. of Colorado at Boulder. Exhibit Hall For the past two years, we have conducted fundamental research into Astro 101 students' conceptual and reasoning difficulties in cosmology. To date, we have analyzed the responses of over 2000 students from institutions across the United States to questions on the Big Bang, the expansion and evolution of the universe, and the evidence for dark matter. Our findings have helped guide the development of a new suite of cosmology Lecture-Tutorials to help students overcome their conceptual and reasoning difficulties. We discuss naïve ideas Astro 101 students have with several cosmology topics and provide evidence that the new Lecture-Tutorials help students achieve larger learning gains than is achieved by lecture alone. This material is based upon work supported by the National Science Foundation under Grant No. 0833364 and Grant No. 0715517, a CCLI Phase III Grant for the Collaboration of Astronomy Teaching Scholars (CATS). Any opinions, findings, and conclusions or recommendations expressed in this material are those of the authors and do not necessarily reflect the views of the National Science Foundation. 247.05 Assessment Of The Effect Of Participation In Zooniverse Projects On Content Knowledge Sebastien Cormier1, E. E. Prather1, G. Brissenden1, C. Lintott2, P. L. Gay3, J. Raddick4, Collaboration of Astronomy Teaching Scholars (CATS) 1Center for Astronomy Education (CAE), Steward Observatory, Univ. of Arizona, 2Adler Planetarium/Univ. of Oxford, 3Southern Illinois Univ. Edwardsville/Astrosphere New Media Association, 4Johns Hopkins Univ. Exhibit Hall The citizen science projects developed by Zooniverse afford volunteers the opportunity to contribute to scientific research in a meaningful way by interacting with actual scientific data. We created two surveys to measure the impact that participation in the Galaxy Zoo and Moon Zoo citizen science projects has on user conceptual knowledge. The Zooniverse Astronomy Concept Survey (ZACS) was designed to assess Galaxy Zoo user understanding of concepts related to galaxies and how their understanding changed through participation in classifying galaxies. The Lunar Cratering Concept Inventory (LCCI) was designed to measure the impact of the Moon Zoo activities on user knowledge about lunar craters and cratering history. We describe how the surveys were developed and validated in collaboration with education researchers and astronomers. Both instruments are administered over time to measure changes to user conceptual knowledge as they gain experience with either Galaxy Zoo or Moon Zoo. Data collection has already begun and in the future we will be able to compare survey answers from users who have classified, for example, a thousand galaxies with users who have only classified ten galaxies. This material is based upon work supported by the National Science Foundation under Grant No. 0715517, a CCLI Phase III Grant for the Collaboration of Astronomy Teaching Scholars (CATS). Any opinions, findings, and conclusions or recommendations expressed in this material are those of the authors and do not necessarily reflect the views of the National Science Foundation and the Sloan Digital Sky Survey III Education and Public Outreach Program. 247.06 Student Practices, Learning, and Attitudes When Using Computerized Ranking Tasks Kevin M. Lee1, E. E. Prather2, Collaboration of Astronomy Teaching Scholars (CATS) 1Univ. of Nebraska, Lincoln, 2Center for Astronomy Education (CAE), Steward Observatory, Univ. of Arizona. Exhibit Hall Ranking Tasks are a novel type of conceptual exercise based on a technique called rule assessment. Ranking Tasks present students with a series of four to eight icons that describe slightly different variations of a basic physical situation. Students are then asked to identify the order, or ranking, of the various situations based on some physical outcome or result. The structure of Ranking Tasks makes it difficult for students to rely strictly on memorized answers and mechanical substitution of formulae. In addition, by changing the presentation of the different scenarios (e.g., photographs, line diagrams, graphs, tables, etc.) we find that Ranking Tasks require students to develop mental schema that are more flexible and robust. Ranking tasks may be implemented on the computer which requires students to order the icons through drag-and-drop. Computer implementation allows the incorporation of background material, grading with feedback, and providing additional similar versions of the task through randomization so that students can build expertise through practice. This poster will summarize the results of a study of student usage of computerized ranking tasks. We will investigate 1) student practices (How do they make use of these tools?), 2) knowledge and skill building (Do student scores improve with iteration and are there diminishing returns?), and 3) student attitudes toward using computerized Ranking Tasks (Do they like using them?). This material is based upon work supported by the National Science Foundation under Grant No. 0715517, a CCLI Phase III Grant for the Collaboration of Astronomy Teaching Scholars (CATS). Any opinions, findings, and conclusions or recommendations expressed in this material are those of the authors and do not necessarily reflect the views of the National Science Foundation. 247.07 Do You Need a Textbook to Teach Astro 101? Alexander L. Rudolph1, Collaboration of Astronomy Teaching Scholars (CATS) 1California State Polytechnic Univ. Exhibit Hall During educational sessions at astronomy meetings, especially during Center for Astronomy Education (CAE) Teaching Excellence workshops, which I have attended and now help present, one of the questions everyone wants to discuss is which textbook to use to teach Astro 101 classes (general education astronomy courses for non-science majors). Some instructors have a favorite. Others will claim that they are all the same and that it doesn’t matter. Increasingly, however, the discussions turn to the question of whether any textbook is needed at all. Some of this discussion has been driven by the increase in the use of interactive learning strategies such as Think-Pair-Share questions, Lecture-Tutorials, and Ranking Tasks. These activities provide students a learning modality very different from the traditional lecture supplemented by homework, and raises the question of whether the learning that takes place during such interactive activities is enough to teach students what we wish them to know about astronomy. I had been teaching an Astro 101 class for almost three years using a full suite of interactive learning strategies, when I decided to teach it without requiring the students to purchase a textbook. Comparison of test scores before and after this change shows that there is no statistical difference in student achievement whether a textbook is required or not. Details on the course and methodology used to reach this conclusion will be presented. This work is supported by the National Science Foundation under Grant No. 0847170, a PAARE Grant for the Calfornia-Arizona Minority Partnership for Astronomy Research and Education (CAMPARE), and Grant No. 0715517, a CCLI Phase III Grant for the Collaboration of Astronomy Teaching Scholars (CATS). Any opinions, findings, and conclusions or recommendations expressed in this material are those of the author and do not necessarily reflect the views of the National Science Foundation. 247.08 Burning Down the Wall: Questions Commonly Asked by Astro 101 Instructors During CAE Workshops Jacqueline Laird1, G. Brissenden1, E. E. Prather1, Collaboration of Astronomy Teaching Scholars (CATS) 1Center for Astronomy Education (CAE), Steward Observatory, Univ. of Arizona. Exhibit Hall The Center for Astronomy Education (CAE), as part of JPL’s NASA Exoplanet Public Engagement Program (ExEP), has been conducting Teaching Excellence Workshops all across the country since 2004. Nearly two thousand current and future astronomy instructors have participated in these workshops. During these highly interactive professional development experiences, participants are given the opportunity to ask anonymous questions to the workshop leaders by writing a question down on a sticky note and placing it on a sheet of paper identified as “The Wall of Burning Questions.” These “Burning Questions” are read aloud and answered by workshop leaders throughout the course of the workshop. Here we present an overview of common themes of questions workshop participants ask, as well as an analysis of the depth of pedagogical content knowledge these questions represent. This material is based upon work supported by the National Science Foundation under Grant No. 0715517, a CCLI Phase III Grant for the Collaboration of Astronomy Teaching Scholars (CATS). Any opinions, findings, and conclusions or recommendations expressed in this material are those of the authors and do not necessarily reflect the views of the National Science Foundation. In addition, we would like to thank Michael Greene and JPL’s NASA Exoplanet Public Engagement Program (ExEP) for their continued support. 247.09 Increasing the Availability of Professional Development Opportunities through the Center for Astronomy Education (CAE) Regional Teaching Exchanges Michael C. Lo Presto1, G. Brissenden2, A. D. Forestell3, R. S. French4, J. Lutz5, D. L. Martino6, W. L. Powell, Jr.7, P. E. Robinson8, A. L. Rudolph9, Collaboration of Astronomy Teaching Scholars (CATS) 1Henry Ford Community College, 2Center for Astronomy Education (CAE), Steward Observatory, Univ. of Arizona, 3SUNY New Paltz, 4MiraCosta College, 5Univ. of Washington, 6Santiago Canyon College, 7Texas Lutheran Univ., 8Westchester Community College, 9California State Polytechnic Univ. Exhibit Hall The Center for Astronomy Education (CAE), as part of JPL’s NASA Exoplanet Public Engagement Program (ExEP), has been conducting Teaching Excellence Workshops all across the country since 2004. Nearly two thousand current and future astronomy instructors have participated in these workshops. To increase the availability of professional development opportunities for past workshop participants, as well as to foster a sense of community amongst geographically linked current and future Astro 101 instructors, we created CAE Regional Teaching Exchanges. Our Exchanges are coordinated by CATS Fellows who are regional experts from the broader CAE community. Our first Regional Exchange was held in 2005, and our newest Exchange region has just been created. We report on the increased availability of professional development through our CAE Regional Teaching Exchanges, the many flavors our Exchanges take on, as well as lessons learned. This material is based upon work supported by the National Science Foundation under Grant No. 0715517, a CCLI Phase III Grant for the Collaboration of Astronomy Teaching Scholars (CATS). Any opinions, findings, and conclusions or recommendations expressed in this material are those of the authors and do not necessarily reflect the views of the National Science Foundation. In addition, we would like to thank Michael Greene and JPL’s NASA Exoplanet Public Engagement Program (ExEP) for their continued support. 247.10 A New Approach to Delivering Astronomy Content Online Kevin Hardegree-Ullman1, C. Impey1, A. Patikkal1, B. Guvenen1, A. Srinathan1, M. Swatzell1 1University of Arizona. Exhibit Hall We have created an online application that clusters the entire Wikipedia and provides a new and useful search engine and interface for the widely used internet knowledge medium. We used an existing open source search engine, and modified it with our own algorithms to give the best possible results from a search query. Astronomy served as the primary test subject in which we analyzed our clustering algorithms. We found that once our algorithms were working well for clustering astronomy articles, similarly decent results were obtained in other academic test subjects. This tool will be implemented and tested for effectiveness in introductory astronomy courses at The University of Arizona. In addition to Wikipedia, we are using our tool to cluster an online astronomy textbook and astronomy lecture video content. Our clustering and search algorithms have potential to be applied to many other subjects and online content. We believe that our tools will be beneficial to students and help them easily navigate and see correlation between subjects within the compendium of knowledge online. This material is based upon work supported by the National Science Foundation under Grant No. 0715517, a CCLI Phase III Grant for the Collaboration of Astronomy Teaching Scholars (CATS). Any opinions, findings, and conclusions or recommendations expressed in this material are those of the author(s) and do not necessarily reflect the views of the National Science Foundation. 248 Astronomy Education and Research in Grades K-12 Poster Session Exhibit Hall 248.01 Researching Effective Methods for Teaching the Phases of the Moon Heather Jones1, E. G. Hintz1, M. J. Lawler1, R. Davies1 1Brigham Young Univ.. Exhibit Hall This project investigates the effectiveness of several commonly used methods for teaching the phases of the moon to fifth and sixth grade students. Common teaching methods investigated are the use of diagrams, animations, modeling/kinesthetics, and direct observations of the moon (in a planetarium). Students are taught about the phases of the moon using one or more of these methods. Their understanding of why the phases of the moon occur is measured by a pre and post assessment. With this data, the effectiveness of each teaching method is evaluated individually and comparatively. In addition, the method’s capacity to discourage the common eclipse misconception about moon phases is also investigated. The results of this research will be useful to teachers and provide foundational data for future research in the development of educational planetarium shows. 248.02 Talk The Talk, A Double E/PO Challenge Rick Kang1 1Oregon Astrophysics Outreach-Pine Mtn. Obs.. Exhibit Hall We use many ordinary words in the process of science, such as Model, Empirical, Correlate, Characteristic, Proportion, Ratio, Noise, Precision, Accuracy, Speculation, and Hierarchy. 1. Perhaps we should take some time to clarify the scientific meaning of these words for the public, particularly for students: a. Promotes understanding of what we are working on. b. Promotes understanding of the scientific process, improving science literacy. 2. There is an ongoing opportunity to offer vocabulary to students, particularly in K-8 classrooms where there is currently great emphasis on reading to meet standards. The additional reading time is often at the expense of science time. How can we effectively include science vocabulary within the reading? I propose starting a forum to discuss these issues. 248.03 The Edelman Galileoscope Education Program: A Collaboration Among Professional Societies Stephen M. Pompea1, K. B. Marvel2, R. T. Fienberg2, D. N. Arion3, A. Herrold4, B. Kruse5, R. T. Sparks1, C. Dugan1 1NOAO, 2American Astronomical Society, 3Carthage Collage, 4National Earth Science Teachers Association, 5Astronomical Society of the Pacific. Exhibit Hall The Edelman Galileoscope Education Program is an ongoing national effort to provide K-12 teachers with Galileoscope refractor kits and the proper training to use them effectively for teaching scientific concepts and observational skills. As such it represents a strategic effort to excite children about astronomy and provides them with a powerful tool to increase science literacy. The program was made possible by a generous gift from Jean and Ric Edelman to the American Astronomical Society (AAS). The AAS teamed with the National Optical Astronomy Observatory (NOAO); Galileoscope, LLC; the National Earth Science Teachers Association (NESTA); and the Astronomical Society of the Pacific (ASP) to distribute telescopes, mainly during teacher workshops. Through the professional development efforts of NESTA, ASP, and NOAO’s Teaching With Telescopes program some 1,400 teachers received Galileoscopes and hands-on training on how to teach optics and astronomy with them. All participating teachers received Galileoscopes free of charge. Another 1,500 or so teachers not connected with these organizations also received telescopes free of charge through an Internet ordering system, paying only for shipping. Under this combination of programs more than 15,000 Galileoscopes have been given to active teachers, reaching an estimated 300,000 students. The professional development program uses a combination of face-to-face workshops, a train-the-trainer model, and Internet-based self-paced instruction. We describe the Edelman Galileoscope Education Program design, training materials, and distribution networks, as well as the geographic distribution of the teachers who received Galileoscopes. This program represents an efficient and effective model for quickly distributing valuable science teaching materials to urban, suburban, and rural teachers _ including homeschoolers _ across the United States. 248.04 Using Solar Filters with a Galileoscope Erika Grundstrom1, R. S. Taylor2 1Vanderbilt University, 2SUNY-Oswego. Exhibit Hall One of the lasting legacies of the International Year of Astronomy in 2009 is the Galileoscope. People around the world have one, but there is a major astronomical object they aren’t supposed to look at - the Sun! We found that in order to facilitate observations during the actual school day, one best incorporate the Sun. We report on a project to build and use solar filters for the Galileoscope and incorporate them into the standard daytime classroom. We will describe the filters and a curriculum we are testing and discuss the difficulties we encountered (number one being this extended solar minimum). We acknowledge a SEED grant from the Astronomical Society of the Pacific and that this work is supported in part by the Vanderbilt University Learning Sciences Institute (LSI) and the Institute of Educational Sciences (IES). 248.05 Stellar Spectroscopy: Barcodes to the Stars Angela R. Sarrazine1 1Fernbank Science Center. Exhibit Hall Peering at the night sky, and more specifically, at all the stars overhead, one begins to wonder: How do astronomers determine the composition of stars if they cannot travel to them and return samples to Earth for use in a laboratory? One way in which astronomers can make these determinations is by using the “starlight” itself. Spectroscopy is a powerful tool in astronomy. The analysis of stellar spectra can reveal the composition, temperature, and velocity of an object as well as several other pieces of information. In an effort to increase student understanding of how spectroscopy works, an analogy to barcodes has been employed with 9th grade students. Young students are very familiar with the scanning technology currently utilized at most stores. While not a one to one analogy of the process, students can begin to understand that the series of black and white lines, the width of the lines, and the spacing between assists the computer in identifying the item for purchase. By a similar token, an astronomer looks at the spectral lines of a star and based upon the thickness, separation, and location of the lines can begin to determine some of the properties of the celestial object. 248.06 A MOSAIC for the Science Classroom Vincent L. Fish1, M. M. Needles1, A. E. E. Rogers1, D. Costa2, J. Cadigan3, C. Clements4, S. K. May5 1MIT Haystack Observatory, 2Lynnfield High School, 3Oak Hill Middle School, 4Marlborough High School, 5Middlesex School. Exhibit Hall MOSAIC (Mesospheric Ozone System for Atmospheric Investigations in the Classroom) is a project to engage secondary and undergraduate students in authentic inquiry-based science learning using a network of inexpensive spectrometers monitoring the mesospheric ozone concentration. The MOSAIC system observes the 11 GHz emission line of ozone using electronics built around satellite television equipment. The possibilities for student investigation are broad and scientifically significant. MOSAIC observations have confirmed diurnal variations in mesospheric ozone concentration and detected semiannual variations that may be due to inter-hemispheric meridional circulation of water vapor. Possible future projects include monitoring the temperature of the mesosphere and correlations with the solar cycle. Students are also encouraged to design their own investigations with MOSAIC data. Early results have been reported in a major scientific journal, and further scientific progress is likely as future MOSAIC systems are deployed -- increasing the sensitivity and geographic coverage of the network. Complete teaching units, including slides, laboratory activities, background information, student worksheets, and conformance with national and Massachusetts educational standards, have been developed to integrate MOSAIC into a classroom environment. One unit introduces the layers of the atmosphere, Earth's energy balance, the greenhouse effect, processes of ozone creation and destruction, noctilucent clouds, heat transfer, the laws of thermodynamics, radio waves (including radio astronomy), and fluid behavior. A second unit, currently being tested in classrooms, uses the MOSAIC system to motivate and deepen understanding of a large portion of electromagnetism in a conceptual physics class. MOSAIC has also been used in a local high school chemistry class. MOSAIC is still in development and is funded by the National Science Foundation. 248.07 An Innovative Collaboration on Dark Skies Education Constance E. Walker1, M. Mayer2, NOAO EPO Students 1National Optical Astronomy Observatory, 2Cooper Center for Environmental Learning. Exhibit Hall Dark night skies are being lost all over the globe, and hundreds of millions of dollars of energy are being wasted in the process.. Improper lighting is the main cause of light pollution. Light pollution is a concern on many fronts, affecting safety, energy conservation, cost, human health, and wildlife. It also robs us of the beauty of viewing the night sky. In the U.S. alone, over half of the population cannot see the Milky Way from where they live. To help address this, the National Optical Astronomy Observatory Education and Public Outreach (NOAO EPO) staff created two programs: Dark Skies Rangers and GLOBE at Night. Through the two programs, students learn about the importance of dark skies and experience activities that illustrate proper lighting, light pollution’s effects on wildlife and how to measure the darkness of their skies. To disseminate the programs locally in an appropriate yet innovative venue, NOAO partnered with the Cooper Center for Environmental Learning in Tucson, Arizona. Operated by the largest school district in Tucson and the University of Arizona College of Education, the Cooper Center educates thousands of students and educators each year about ecology, science, and the beauty and wonders of the Sonoran Desert. During the first academic year (2009-2010), we achieved our goal of reaching nearly 20 teachers in 40 classrooms of 1000 students. We gave two 3-hour teacher-training sessions and provided nineteen 2.5-hour on-site evening sessions on dark skies activities for the students of the teachers trained. One outcome of the program was the contribution of ~1000 “GLOBE at Night 2010” night-sky brightness measurements by Tucson students. Training sessions at similar levels are continuing this year. The partnership, planning, lesson learned, and outcomes of NOAO’s collaboration with the environmental center will be presented. 248.08 The James Webb Space Telescope RealWorld-InWorld Design Challenge: Involving Professionals in a Virtual Classroom Margaret Masetti1, S. Bowers2 1ADNET Systems, Inc. & NASA GSFC, 2National Institute of Aerospace. Exhibit Hall Students around the country are becoming experts on the James Webb Space Telescope by designing solutions to two of the design challenges presented by this complex mission. RealWorld-InWorld has two parts; the first (the Real World portion) has high-school students working face to face in their classroom as engineers and scientists. The InWorld phase starts December 15, 2010 as interested teachers and their teams of high school students register to move their work into a 3D multi-user virtual world environment. At the start of this phase, college students from all over the country choose a registered team to lead InWorld. Each InWorld team is also assigned an engineer or scientist mentor. In this virtual world setting, each team refines their design solutions and creates a 3D model of the Webb telescope. InWorld teams will use 21st century tools to collaborate and build in the virtual world environment. Each team will learn, not only from their own team members, but will have the opportunity to interact with James Webb Space Telescope researchers through the virtual world setting, which allows for synchronous interactions. Halfway through the challenge, design solutions will be critiqued and a mystery problem will be introduced for each team. The top five teams will be invited to present their work during a synchronous Education Forum April 14, 2011. The top team will earn scholarships and technology. This is an excellent opportunity for professionals in both astronomy and associated engineering disciplines to become involved with a unique educational program. Besides the chance to mentor a group of interested students, there are many opportunities to interact with the students as a guest, via chats and presentations. 248.09 Astronomy 101 in Washington State High Schools Julie H. Lutz1, S. Garner1, T. Stetter1, J. McKeever1, V. Santo Pietro2 1Univ. of Washington, 2Shoreline High School. Exhibit Hall The University of Washington in the High School (UWHS) program enables high schools to offer the 5 quarter credits Astronomy 101 (Astr 101) course for college credits. The credits are transferable to most colleges and universities. The course provides an alternative to advance placement courses and programs such as Washington's Running Start whereby high school students take courses at community colleges. Astr 101 focuses on stars, galaxies and the universe, as well as background topics such as gravitation, electromagnetic radiation and telescopes. The course satisfies the UW “natural world” and “quantitative/symbolic reasoning” distribution requirements. Students must pay a fee to enroll, but the credits cost less than half what they would cost for the course if taken on one of the UW campuses. The course can be offered as either one semester or full-year at the high school. Teachers who offer Astr 101 must be approved in advance by the UW Astronomy Department, and their syllabi and course materials approved also. Teachers receive orientation, professional development opportunities, classroom visits and support (special web site, answering questions, making arrangements for campus visits, planetarium visits) from astronomy department course coordinator. The UWHS Astr 101 program has produced positive outcomes for the astronomy department, the participating teachers and the students who complete the course. In this poster we will discuss our 5 years of experience with offering Astr 101, including benefits to the students, teachers, high schools, university and department, student outcomes, course assessments and resources for offering the course. 248.10 Educational Aspects of Searching for Variable Stars in the Mid-IR Sky Margaret (Peggy) Piper1, B. Thomas2, R. DeCoster3, R. Rosignolo1, J. Romero1, J. Christensen1, O. Rudio2, D. Brennan2, A. Antonow3, A. Sehgal3, D. Hoard4, S. Howell5 1Lincoln-Way North High School, 2North Middle School, 3Niles West High School, 4Spitzer Science Center, 5NOAO. Exhibit Hall Using archival Spitzer Space Telescope Infrared Array Camera (IRAC) data, our team of students, educators and astronomers attempted to discover new variable stars in mid-infrared (3-8 micron) wavelengths. Our educational goal was to learn, and then disseminate, methods to ways to (a) utilize various image processing software tools and (b) subsequently analyze and display gathered data in a meaningful form in order to identify variable stars. We processed a total of 6447 images in three target fields, examining a total of 227 stars for this project. Photometric data were produced for each point source and that data was used to create light curves and brightness vs. standard deviation curves. Our target fields were taken from Spitzer observations of exoplanet transits, which utilized comparatively long, uninterrupted sequences of IRAC observations. This poster will illustrate how students and teachers learned to use imaging software to gather and display photometric data for targets in this project, and created tutorials to enhance the use of these tools in astronomy classrooms. This work was supported by the NASA’s Spitzer Science Center and NOAO (National Optical Astronomy Observatory). 248.11 Authentic Astronomy Research Experiences for Teachers: the NASA/IPAC Teacher Archive Research Program (NITARP) Luisa M. Rebull1, V. Gorjian2, G. Squires1, NITARP Team 1Caltech, 2JPL. Exhibit Hall How many times have you gotten a question from the general public, or read a news story, and concluded that "they just don't understand how real science works"? One really good way to get the word out about how science works is to have more people experience the process of scientific research. The way we have chosen to do this, since 2004, is to provide authentic research experiences for teachers using Spitzer data. (The program used to be called the Spitzer Teacher Program for Teachers and Students, and in 2009 was rechristened NITARP, the NASA/IPAC Teacher Archive Research Program.) We partner small groups of teachers with a mentor astronomer, they do research as a team, write up a poster, and present it at an AAS meeting. The teachers incorporate this experience into their classroom, and their experiences color their teaching for years to come, influencing 100s of students per teacher. Four different teams from the 2010 class of NITARP teachers are presenting scientific and educational results at this AAS meeting; please look for them! 248.12 Using NASA Archives in High Schools to Study AGN Helen Petach1, T. Spuck1, K. Meredith1, E. Ramseyer1, V. Gorjian2 1NASA-NITARP, 2JPL. Exhibit Hall The NITARP (NASA IPAC Teacher Archive Research Project) program provides a link between NASA researchers and high school teachers and students. This past year the Luminous Data Miners (LDM) developed and implemented a research plan to investigate whether the UV light emitted from the accretion disk of an Active Galactic Nucleus (AGN) is correlated with the IR emission from its surrounding dust. Contemporaneous data was obtained from the GALEX and Spitzer data archives for a set of galaxies. Scientists, teachers, and students from across the country work together in this authentic research experience. Students learned about the physics of the science in question, the structure of the archived data stored in NASA databases, extraction methods for obtaining relevant data, use of photometry tools to make brightness measurements, and relevant correlations that could be determined. Our results suggest that students are eager to have these research opportunities and will make use of data archives to carry out research projects to answer relevant questions. This poster will highlight the process the students and teachers went through and the tools they developed along the way. 248.13 Multi-Sensory Approach to Search for Young Stellar Objects in CG4 Vivian L. Hoette1, L. M. Rebull2, K. McCarron3, C. H. Johnson4, C. Gartner5, J. VanDerMolen5, L. Gamble6, L. Matche5, A. McCartney5, M. Doering6, R. Crump4, A. Laorr4, K. Mork4, E. Steinbergs4, E. Wigley4, S. Caruso4, N. Killingstad4, T. McCanna4 1University of Chicago, Yerkes Observatory, 2SSC/IPAC/CalTech, 3Oak Park and River Forest High School, 4Breck School, 5Wisconsin School for the Deaf, 6Wisconsin Center for the Blind and Visually Impaired. Exhibit Hall Individuals with disabilities - specifically individuals who are deaf or hard of hearing (DHH) and/or blind and visually-impaired (BVI) - have traditionally been underrepresented in the fields of Science, Technology, Engineering, and Math (STEM). The low incidence rate of these populations, coupled with geographic isolation, creates limited opportunities for students to work with and receive mentoring by professionals who not only have specialty knowledge in disability areas but also work in STEM fields. Yerkes Observatory scientists, along with educators from the Wisconsin School for the Deaf, the Wisconsin Center for the Blind and Visually Impaired, Breck School, and Oak Park and River Forest High School, are engaged in active research with a Spitzer Science Center (SSC) scientist. Our ultimate goals are threefold; to engage DHH and BVI students with equal success as their sighted and hearing peers, to share our techniques to make astronomy more accessible to DHH and BVI youth, and to generate a life-long interest which will lead our students to STEM careers. This poster tracks our work with an SSC scientist during the spring, summer, and fall of 2010. The group coauthored another AAS poster on finding Young Stellar Objects (YSO) in the CG4 Nebula in Puppis. During the project, the students, scientists and teachers developed a number of techniques for learning the necessary science as well as doing the required data acquisition and analysis. Collaborations were formed between students with disabilities and their non-disabled peers to create multi-media projects. Ultimately, the projects created for our work with NITARP will be disseminated through our professional connections in order to ignite a passion for astronomy in all students - with and without disabilities. This research was made possible through the NASA/IPAC Teacher Archive Research Project (NITARP) and was funded by NASA Astrophysics Data Program and Archive Outreach funds. 248.14 Building Astronomy Curriculum to Include the Sight Impaired: Week long summer camp activities for Middle School Students adherent to Washington State Curriculum Standards (EARL's) Natalie Ramien1, S. R. Loebman1, V. Player2, A. Larson1, N. B. Torcolini3, A. Traverse1 1University of Washington, 2Shanghai Community International School, China, 3Stanford. Exhibit Hall Currently astronomy learning is heavily geared towards visual aids; however, roughly 10 million people in North America are sight impaired. Every student should have access to meaningful astronomy curriculum; an understanding of astronomy is an expectation of national and state science learning requirements. Over the last ten years, Noreen Grice has developed Braille and large print astronomy text books aimed at sight impaired learners. We build upon Grice's written work and present here a five day lesson plan that integrates 2D reading with 3D activities. Through this curriculum, students develop an intuitive understanding of astronomical distance, size, composition and lifetimes. We present five distinct lesson modules that can be taught individually or in a sequential form: the planets, our sun, stars, stellar evolution and galaxies. We have tested these modules on sight impaired students and report the results here. Overall, we find the work presented here lends itself equally well to a week long science camp geared toward middle school sight impaired taught by astronomers or as supplemental material integrated into a regular classroom science curriculum. This work was made possible by a 2007 Simple Effective Education and Dissemination (SEED) Grant For Astronomy Researchers, Astronomical Society of the Pacific through funds provided by the Planck Mission, Jet Propulsion Laboratory, California Institute of Technology. 249 Cosmology Poster Session Exhibit Hall 249.01 Enhanced Absorption and Emission in Hydrogen Lines at the Epoch of Recombination D. Cassell1, Vladimir Strelnitski2 1Shippensburg University & Maria Mitchell Obs, 2Maria Mitchell Obs.. Exhibit Hall The important problem of possible disturbances in the Comsic Microwave Background (CMB) left by high n hydrogen transitions during the epoch of recombination has been intensively studied in the past decade. However the simplifying assumptions made in most of the studies may be misleading. We consider the problem from the thermodynamic point of view to show that (1) the available detailed calculations of hydrogen level populations and ensuing non-equilibrium effects (such as masing) for the ordinary HII regions are not applicable to the recombining expanding Universe; (2) taking into account the collisional interaction of neutral atoms with electrons and ions in computer simulations is crucially important for quantitative predictions of possible spectral disturbances. It appears, in particular, that a proper account for collisions (and the treatment of all the angular momentum sublevels separately) will show the possibility of not only emission but also absorption disturbances left in the CMB by the epoch of recombination. Our approach allows us to estimate only roughly the wavelength domains where the emission and absorption disturbances are anticipated. Challenging computer simulations taking into account collisions and considering the l-substates separately up to the Rydberg levels with n ~ 200 are needed to make more accurate quantitative predictions. This project was supported by NSF/REU grant AST-0851892 and the Nantucket Maria Mitchell Association. 249.02 The Cosmic Infrared Background Experiment: Flight Characterization Of The Ciber Narrow Band Spectrometer. Louis R. Levenson1, J. Battle2, J. J. Bock3, A. Cooray4, V. Hristov1, B. Keating5, D. Lee6, P. Mason1, T. Matsumoto7, S. Matsuura7, U. W. Nam6, T. Renbarger5, I. Sullivan1, K. Suzuki8, T. Wada7, M. Zemcov1 1Caltech, 2JPL, 3JPL, Caltech, 4University of California, Irvine, 5University of California, San Diego, 6KASI, Korea, Republic of, 7ISAS/JAXA, Japan, 8Nagoya University, Japan. Exhibit Hall Subtraction of the Zodiacal light foreground is the dominant source of uncertainty in absolute photometric measurements of the extra-galactic background at near-infrared to optical wavelengths. The second flight of the Cosmic Infrared Background ExpeRiment (CIBER) occurred on July 10th, 2010. CIBER is a NASA sounding rocket experiment carrying four co-aligned instruments including two imaging telescopes with wide passbands centered at 1 and 1.6 microns, respectively, as well as a low resolution spectrometer and a narrow-band spectrometer. THE CIBER spectrometers are absolutely calibrated in collaboration with NIST. The narrow-band spectrometer filter is centered on the Ca II solar Fraunhofer line at 854.2 nm and is designed to measure the equivalent width of the solar line reflected by the interplanetary dust in order to obtain an absolute measurement of the Zodiacal contribution to the infrared sky at that wavelength. In conjunction with measured low resolution spectrum from 700 to 1900 nm, this will provide an accurate independent check of the DIRBE Zodiacal light models. Here we describe the NBS instrument, calibration and in-flight characterization. 249.03 Imaging the Spatial Fluctuations in Cosmic IR Background from Reionization with CIBER Chris Frazer1, J. Bock2, A. Cooray1, M. Kawada3, M. Kim4, D. Lee5, L. Levenson2, T. Matsumoto4, S. Matsumuura3, K. Mitchell-Wynne1, T. Renbarger6, J. Smidt1, I. Sullivan2, T. Arai3, K. Tsumura3, T. Wada3, M. Zemcov2 1University of California, Irvine, 2Caltech, 3Institute of Space and Astronoutical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), Japan, 4Seoul National University, Korea, Republic of, 5Korea Astronomy and Space Science Institute (KASI), Korea, Republic of, 6University of California, San Diego. Exhibit Hall The Cosmic Infrared Background Experiment (CIBER) is a rocket-born absolute photometry imaging and spectroscopy experiment optimized to detect unresolved infrared signatures of first-light galaxies that were present during reionization. The signatures from reionization are theorized to be dominant at the wavelengths upon which CIBER surveys. CIBER consists of two wide field imagers to measure the extragalactic background fluctuations in the H and I-Bands (1.6 and 0.9 microns respectively) of the cosmic infrared background (CIB) as well as two spectrometers designed to take measurements of the foreground zodiacal light and the absolute Extragalactic Background Light (EBL) spectrum They imagers are capable of examining high-redshift (z ~ 10-20) CIB fluctuations which will facilitate in the study of surface densities of sources associated with reionization. Studies of galaxies with similar redshift parameters (z > 6) are largely unaccounted for. The spectrometer configuration consists of one low resolution spectrometer and one narrow band spectrometer. They are respectively designed to take measurements of the absolute Extragalactic Background Light (EBL) spectrum, and foreground zodiacal light. In this poster we present the specifications for both CIBER imagers and detail how the fluctuations from galaxies during reionization will be measured. 249.04 A Constraint On the Integrated Mass Power Spectrum Out to z = 1100 From Lensing of the Cosmic Microwave Background Joseph Smidt1, A. Cooray1, A. Amblard1, S. Joudaki1, D. Munshi2, M. G. Santos3, P. Serra1 1UC Irvine, 2University of Edinburgh, United Kingdom, 3Instituto Superior Tecnico, Portugal. Exhibit Hall The temperature fluctuations and polarization of the Cosmic Microwave Background (CMB) are now a well-known probe of the Universe at an infant age of 400,000 years. During the transit to us from the surface of last scattering, the CMB photons are expected to undergo modifications induced by the intervening large-scale structure. Among the expected secondary effects is the weak gravitational lensing of the CMB by the foreground dark matter distribution. We derive a quadratic estimator that uses the non-Gaussianities generated by the lensing effect at the four-point function level to extract the power spectrum of lensing potential fluctuations integrated out to z ? 1100. Using WMAP 7-year temperature maps, we report the first direct constraints of this lensing potential power spectrum and find that it has an amplitude of AL = 0.96 ± 0.60, 1.06 ± 0.69 and 0.97 ± 0.47 using the W, V and W+V bands, respectively. 249.05 A Cosmological Discriminator Designed to Avoid Selection Bias Amir Shahmoradi1, R. J. Nemiroff1 1Michigan Technological University. Exhibit Hall We define a new cosmological discriminator -- a ``one-sided Amati relation" -- which is defined by only the bright/soft side of the Eiso versus Epeak (Amati) relation, since this does not suffer from significant selection bias. An advantage of this approach is that changing a GRB redshift would only slide it along the one-sided Amati relation, making actual GRB redshifts less important than how GRB brightness and hardness change with cosmological distance. Therefore, it is the slope of this one-sided Amati relation that makes it a cosmological model discriminator. We investigate the limits of the power of this method to discern between cosmological models where dark energy changes with redshift. 249.06 The Small-scale Clustering Of Massive Galaxies At 0.2 1), referred to as "MHD active" grains, and larger grains that are decoupled from the field by collisions with neutral gas particles (Hall parameter < 1), which can be called "MHD inactive" grains. The limiting MHD signal speed for the lowest-frequency, farthest-traveling waves is set by the net mass of the "MHD active" grains that are loaded onto magnetic field lines, which can be a substantial portion (~ 30% - 70%) of the total dust mass. As a result, the limiting MHD signal speed in dusty clouds is significantly smaller than what it would be in dust-free clouds. This can have important consequences for the formation of MHD precursors and shocks in clouds and cores. 251.02 Magnetic Fields in Photodissociation Regions Benjamin Montet1, D. S. Balser2, D. A. Roshi2, J. Shitanishi3, T. M. Bania4, R. T. Rood5 1University of Illinois, 2National Radio Astronomy Observatory, 3University of Southern California, 4Boston University, 5University of Virginia. Exhibit Hall Photodissociation regions (PDRs) are predominately neutral volumes at the molecular cloud/HII region interface of star forming complexes. Far-ultraviolet photons with energies below 13.6 eV can escape HII regions and dissociate atoms with a lower ionization potential, such as carbon, within PDRs. This has been verified, for example, by detection of carbon radio recombination line (CRL) emission from PDRs. Roshi (2007) suggested that the non-thermal component of CRL line width is dominated by magnetic turbulence. He combined data from observations of several CRLs separated in frequency and radiative transfer models of the CRL emission regions to derive the magnetic field strength. Here, we discuss PDR models toward four HII regions using observations from the Green Bank Telescope (GBT) and compare the derived magnetic field strength with published Zeeman observations to test this hypothesis. 251.02 Analysis of MHD Interstellar Turbulence using Tsallis Statistics Benjamin M. Tofflemire1, A. Lazarian2, B. Burkhart2 1University of Washington, 2University of Wisconsin. Exhibit Hall In an effort to characterize interstellar magneto-hydrodynamic (MHD) turbulence, we study probability distribution functions (PDFs) of spacial increments of density, velocity, and magnetic field strength for fourteen three dimensional ideal isothermal MHD simulations. We fit the PDFs using the Tsallis function and study the fit parameters dependence on the compressibility and magnetization of the gas. For three dimensional density, column density, and PPV (Position-Positions-Velocity) data we find that the Tsallis function fits PDFs of high resolution MHD turbulence well, with the fit parameters corresponding to amplitude and width showing strong sensitivities to the sonic and Alfvén Mach numbers. Specifically, the width of the PDF is sensitive to magnetization especially in cases where the sonic number is high. These dependencies are also found for cases where smoothing, noise, and cloud-like boundary conditions are introduced to simulate observable qualities. This could make Tsallis statistics a useful tool in characterizing magnetic fields in the interstellar medium. This work was supported by the National Science Foundation's REU program through NSF Award AST-1004881. 251.03 Driven Hydromagnetic Waves and Shocks in Dusty Interstellar Clouds Maximilian Katz1, G. E. Ciolek1, W. G. Roberge1 1New York Center for Astrobiology and Department of Physics, Applied Physics, and Astronomy Rensselaer Polytechnic Institute. Exhibit Hall Dust grains are an important component of star-forming molecular clouds. Grains play a fundamental role in interstellar chemistry, and as a consequence of this, they may contribute to reactions of astrobiological interest. Under typical conditions, most dust grains are electrically charged, and will be a source of electrical current, in addition to gas-phase ions and electrons. Depending on their size, the gas density, and the field strength, charged dust grains can couple to the magnetic field and become loaded onto the field lines threading a cloud. As a result of this coupling, grains can significantly alter magnetohydrodynamic (MHD) phenomena in star-forming regions. Using linear algebra and Fourier transform methods, we have created a numerical code that calculates the time-dependent evolution of MHD disturbances that propagate perpendicular to the direction of the magnetic field within weakly ionized, dusty interstellar clouds and cores. We apply this code to a model of colliding clouds to study the formation and early-time evolution of hydromagnetic waves and shocks. The results of models with grains that are either poorly coupled or strongly coupled to the magnetic field are described and contrasted. We find that in clouds with strong coupling, the inertia added by grain loading on magnetic field lines dramatically reduces the rate at which a MHD signal --- the forerunner to a magnetic precursor --- propagates ahead of the shock, compared to that which occurs in models with poorly coupled grains. 251.03 Constraining Galactic Dynamo Models with NIR Polarimetry Michael D. Pavel1, D. P. Clemens1, A. F. Pinnick1 1Boston University. Exhibit Hall Polarization of background starlight is used to probe interstellar magnetic fields. While it has been widely used at optical wavelengths, the near-infrared polarimetric sky remains largely unexplored. In addition to probing longer sightlines, NIR polarimetry is less affected by foreground magnetic structures which allows us to study the large-scale, quiescent Galactic magnetic field. We combine observed NIR polarimetry with simulated observations to constrain dynamo models of the Galactic magnetic field. Polarimetric data were obtained with the Mimir instrument on the Perkins Telescope along a line of constant Galactic longitude (l=150) with pointings spaced between -75 1 kpc. This naturally produces the warm ionized medium through photoionization due primarily to O stars near the plane. However, the hydrodynamical models reproduce the peak but not the width of the emission measure distribution observed in Wisconsin H-Alpha Mapper (WHAM) data. Here, we discuss the role of magnetic fields in the structure of gas away from the plane. We compare emission measure distributions from models with varying magnetic field strengths to the WHAM observations. The simulations were performed using the adaptive mesh refinement grid code FLASH with the new MHD solver developed by Waagan et al. This work was partly supported by NASA/SAO grant TM0-11008X and by NSF grant AST-0607512. 251.07 The Wisconsin H-Alpha Mapper Sky Survey: A First Look at the Global Distribution of Diffuse Ionized Gas in the Milky Way Nitish Chopra1, L. M. Haffner1, R. J. Reynolds1, G. J. Madsen2, A. S. Hill1, K. A. Barger1, K. P. Jaehnig1, E. J. Mierkiewicz1, J. W. Percival1, N. M. Pingel1, D. T. Reese1, M. C. Gostisha3 1University of Wisconsin-Madison, 2Sydney Institute for Astronomy, School of Physics, University of Sydney, Australia, 3University of Wisconsin-Whitewater. Exhibit Hall After a year of observations from its new location on Cerro Tololo, the Wisconsin H? Mapper (WHAM) has nearly completed survey observations below ? < -30°. This new data combined with the Northern Sky Survey provides the first kinematic, all-sky survey of diffuse H? from the Milky Way. Aside from many large-scale, locally-ionized regions, much of this emission arises from the Warm Ionized Medium (WIM), a diffuse but thick component of the ISM that extends several kiloparsecs into the Galactic halo. WHAM was designed primarily to study the WIM, delivering a spatially integrated spectrum from a one-degree beam on the sky covering 200 km s-1 with 12 km s-1 spectral resolution. The short exposures of the survey reach sensitivity levels of about 0.1 R (EM ? 0.2 pc cm-6) and reveal emission toward nearly every direction in the sky. Here, we present our early efforts at reducing this new southern dataset and offer a first look at the global distribution and kinematics of diffuse ionized gas throughout the Galaxy. WHAM and the research presented here are funded by NSF award AST-0607512. We also thank the excellent and responsive staff at CTIO in Chile for helping to keep our remote installation fully operational. 251.08 WHAM Discovery of a New Superbubble in Circinus Martin Gostisha1, R. A. Benjamin1, L. M. Haffner2 1UW-Whitewater, 2UW-Madison. Exhibit Hall We present a Wisconsin H-alpha Mapper (WHAM) survey of the fourth quadrant of the Galactic plane in diffuse emission from [S II] 6716 A, covering Galactic longitude l=270-360 degrees and latitude |b|<12 degrees. One of the more prominent features seen is a large-scale ionized bubble, centered at l=320.0 deg, b=3.4 deg with a diameter of 7 degrees. Spectra of the center of this region shows line splitting characteristic of an expanding bubble. A search for high mass star in the region shows that this bubble subtends over 40 O stars, including the cluster Pismis 20 which is part of the Circinus OB association. Assuming that the bubble is at the distance of this cluster, yields a bubble diameter of 300 parsec. When this is combined with the measured expansion velocity of 7 km/s, we derive a bubble age of approximately 2 Myrs, consistent with the estimated age of the Circinus OB association. We discuss the energetics of the bubble as well as the result of searching for this bubble using tracers at other wavelengths. This research was supported the NSF REU site grant to the University of Wisconsin-Madison. 251.09 Studying the Temperature and Ionization State of the Warm Ionized Medium Melissa Halford1, E. J. Mierkiewicz2, R. J. Reynolds2, G. J. Madsen3, L. M. Haffner2, K. A. Barger2, F. L. Roesler2 1Cornell University, 2University of Wisconsin-Madison, 3University of Sydney, Australia. Exhibit Hall Using data from the Wisconsin Hydrogen Alpha Mapper (WHAM) and Pine Bluff Observatory's Spatial Heterodyne Spectrometer (SHS), we studied the warm ionized component of the Galaxy's interstellar medium (WIM). Line ratios of H-alpha, [N II], [O II] and [S II] emission were used to study the WIM gas in both the local spiral arm and more distant areas of the Galaxy. The strength of the [S II] line was used to measure the ionization state in a set of nine look directions and ratios of [N II]/H-alpha and [O II]/H-alpha provide a measure of temperature. Our study expands upon and confirms the results of previous [O II] studies of the WIM, which limited themselves to line ratios including only the local component of the [O II] emission. The work presented here includes a detailed component analysis of WIM emission from non-local gas in the kinematically distinct Perseus spiral arm and uses [S II] data that was not available in the previous [O II] study. This work was supported by the National Science Foundation's REU program through NSF Award AST-1004881. WHAM is funded by the National Science Foundation through grant AST-0607512; the [OII] SHS is funded by the National Science Foundation through grant AST-0908894. 251.10 Probing Our Heliospheric History: Constructing A Density Profile Of The LISM In The Sun’s Rearview Mirror. Katherine Wyman1, S. Redfield1 1Wesleyan University. Exhibit Hall In the course of our motion through the Galaxy, the Solar System has encountered many interstellar environments of varying characteristics. ISM density variations spanning six orders of magnitude are commonly seen throughout the general Galactic environment, and a sufficiently dense cloud within this range has the potential to compress the heliosphere to within one Astronomical Unit. We present a reconstruction of the density profile for the clouds we have most recently passed through based on high-resolution optical spectra towards nearby stars. The data were obtained with the Harlan J Smith 2.7-meter telescope coudé spectrograph at McDonald Observatory. Observations were made of interstellar NaI and CaII doublet absorption towards 49 bright stars along the historical path of solar motion in our orbit around the center of the Galaxy. Spectra were taken of stars out to a distance of 480 parsecs, with a median separation distance of 5 parsecs between adjacent stars. No absorption is seen out to a distance of 120 pc (consistent with the Local Bubble), but a complex collection of absorbers (up to 10 components) is seen in stars between 130 and 480 pc. A possible link between our local interstellar environment, cosmic rays, and our planetary climate has long been a subject of interest to members of the astronomical community. Compression of the heliosphere (one of our three cosmic ray shields) due to passage through a dense interstellar cloud could have drastic effects on Earth’s climate: global cooling (atmospheric dust deposition), weather patterns (cloud nucleation), and evolution (DNA mutations). A timescale of interaction with each ISM component in this path can be constructed and ultimately compared with Earth’s geologic record. 251.11 Analysis Of Ultra Compact Ionized Hydrogen Regions Within The Northern Half Of The Galactic Disk John Bruce1 1Manchester College. Exhibit Hall From a catalog of 199 candidate ultra compact (UC) HII regions 123 sources included in the the intersection of the GLIMPSE (8 ?m),Cornish (6 cm), and Bolocam (~1.1 mm) galactic plane surveys (BGPS) were analyzed. The sources were sorted based on 6 cm morphology and coincidence with 8 ?m bubbles. The ~1.1 mm flux attributes were measured and calculations were performed to determine the ionized hydrogen contributions to the ~1.1 mm flux. The category averages and frequencies were obtained as well. Significant differences in HII percentages were present among the morphology groups but ranged widely, without apparent distinction, between the bubble forming and triggered source categories. 251.12 H? Survey of Emission Line Regions in M33 and Local Group Dwarf Galaxies Cindy Blaha1, T. Johnson1, R. Cawthon1, M. Dixon1, C. Murray1, P. Massey2, P. Hodge3 1Carleton College, 2Lowell Observatory, 3University of Washington. Exhibit Hall We present the results of a survey of H ? emission line regions in M33 and seven dwarf galaxies in the Local Group (NGC6822, IC10, WLM, Sextans A and B, Phoenix and Pegasus). Using data from the Local Group Galaxy Survey (LGGS - see Massey et al, 2006)), we used continuum-subtracted H? emission line images to define emission regions with a faint flux limit of 10 -17 ergs-sec-1-cm-2 above the background. We have obtained photometric measurements for over 4000 H ? emission regions in M33 and five of the seven dwarf galaxies. Using these regions, with boundaries defined by their H ?-emission, we also determined fluxes for the continuum-subtracted [OIII] and [SII] images and constructed a catalog of H ? fluxes, region sizes and [OIII]/ H ? and [SII]/ H ? line ratios. The H?? region luminosity functions and size distributions for spiral galaxy M33 are compared with those of the dwarf galaxies NGC 6822 and IC10. For M33, the average [SII]/ H ? line ratios, plotted as a function of galactocentric radius, display a linear trend with a very shallow slope. The galaxy-wide averages of [SII]/ H ? line ratios correlate with the masses of the dwarf galaxies following the previously established dwarf galaxy mass-metallicity relationship. An interactive catalog of these LGGS emission line surveys will be made available on-line. 251.13 Wind Bubbles around Massive Stars: Ionization-Gasdynamics Modelling and X-ray Emission Calculations Vikram Dwarkadas1, D. Rosenberg2 1Univ. of Chicago, 2National Center for Atmospheric Research. Exhibit Hall Using a code that employs a self-consistent method for computing the effects of photo-ionization on circumstellar gas dynamics, we model the formation of wind-driven nebulae around massive stars. Our algorithm incorporates a simplified model of the photo-ionization source, computes the fractional ionization of hydrogen due to the photo-ionizing flux and recombination, and determines self-consistently the energy balance due to ionization, photo-heating and radiative cooling. We take into account changes in stellar properties and mass-loss over the star's evolution. Our multi-dimensional simulations clearly reveal the presence of strong ionization front instabilities, similar to those seen in galactic ionization fronts. In this poster we describe the code, and show how inclusion of photo-ionization affects the wind bubble structure and dynamics. Using various X-ray emission models, we compute the X-ray flux and spectra from our wind bubble models, and compare to observed data. VVD's research is supported by grant TM9-0001X provided by NASA through the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. 251.14 More Samples of Massive Star Forming Complexes in the Spitzer GLIMPSE Survey Eve J. Lee1, N. Murray1, M. Rahman1 1University of Toronto, Canada. Exhibit Hall In previous work, we identified 40 star-forming complexes (SFCs) in the 13 most luminous WMAP free-free sources, using Spitzer GLIMPSE and Midcourse Space Experiment surveys. The bubbles were interpreted as an evidence of radial expansion due to a central massive star cluster. The high free-free luminosity and negligible synchroton radiation demonstrated that the initial driver of the bubbles were not supernovae. Meanwhile, the energy injected into the interstellar medium by the bubbles was found to be similar to that required to maintain turbulent motion in the gas disk inside 8 kpc. In this work we report the identification of approximately 200 new SFCs in the 83 WMAP free-free sources using a combination of bubble morphology in 8 micron emission, radio recombination, and molecular line radial velocities. We also recover approximately 80% of the previously found 40 SFCs. We determine the expansion velocity, physical distance, and radius for all the complexes. We report their expansion kinetic energy and its relation to turbulent motion in the interstellar medium. 251.15 The Milky Way Project: Citizen Science with GLIMPSE Robert Simpson1, Milky Way Project Team 1Oxford University, United Kingdom. Exhibit Hall The infrared Spitzer GLIMPSE Survey mapped the midplane of the Milky Way in exquisite detail (Benjamin et al., 2003; Churchwell et al. 2009). Features such as bubbles (HII regions, supernova remnants - Churchwell et al. 2006; 2007) and extended green objects (EGOs - Cyganowski et al. 2008) were extracted from these data through visual classification by a handful of researchers. The Zooniverse (Galaxy Zoo, Moon Zoo - http://www.zooniverse.org) aims to use GLIMPSE/MIPSGAL data, in conjunction with new GLIMPSE 360 data (Whitney et al. 2009), produce definitive maps of such structures through a new citizen science website. A set of online tools have been developed that allow the public to draw the locations and sizes of such objects onto the GLIMPSE/MIPSGAL data. 'The Milky Way Project' will utilize the Zooniverse user base of over 320,000 volunteers to produce detailed catalogues of bubbles, and intermediate-mass young stellar objects (YSOs) in the GLIMPSE/MIPSGAL data. It will also aim to locate EGOs, identified by their bright 4.5 micron emission (Cyganowski et al. 2008). The science team will then perform a variety of follow-up work based on these catalogues. Additionally we will ask users to identify interesting or unusual objects that they spot within the GLIMPSE/MIPSGAL images. These catalogues of objects, which will include star clusters (e.g. Mercer et al., 2005), stellar bowshocks (e.g. Povich et al. 2008; Kobulnicky, Gilbert and Kiminki 2010) and galaxies in the zone of avoidance (e.g. Marleau et al., 2009) can then be used to guide future research. 'The Milky Way Project' is the ninth citizen science project from the Zooniverse. As more data become available (e.g. from Herschel's HiGAL survey), the project aims to expand and look at other, more diverse features in far-infrared and submillimetre data. 251.16 Stereo 3-D Presentation of Hubble Space Telescope Imagery Zoltan G. Levay1, G. Bacon1, H. E. Bond1, T. M. Borders1, C. A. Christian1, L. M. Frattare1, F. Hamilton1, W. Januszewski1, M. Livio1, M. Mutchler1, K. S. Noll1, F. Summers1 1STScI. Exhibit Hall 3-dimensional (3-D) visualizations are a means of adding depth to otherwise 2-dimensional images. For astronomical images, depth is frequently not measured, but relative depth relationships can be inferred. We present a 3-D visualization of a portion of the Carina Nebula imaged with the Hubble Space Telescope. The source image is a color composite of two datasets obtained with the Advanced Camera for Surveys. Images in the H?+[N II] filter (F658N) were taken from a 2005 Carina Nebula survey mosaic by Smith et al. (2010, MNRAS, 405, 1153). Images in the [O III] filter (F502N) were obtained by our team in 2010 in parallel to WFC3 observations of the nearby HH 901 region (HST proposal 12050). A 3-D model was constructed from the color composite image by separating it into several planes. Stars and nebular structures were extracted from the image and placed on different planes in 3-D digital modeling software using morphology of nebular features to infer relative depth. Relief texture was added to some of the nebular structures in the model to further enhance the perception of depth. For a static image, frames rendered from the 3-D model at two different viewpoints are composited into a single image in anaglyph (red-blue) stereo that will be shown. 251.17 FUV Images and Physical Properties of the Orion-Eridanus Superbubble Region Young-soo Jo1, K. Min1, K. Seon2 1Korea Advanced Institute of Science and Technology (KAIST), Korea, Republic of, 2Korea Astronomy and Space Science Institute (KASI), Korea, Republic of. Exhibit Hall The far-ultraviolet (FUV) C IV and H2 emission spectra of Orion-Eridanus Superbubble (OES) is hereby presented. The OES seems to consist of multiple phase through the detection of highly-ionized gas and pervasive neutral hydrogen. The former is traced by hot gas while the latter is traced by cold medium. A spectral image made with H2 fluorescent emission shows that the spatial distribution of hydrogen molecule is well correlated with the dust map. The model spectra was taken from a photodissociation region (PDR) radiation code which finds a best suitable parameter such as hydrogen density and intensity of the radiation field. C IV emission is caused by intermediate temperature ISM about 105K. Therefore we could get more clear evidence to reveal the morphology of OES. In this process, the hydrogen density and gas temperature were also estimated. The data were obtained with the Far-Ultraviolet Imaging Spectrograph (FIMS) and the whole data handling were followed by previous FIMS analysis. 251.18 Simulating Dusty Wind-Blown Bubbles Jessamy Rogers1, C. Watson1 1Manchester College. Exhibit Hall 24 micron and 70 micron band images of two wind blown bubbles-- N-90 and S-146-- were analyzed and used to constrain the results of a simulation using Cloudy 3D. In particular, the effects of the dust grains in the interior of the bubble were examined, including the impact of distance-variable grain size distributions. It was discovered that the emissions of N-90 were well reproduced by the simulation, although S-146 saw only moderate reproduction. In both cases, the best fit was produced by parameters of questionable realism. 251.19 Modeling the Evolution of Cold Cloud Interstellar Dust-Grain Ices Tyler Pauly1, R. T. Garrod2 1Iowa State University, 2Department of Astronomy, Cornell University. Exhibit Hall We investigate the formation and evolution of interstellar dust-grain ices under cold cloud conditions, with a particular emphasis on CO2. We use a three-phase model (gas/surface/mantle) to simulate the coupled gas--grain chemistry, allowing the distinction of the chemically-active surface from the ice layers preserved in the mantle beneath. We undertake to treat more accurately the quantum-tunneling rates of barrier-mediated surface reactions, and we explicitly consider competition between such reaction rates and thermal hopping processes. These models show excellent agreement with the observed behavior of CO and CO2 ice in the interstellar medium. The observed threshold between regimes in which CO2 or CO is the dominant ice constituent after H2O is found to be caused ultimately by the near-complete gas-phase conversion of atomic carbon to CO, which is itself determined by CO and H2 self-shielding. The change in the availability of gas-phase carbon alters the balance of the grain-surface chemistry, leading to a sharp change-over in the dominance of CO2/CO. The most probable grain-surface production mechanism for CO2 is the formation of a loosely-bound O...CO complex, whose oxygen atom is easily hydrogenated, leaving a highly excited complex which quickly overcomes an activation energy barrier to form CO2 + H. 251.20 Cosmic Origins Spectrograph Observations Of A Dense Translucent Cloud Theodore P. Snow1, E. B. Burgh1, J. P. Destree1 1Univ. of Colorado. Exhibit Hall Cosmic Origins Spectrograph Observations of a Dense Translucent Cloud Theodore P. Snow Eric B. Burgh Joshua P. Destree The Cosmic Origins Spectrograph (COS) has greater sensitivity at moderate resolution than any UV spectrograph before 2009. One of the COS programs is to obtain UV spectra of interstellar translucent clouds. In these clouds H2 is expected to dominate over H I and carbon should be making the transition from C II to C I to CO. Now we have obtained spectra of NGC 2024 No. 1, the most reddened star in our program. This sightline conforms to the definition of an extreme translucent cloud, with H2 far dominating over H I by two orders of magnitude while CO contains most of the carbon. This would be classified as dark cloud but for the fact that UV radiation passes through it - with difficulty. We present column densities of H I, H2 (inferred from the good correlation with CH), and CO. We have also obtained COS spectra of a few other stars, notably Cyg OB 8A and HD 204287, and we compare them with NCG 2024 No. 1. Forthcoming observations will establish abundances of other neutral atoms, ionized species, and simple molecules. 251.21 On the Excitation of “Quasi-thermal” Lines of Methanol Adam Michael1, M. Baubock2, V. Strelnitski3 1Wesleyan U. & Maria Mitchell Obs., 2Boston U. & Maria Mitchell Obs., 3Maria Mitchell Obs.. Exhibit Hall We revisit the problem of the excitation of “quasi-thermal” lines of methanol in dense molecular clouds. Our analysis is based on the observations of 13 clouds in the four rotational lines of E-methanol (J0 - J-1 ; J =1-4) at 157 GHz using the 12-m ARO telescope on Kitt Peak (AZ) and on comparison of the results with the steady-state solutions for the level populations in a Monte-Carlo simulation of radiative transfer. A higher spectral resolution allowed us to deconvolve the blended 10-1-1, 20-2-1 and 30-3-1 lines better than in previous works. Treating the 157 GHz lines as spontaneous and optically thin, we estimate the relative populations of the J =1 to 4 levels in the K= 0 stack. Most of the sources demonstrate strong deviations from the thermal population distribution with a single excitation temperature. A number of them can be divided into two groups showing the signatures of either “Class I” or “Class II” pumping. This dichotomy is probably determined by the distance of the bulk of the observed gas from the closest IR source controlling the strength of the “Class II” pumping. However, a considerable number of sources do not fit into either class, some of them showing, in particular, a significant overheating of the 40-30 transition not predicted by either pumping model. This discrepancy can be due to oversimplification of our theoretical model. This project was supported by NSF/REU grant AST-0851892 and the Nantucket Maria Mitchell Association. 251.22 Grain Alignment in Starless Cores Terry Jay Jones1, M. Krejny1, B. Andersson2, P. Bastien3 1Univ. of Minnesota, 2SOFIA Science Center, USRA, 3Univ. of Montreal, Canada. Exhibit Hall We present observations of the polarization at 2.2 microns of background field stars shining through dense molecular cloud cores with no ongoing star formation, so-called 'starless cores'. This allows us to extend the work of Whittet et al. to Av > 40 mag. We compare these results to previous polarimetry of background field stars and embedded YSO's. We find that beyond Av ~ 12 mag., the observations are consistent with the absence of polarizing grains at these extreme optical depths. This is in contrast for lines of sight to embedded YSO's, which maintain increasing polarization with optical depth up to Av = 100 mag. 251.23 Spatially Resolved H2 Line Ratios in the HH7 Bow Shock Rosemary E. Pike1, T. R. Geballe1, A. C. Chrysostomou2, M. G. Burton3, P. W. J. L. Brand4 1Gemini Observatory, 2Joint Astronomy Center, 3University of New South Wales, Australia, 4Royal Observatory, United Kingdom. Exhibit Hall We have obtained K-band spectra, at R~5,000 and 0.3 arc-second angular resolution, of the HH7 bow shock, using the Near-infrared Integral Field Spectrograph (NIFS) at Gemini North. The spectra include H2 lines covering a wide range of upper state energy levels, from ~6,000 K to ~25,000 K. We have measured the strengths of the rovibrational H2 lines 1-0 S(0) through S(2) and Q(1) through Q(4); 2-1 S(0) through S(3); 3-2 S(0) through S(3); and 4-3 S(3) and S(4). The H2 line intensity ratios will be used to determine the excitation temperature at different positions in the bow shock. Continuous shock (C-shock) models with ionized gas and magnetic mediation tend to predict that the temperature is constant through much of a shocked gas column and thus that the excitation temperature at each position will be independent of which line ratios are used to calculate it, but will vary with location in the bow shock. In the jump shock (J-shock) scenario, in which the gas is heated very suddenly and begins to cool immediately, the excitation temperature varies through the post-shock gas and line ratios depend on the line pair chosen. In this case one would expect to observe the same variation in excitation at all locations. Previous observations of shocks in a number of molecular clouds seem to support the J-shock behavior, but this may be a product of insufficient angular resolution, with previous observations unable to resolve separate shock fronts. Our angular resolution over the 3 x 3 arc-second field of view positioned along the bow shock of HH7 is an improvement by a factor of five over previous observations. 251.24 Monte-carlo Simulation For Dust Scattering In The Ophiuchus Molecular Complex Lim Tae-Ho1, K. Min1, K. Seon2 1KAIST, Korea, Republic of, 2KASI, Korea, Republic of. Exhibit Hall We present the results of FUV dust scattering simulation, which is based on the Monte-Carlo method. In this simulation, we focus on the multiple scattering in the Ophiuchus complex region because the single scattering case in the region already reported by Lee et al. 2008. We compare the simulation result to the FUV intensity with FIMS and the single scattering result. We also discuss the parameters related to the results of this simulation, such as asymmetry factor, albedo and other different setting-ups. 251.25 Investigating the Density Structure of Bok Globule CB188 Andrew Johnson1, A. C. Updike1, D. H. Hartmann1 1Clemson. Exhibit Hall Extinction effects are ubiquitous in the interstellar medium of galaxies. In particular, extinction due to molecular clouds can significantly change the color and brightness of background or embedded objects. The structure of molecular clouds is an important observable, relevant for the initial conditions under which star formation takes place. Mapping the effects of extinction across a molecular cloud can be used to deduce its internal structure. We present such an analysis for Bok Globule CB188 which we observed with the 0.9m SARA telescope at Kitt Peak National Observatory. The geometry of CB188 is such that it can be approximated by a spherical model. We investigate several possible density structures (such as constant density and the Bonnor-Ebert model) and compare them to our observations of a changing apparent radius as a function of wavelength. This project was funded by the National Science Foundation Research Experiences for Undergraduates (REU) program through grant NSF AST-1004872. 251.26 The CO Isotope Ratio of the Large Magellanic Cloud Sarah Wyss1, J. Ott1, D. Meier2, T. Wong3, A. Hughes4, J. Pineda5, E. Muller6 1National Radio Astronomy Observatory, 2New Mexico Institute of Mining and Technology, 3University of Illinois, 4Swinburne University of Technology, Australia, 5Jet Propulsion Laboratory, 6Nagoya University, Japan. Exhibit Hall Giant molecular clouds (GMCs) are the home of star formation, yet are difficult to observe and thus their physical characteristics remain largely unknown. The proximity, size, inclination and star-forming properties of the Large Magellanic Cloud (LMC, distance 50kpc) present a perfect opportunity for a comprehensive, high-spectral-resolution and high-spatial-resolution survey of these clouds. Using the 12CO (1-0) and 13CO (1-0) Magellanic Mopra Assessment (MAGMA) data, we study over 155 giant molecular clouds distributed throughout the LMC at 8pc resolution. The 13CO (1-0) transition is detected at or above the level of significance in all clouds examined. The intensity ratio of the 13CO (1-0) to 12CO (1-0) transitions is found to be highly uniform across the LMC, not varying strongly with GMC evolutionary state, galactocentric regions, star formation rate or interaction with the Milky Way. We discover an unexplained correlation between 12CO average brightness temperature and the isotope intensity ratio. We produce galaxy-wide spectra in 12CO (1-0) and 13CO (1-0) and examine the galaxy-wide 13CO (1-0) to 12CO (1-0) ratio, simulating observations of similar, more distant galaxies. Comparison of this ratio with the ratio measured locally from individual clouds yields an overall 13CO (1-0) filling factor of 0.3 of 12CO(1-0). 251.27 Infrared Study of Star Forming Regions in the Magellanic Clouds via Spitzer Brandon L. Lawton1, K. D. Gordon1, SAGE-LMC Spitzer Legacy Team, SAGE-SMC Spitzer Legacy Team 1STScI. Exhibit Hall The study of the infrared properties of star forming regions allows us to probe the nature of the UV obscuring dust and the central ionizing stellar populations. The close proximity of the Magellanic Clouds allows us to probe the nature of these star forming regions at small spatial scales. We present the photometry and results of the first infrared-selected star forming region catalogs of the LMC and SMC using the Spitzer Space Telescope and compare the results to H-alpha selected catalogs in the literature. The sources are selected in 24um via a clump-finding algorithm. An analysis of star forming region infrared spectral energy distributions, luminosity functions, size distributions, and computed star formation rates are explored, with differences between the LMC and SMC highlighted. 251.28 Detection Of New High Velocity Clouds Using The Leiden-Argentina-Bonn Hi All-sky Survey Tyler Engel1, B. Wakker2, C. Witt1, M. C. Gostisha1, E. Thomson1, L. Stratman1, R. A. Benjamin1 1University of Wisconsin-Whitewater, 2University of Wisconsin-Madison. Exhibit Hall We describe a new effort to use the Leiden/Argentina/Bonn (LAB) Galactic HI survey to update the high-velocity clouds catalog of Wakker and van Woerden (1991). The LAB survey (Kalberla et al 2005) combined the Leiden-Dwingeloo survey (Hartmann and Burton 1997) with a complementary southern sky survey (Arnal et al 2000). This survey provides improved angular spacing (0.5 deg vs. 1 deg) and velocity resolution (1 km/s vs. 16 km/s), although it was less sensitive than previous surveys. We describe how we fit the LAB high velocity gas with Gaussian components, providing three levels of review for the quality of fits, and compare the resulting high velocity cloud catalog to previous results for galactic latitudes greater than b=45 degrees. This research was supported by NASA ATP grant NNX10AI70G to the University of Wisconsin-Whitewater. 251.29 Forbidden Velocity Wings In The Inner-Galaxy ALFA Low-latitude HI (I-GALFA) Survey Ji-hyun Kang1, B. Koo2, S. J. Gibson3, K. A. Douglas4, G. Park2, J. E. G. Peek5, E. J. Korpela6, C. E. Heiles6 1NAIC/Arecibo Observatory, 2Seoul National University, Korea, Republic of, 3Western Kentucky University, 4University of Exeter, United Kingdom, 5Colombia University, 6University of California - Berkeley. Exhibit Hall The faint wing-like features at velocities beyond the velocity boundaries of the Galactic rotation (Forbidden-Velocity Wings, FVWs) in the large-scale position-velocity diagrams of the HI surveys are thought to be associated with dynamical Galactic events. Most of the FVWs do not have counterparts in radio continuum or X-rays. The primary candidates of these FVWs with previously unknown nature are rapidly expanding HI shells of the old Galactic supernova remnants, which are too faint to be visible in other frequencies. We present preliminary results of a search for FVWs in the I-GALFA survey, which has the unprecedented sensitivity and resolution. About 40 FVWs have been identified in the Galactic Plane, 70% of which are smaller and fainter than the previously identified FVWs and are not associated with the known Galactic objects. We present their statistical properties and the HI images of some interesting FVWs. 251.30 Progress On A New Catalog Of Intermediate Velocity Clouds Using The Leiden-Argentina-Bonn HI All-sky Survey Christopher M. Witt1, B. Wakker2, T. D. Engel1, M. C. Gostisha1, E. Thomson1, L. Stratman1, R. A. Benjamin1 1University of Wisconsin-Whitewater, 2University of Wisconsin-Madison. Exhibit Hall We present progress towards the creation of a new all-sky catalog of intermediate velocity clouds using the Leiden/Argentina/Bonn (LAB) Galactic HI survey. We have developed a Gaussian fitting program to fit individual spectra. Each spectra is initially fit automatically with a set of Gaussians, and then reviewed and adjusted, if necessary, by hand by our undergraduate team. When a satisfactory fit is found, it is submitted for review and adjustment by the senior team member. Intermediate clouds and complexes are formed by grouping Gaussian components by velocity and section of the sky. When complete, this will be the first all-sky catalog of intermediate velocity clouds, which can be compared to dynamical models of the Galactic fountain flows. We present preliminary results for the catalog in the sky with Galactic latitude greater than 45 degrees. This research was supported by NASA ATP grant NNX10AI70G to the University of Wisconsin-Whitewater. 251.31 A High Velocity Cloud Detected Towards M13 Barry Welsh1, R. Lallement2, J. Wheatley1 1UC, Berkeley, 2LATMOS-IPSL, France. Exhibit Hall We present HST-COS observations of the interstellar sight-line towards the M13 globular cluster. High velocity gas at V ~ -120 km/s and intermediate velocity gas at V ~ -65 km/s has been detected in many UV absorption lines. The HVC gas is probably associated with the Complex K IVC with a distance of 1.0 < z < 4.7 kpc. This would place the infalling HVC gas far closer than previous estimates of HV clouds surrounding our Galaxy. 252 LSST Posters Poster Session Exhibit Hall 252.01 LSST Observatory and Science Opportunities Zeljko Ivezic1, M. A. Strauss2, J. A. Tyson3, T. Axelrod4, J. S. Bloom5, LSST Collaboration 1Univ. of Washington, 2Princeton Univ., 3Univ. of California Davis, 4Univ. of Arizona, 5Univ. of California Berkeley. Exhibit Hall The LSST design is driven by four science themes: dark energy, Galactic structure, transient objects, and the search for near-Earth asteroids. The LSST will carry out a ten-year imaging survey of 20,000 sq.deg. of the sky in six broad optical bands, with a deep stack reaching r~27.5 (5 sigma, point source). The current design, with an 8.4m (6.7m effective) primary mirror and a 9.6 square degree field of view, will allow about 10,000 square degrees of sky to be imaged to an effective depth of r=24.5 every three nights. The resulting petabytes of data will be made available to the US and Chilean communities for scientific investigations ranging from the properties of near-Earth asteroids, to characterizations of dark energy from strong and weak lensing, galaxy clustering, and distant supernovae. Eleven LSST Science Collaborations are actively laying the groundwork for first light: working on image analysis algorithms and database design, exploring cadence choices, developing commissioning plans, and outlining scientific opportunities. These Collaborations have over 200 members to date, with membership open to the US community via an application process administered by NOAO. 252.02 The LSST: A System of Systems Chuck F. Claver1, G. P. Debois-Felsmann2, F. Delgado3, P. Hascall2, S. Marshall4, M. Nordby2, G. Schumacher3, J. Sebag5, LSST Collaboration 1NOAO/LSST, 2SLAC National Accelerator Laboratory, 3Cerro Tololo Interamerican Observatory, Chile, 4SLAC National Acceperator Laboratory, 5National Optical Astronomy Observatory. Exhibit Hall The Large Synoptic Survey Telescope (LSST) is a complete observing system that acquires and archives images, processes and analyzes them, and publishes reduced images and catalogs of sources and objects. The LSST will operate over a ten year period producing a survey of 20,000 square degrees over the entire [Southern] sky in 6 filters (ugrizy) with each field having been visited several hundred times enabling a wide spectrum of science from fast transients to exploration of dark matter and dark energy. The LSST itself is a complex system of systems consisting of the 8.4m 3-mirror telescope, a 3.2 billion pixel camera, and a peta-scale data management system. The LSST project uses a Model Based Systems Engineering (MBSE) methodology to ensure an integrated approach to system design and rigorous definition of system interfaces and specifications. The MBSE methodology is applied through modeling of the LSST’s systems with the System Modeling Language (SysML). The SysML modeling recursively establishes the threefold relationship between requirements, logical & physical functional decomposition and definition, and system and component behavior at successively deeper level of abstraction and detail. The LSST modeling includes the analysis and documenting the flow of command and control information and data between the suite of systems in the LSST observatory that are needed to carry out the activities of the survey. The MBSE approach is applied throughout all stages of the project from design, to validation and verification, though to commissioning. 252.03 LSST Operations Plan Sidney Wolff1, D. Silva2, R. Blum2, V. Krabbendam2, J. Kantor1, C. Smith3, A. Walker3 1LSST, 2NOAO, 3CTIO. Exhibit Hall The LSST will be operated in survey mode only. The primary goals of LSST operations are to: 1) maintain the end-to-end survey throughput at a level consistent with achieving the goals for the number of individual exposures at the level specified in the Science Requirements Document within 10 years; 2) achieve the specifications on image quality, photometric and astrometric accuracy, etc.; and 3) enable effective use of the data by a broad community of users. In order to maintain the cadence required, the observations, data processing, data quality assurance, archiving, and access for the community must all be highly automated. The LSST operations plan describes the operational model, the facilities required and their locations, and the services that will be provided. 252.04 LSST Education and Public Outreach Suzanne H. Jacoby1, K. D. Borne2, G. Brissenden3, C. A. Christian4, A. A. Henden5, C. J. Lintott6, J. K. Olsen3, E. E. Prather3, M. J. Raddick7, D. M. Ratcliffe8, T. S. Spuck9, M. Subbarao10, G. Squires11, LSST Outreach Advisory Board 1LSST, 2George Mason University, 3University of Arizona, 4Space Telescope Science Institute, 5AAVSO, 6University of Oxford, United Kingdom, 7Johns Hopkins University, 8Wichita State University, 9Oil City High School, 10Adler Planetarium, 11CalTech/IPAC. Exhibit Hall With its open data policy, survey mode of operations and data products with vast potential for discovery, LSST exemplifies the exponential growth of data volumes in astronomy and presents unprecedented opportunities for Education and Public Outreach (EPO). LSST will provide cyberinfrastructure and interfaces enabling users to visualize and interact with data in classrooms, science centers, and individual learning environments. We’re building on new media technologies that emphasize collaboration, communication, and personalization with an emphasis on Citizen Science and authentic research experiences. We present plans, prototypes, and results of EPO efforts underway during LSST Design and Development. 252.05 LSST Telescope and Optics Status Victor Krabbendam1, W. J. Gressler1, J. R. Andrew1, J. D. Barr1, J. DeVries1, E. Hileman1, M. Liang1, D. R. Neill1, J. Sebag1, O. Wiecha1, LSST Collaboration 1NOAO/LSST. Exhibit Hall The LSST Project continues to advance the design and development of an observatory system capable of capturing 20,000 deg2 of the sky in six wavebands over ten years. Optical fabrication of the unique M1/M3 monolithic mirror has entered final front surface optical processing. After substantial grinding to remove 5 tons of excess glass above the M3 surface, a residual of a single spin casting, both distinct optical surfaces are now clearly evident. Loose abrasive grinding has begun and polishing is to occur during 2011 and final optical testing is planned in early 2012. The M1/M3 telescope cell and internal component designs have matured to support on telescope operational requirements and off telescope coating needs. The mirror position system (hardpoint actuators) and mirror support system (figure actuator) designs have developed through internal laboratory analysis and testing. Review of thermal requirements has assisted with definition of a thermal conditioning and control system. Pre-cooling the M1/M3 substrate will enable productive observing during the large temperature swing often seen at twilight. The M2 ULE™ substrate is complete and lies in storage waiting for additional funding to enable final optical polishing. This 3.5m diameter, 100mm thick meniscus substrate has been ground to within 40 microns of final figure. Detailed design of the telescope mount, including subflooring, has been developed. Finally, substantial progress has been achieved on the facility design. In early 2010, LSST contracted with ARCADIS Geotecnica Consultores, a Santiago based engineering firm to lead the formal architectural design effort for the summit facility. 252.06 Performance of the LSST Camera D. Kirk Gilmore1 1Stanford/KIPAC. Exhibit Hall The LSST camera will be the largest digital camera ever built. As such, its design presents a number of challenges. The field of view will be 3.5 degrees in diameter and will be sampled by a 3.2 billion pixel array of sensors. The entire array will be read-out in under 2 seconds, which all lead to demanding constraints on the sensor architecture and the read-out electronics. In addition, given the fast, optical beam (f/1.2), the camera tolerances on the assembly and alignment of the focal plane and optics are tight. The camera also incorporates three large refractive lenses, an array of five, wide-band large filters mounted on a carrousel, and a mechanical shutter. We present an overview of the baseline camera design, with an emphasis on the requirements and expected performance of the design that will allow the camera to meet its scientific objectives. 252.07 End-to-End Simulations of the LSST System K. Simon Krughoff1, Z. Ahmad2, J. Bankert2, D. Bard3, A. J. Connolly1, C. Chang4, R. R. Gibson1, K. Gilmore4, E. Grace2, M. Hannel2, J. G. Jernigan5, L. Jones1, S. M. Kahn4, S. Lorenz2, S. Marshall4, S. Nagarajan2, J. R. Peterson2, J. Pizagno1, A. P. Rasmussen4, M. Shmakova3, N. Sylvestre1, N. Todd2, M. Young2 1University of Washington, 2Purdue University, 3KIPAC/SLAC, 4Stanford/SLAC, 5SSL/UC Berkeley. Exhibit Hall Efficient use of the data produced by the Large Synoptic Survey Telescope (LSST) will require comprehensive a priori knowledge of the impact of telescope design and implementation on the resulting catalogs and images. This includes gross characteristics like per band detection limits (coadded and single frame), as well as fine grained information such as point spread function behavior as a function of focal plane position and limits on the ability of the imaging system and reduction pipelines to accurately determine galaxy shapes. The LSST Image Simulation group is leading the effort to simulate the LSST system from end-to-end to high fidelity. Input catalogs including source variability, moving objects, and cosmological transients are matched to the LSST survey depth of r=28. These catalogs can be used to produce simulated images for excersizing the data reduction pipelines as well as simulated catalogs for calibration, moving object detection, and probing proposed science questions. We present the progress toward end-to-end simulation of the LSST system. 252.08 Visualization of Simulated LSST Images Stuart L. Marshall1, J. Jernigan2, S. K. Kahn1, A. Connolly3, J. R. Peterson4, Z. Ahmad4, J. Bankert4, D. Bard1, C. Chang1, R. Gibson3, K. Gilmore1, E. Grace4, M. Hannel4, L. Jones3, S. Krughoff3, S. Lorenz4, S. Nagarajan4, J. Pizagno3, A. P. Rasmussen1, M. Shmakova5, N. Sylvestre3, N. Todd4, M. Young4 1Stanford/SLAC, 2SSL/UC Berkeley, 3U. Washington, 4Purdue, 5KIPAC/SLAC. Exhibit Hall The Image Simulation team for the Large Synoptic Survey Telescope (LSST) will show a series of sample images for a portion of the full field of view at a resolution of one LSST pixel (0.2 arc second) matching one pixel of a large 6000 x 6000 pixel display that is 7 x 7 feet in size. One full LSST field of view is composed of ~3 billion pixels, meaning that the large display can only show about 1.2 percent of the full field. This full resolution image corresponds to a square with a side that matches ~11 percent of the diameter of the full field. We will also display example full field of view images that include all stars, galaxies and moving objects near the threshold of detection for a 15 second exposure, and zoom in on 6000 X 6000 pixel (20 x 20 arc minute) regions of interest. In addition to these high resolution images, we will present a dynamic movie of the process of simulating each photon. Also we will show a full sky visualization of the catalog and stars, galaxies and moving objects that provide the input for the Monte Carlo image simulator for LSST. 252.09 LSST Astroinformatics And Astrostatistics: Data-oriented Astronomical Research Kirk D. Borne1, K. Stassun2, R. J. Brunner3, S. G. Djorgovski4, M. Graham4, J. Hakkila5, A. Mahabal4, M. Paegert2, M. Pesenson4, A. Ptak6, J. Scargle6, LSST Informatics and Statistics Team 1George Mason Univ., 2Vanderbilt U., 3U. Illinois, 4Caltech, 5College of Charleston, 6NASA. Exhibit Hall The LSST Informatics and Statistics Science Collaboration (ISSC) focuses on research and scientific discovery challenges posed by the very large and complex data collection that LSST will generate. Application areas include astroinformatics, machine learning, data mining, astrostatistics, visualization, scientific data semantics, time series analysis, and advanced signal processing. Research problems to be addressed with these methodologies include transient event characterization and classification, rare class discovery, correlation mining, outlier/anomaly/surprise detection, improved estimators (e.g., for photometric redshift or early onset supernova classification), exploration of highly dimensional (multivariate) data catalogs, and more. We present sample science results from these data-oriented approaches to large-data astronomical research. We present results from LSST ISSC team members, including the EB (Eclipsing Binary) Factory, the environmental variations in the fundamental plane of elliptical galaxies, and outlier detection in multivariate catalogs. 252.10 Inventorying the Solar System with LSST R. Lynne Jones1, M. E. Brown2, P. A. Abel3, S. R. Chesley4, J. Durech5, Y. R. Fernandez6, A. W. Harris7, M. J. Holman8, Z. Ivezic9, R. Jedicke10, M. Kaasalainen11, N. A. Kaib12, Z. Knevezic13, A. Milani14, A. Park15, D. Ragozzine8, S. T. Ridgway16, D. E. Trilling17, B. Vrsnak18, LSST Solar System Science Collaboration 1Univ. of Washington, 2CalTech, 3PSI/NASA Johnson, 4JPL, 5Charles University, Czech Republic, 6University of Central Florida, 7Space Science Institute, 8Center for Astrophysics, 9Univ. of Washington, University of Zagreb, 10Institute for Astronomy, 11University of Helsinki, Finland, 12CITA, Canada, 13Astronomy Observatory Belgrade, Serbia, 14University of Pisa, Italy, 15University of Victoria, Canada, 16NOAO, 17Northern Arizona University, 18Hvar Observatory, Croatia. Exhibit Hall Near the ecliptic, LSST is expected to detect approximately 4000 moving objects per 9.6 square degree field of view. Each pointing (with mag limits r~24.5) will be revisited within 30-45 minutes, several times per month. Automated software will provide the means to link these individual detections into orbits. The result will be publicly available catalogs of hundreds of thousands of NEOs and Jupiter Trojans, millions of asteroids, tens of thousands of TNOs, as well as thousands of other objects such as comets and irregular satellites of the major planets. These catalogs will contain final orbits as well as the individual (multi-color) observations, calibrated to high precisision in astrometry (~50 mas) and photometry (~0.01 mag). With these large datasets, LSST will provide new insights into links between populations of moving objects, such as the relationship between Main Belt asteroids and NEOs. Models of solar system evolution, such as the Nice model, can be tested against an order of magnitude larger statistical sample, providing much stronger constraints than are currently possible. With high accuracy multi-color photometry, lightcurves and colors will be determined for a significant fraction of the objects detected. Using sparse lightcurve inversion, spin state and shape models will be derived for tens of thousands of main belt asteroids. Derivation of proper elements for Main Belt asteroids will greatly enlarge existing asteroid families, particularly at smaller sizes, and precise color information will facilitate further division. More unpredictable discoveries, such as the potential for observing a real-time collision, could lead to new insights into physical properties, the size distribution at very small diameters, the orbital evolution of asteroids, or the discovery of possible space mission targets. 252.11 Comet Science with LSST Michael Solontoi1, Ž. Ivezi?2, L. Jones2 1Adler Planetarium, 2University of Washington. Exhibit Hall The LSST will detect an unprecedented number (~10,000) of comets to r=24.5 over a ten year time frame. We simulate characteristic comet orbits through the LSST observational cadence and demonstrate that the LSST will observe individual Jupiter Family Comets (JFC) hundreds of times over their entire orbit, tracing each comet's evolution from presumed dormancy at large heliocentric distances, through the onset of out-gassing, and then back to inactivity. Simulations of Long Period Comets predict that LSST will make dozens of observations of each such comet, either on their way into and out of the Solar System, allowing in many cases early detection of these objects, or a number of observations while passing through perihelion, where the comets are the most active and variable. 252.12 Exploring the Transient and Variable Universe with LSST Andrew C. Becker1, J. S. Bloom2, L. M. Walkowicz2, LSST Collaboration 1Univ. of Washington, 2University of California, Berkeley. Exhibit Hall LSST's real-time image processing pipeline is expected to release tens of thousands of variability alerts per night. Many of these alerts will be associated with previously known classes of Galactic and cosmological variability. However, with LSST's novel combination of areal coverage, photometric depth, and rapid time sampling, new classes of phenomena will be uncovered. To recognize them, we must first characterize the menagerie of known transient and variable phenomena as they will be seen by LSST. We report here on efforts to model the signatures of astrophysical variability using the operational and image simulation tools being developed by LSST. This includes the injection of variable flux, at the pixel level, into simulated LSST images, and the measurement of this signal using the LSST Data Management stack. We also address LSST's potential capability to serve as a localization resource for alerts issued by gravity wave experiments, whose effective beam size is well-matched to LSST's field of view. This opportunity for trans-spectral astrophysics requires interrupt and follow-up capabilities in the LSST scheduler, as well as well-defined conditions to trigger them. 252.13 Measuring RR Lyrae Stars Throughout the Local Group with LSST Hakeem Oluseyi1, A. Becker2, C. C. Culliton3, M. Furqan1, K. L. Hoadley1, P. Regencia1, A. J. Wells1, I. J. Allison4, S. Jacoby5, Z. Ivezic2, L. Jones2, S. Krughoff2, B. Sesar6 1Florida Institute of Technology, 2University of Washington, 3Pennsylvania State University, 4Alabama A&M University, 5LSST Corporation, 6California Institute of Technology. Exhibit Hall We report on a study to determine the efficiency of the Large Synoptic Survey Telescope to recover the periods and shapes of RR Lyrae light curves, and their brightnesses. We select the smoothed light curves of 40 such stars observed by the Sloan Digital Sky Survey in the "Stripe 82" region, 30 of type RRab and 10 of type RRc, that evenly sample the known period-shape relationship for these stars. We place each of these in 1007 fields across the sky, each of which represents a different realization of the LSST sampling cadence, and that sample 5 particular observing modes. A light curve simulation tool was used to sample the RR Lyrae light curves, returning each as it would have been observed by LSST, including realistic limiting magnitudes and photometric scatter. We report here the brightness, period, Fourier-shape, and template-shape recovery as a function of distance from ~ 75 kpc to ~ 2 Mpc, with survey lengths varying from one to ten years. We find that ten years of LSST data are sufficient to recover the pulsation periods with a precision exceeding 0.001% for ~ 90% of stars within ~ 380 kpc of the Sun for Universal Cadence (UC) fields, and out to ~ 760 kpc for Deep Drilling (DD) fields, with the limit for successful period recoveries extending out to ~ 1.5 Mpc. For virtually all stars that had their periods recovered, their Fourier-based light curve shape parameter phi-31 was recovered with sufficient precision to recover photometric metallicities to within 0.14 dex out to ~ 1 Mpc in both the UC and DD fields. We outline an observing strategy that will increase the efficiency of period recovery for the majority of variable phenomena likely to be observed by LSST. 252.14 Mapping Milky Way And Local Volume Structure With LSST Marla C. Geha1, B. Willman2, J. Bochanski3, J. Bullock4, M. Catelan5, V. Debattista6, C. Grillmair7, A. Jordan5, M. Juric8, J. Kalirai9, N. Kallivayalil1, P. McGehee7, D. Minniti5, R. Munoz1, R. Roskar10, A. Sarajedini11, J. Simon12, J. Strader8, LSST MWLV Collaboration 1Yale University, 2Haverford, 3Penn State, 4UC Irvine, 5PUC, Chile, Chile, 6UCLan, United Kingdom, 7IPAC/Caltech, 8CfA, 9STScI, 10University of Washington, 11UFlorida, 12Carnegie Observatories. Exhibit Hall The LSST will yield revolutionary, multi-dimensional maps of the Milky Way (MW) galaxy and its neighbors. With its planned 1000 epochs over 6 bands and a final limiting magnitude of r=27.5 (AB mag; 5-sigma), it will provide an excellent resource for mapping the structure and accretion history of the MW and beyond in a way that the present generation of surveys can only hint at. LSST is expected to catalog 10 billion stars, including photometric metallicities for the 200 million F/G stars within 100 kpc and map the tangential velocity field of stars bright than r=24 mag to at least 10 kpc (at 10 km/s precision) and as far as 25 kpc (at 60 km/s precision). Specific related science to be enabled by LSST includes: mapping the 3D distribution of dust in the MW's disk, including variations in RV; understanding the smooth distribution of stars in the MW and other nearby galaxies; understanding large-scale chemical gradients in the MW; discovering lumps and streams in metallicity and phase-space; inferring the mass distribution in the MW; discovering ultra-faint galaxies throughout the Local Volume. 252.15 The Stellar Populations of the Milky Way and Nearby Galaxies with LSST Knut A. Olsen1, K. Covey2, A. Saha1, T. C. Beers3, J. Bochanski4, P. Boeshaar5, P. Cargile6, M. Catelan7, A. Burgasser8, K. Cook9, S. Dhital6, D. Figer10, Z. Ivezic11, J. Kalirai12, P. McGehee13, D. Minniti7, J. Pepper6, A. Prsa14, A. Sarajedini15, D. Silva1, J. A. Smith16, K. Stassun6, P. Thorman5, B. Williams11, LSST Stellar Populations Collaboration 1NOAO, 2Cornell University, 3Michigan State University/JINA, 4Penn State University, 5U.C. Davis, 6Vanderbilt University, 7Pontificia Universidad Católica, Chile, 8U.C. San Diego, 9LLNL, 10RIT, 11University of Washington, 12STScI, 13IPAC/Caltech, 14Villanova University, 15University of Florida, 16Austin Peay State University. Exhibit Hall The LSST will produce a multi-color map and photometric object catalog of half the sky to r=27.6 (AB mag; 5-sigma) when observations at the individual epochs of the standard cadence are stacked. Analyzing the ten years of independent measurements in each field will allow variability, proper motion and parallax measurements to be derived for objects brighter than r=24.5. These photometric, astrometric, and variability data will enable the construction of a detailed and robust map of the stellar populations of the Milky Way, its satellites and its nearest extra-galactic neighbors--allowing exploration of their star formation, chemical enrichment, and accretion histories on a grand scale. For example, with geometric parallax accuracy of 1 milli-arc-sec, comparable to HIPPARCOS but reaching more than 10 magnitudes fainter, LSST will allow a complete census of all stars above the hydrogen-burning limit that are closer than 500 pc, including thousands of predicted L and T dwarfs. The LSST time sampling will identify and characterize variable stars of all types, from time scales of ~ 1 hr to several years, a feast for variable star astrophysics; LSST's projected impact on the study of several variable star classes, including eclipsing binaries, are discussed here. We also describe the ongoing efforts of the collaboration to optimize the LSST system for stellar populations science. We are currently investigating the trade-offs associated with the exact wavelength boundaries of the LSST filters, identifying the most scientifically valuable locations for fields that will receive enhanced temporal coverage compared to the standard cadence, and analyzing synthetic LSST outputs to verify that the system's performance will be sufficient to achieve our highest priority science goals. 252.16 Galaxy Evolution with LSST Andrew Ptak1, LSST Galaxies Collaboration 1NASA/GSFC. Exhibit Hall LSST will be a unique tool to study the universe of galaxies. The database will provide photometry for 1010 galaxies, from the Local Group to thousands of z>6 galaxies. It will provide structural measurements and 6-band photometry for about 109 galaxies, largely at z<1.5. The key goal of the LSST Galaxies Collaboration is to measure the multivariate properties of the galaxy population including trends with redshift and environment. This includes observed galaxy properties (luminosities, colors, sizes, and morphologies) as well as derived galaxy properties (stellar masses, ages, and star formation rates) and how the joint distribution of these galaxy properties depends on redshift and environment as measured on a wide range of scales. Galaxy formation is inherently stochastic, but is fundamentally governed by the statistical properties of the underlying dark-matter density field. Determining how the evolving multivariate galaxy properties and scaling relations depend on this density field, and on the distribution and evolution of dark matter halos, will connect the results of large surveys to theoretical models of structure formation and galaxy formation. 252.17 AGN Science with LSST Robert Gibson1, S. F. Anderson1, D. R. Ballantyne2, A. J. Barth3, W. N. Brandt4, R. J. Brunner5, G. Chartas6, P. Coppi7, W. de Vries8, M. Eracleous4, X. Fan9, A. G. Gray2, R. F. Green10, Z. Ivezic11, M. Lacy12, P. Lira13, G. M. Madejski14, J. A. Newman15, G. T. Richards16, D. P. Schneider4, A. Seth17, O. Shemmer18, H. A. Smith17, M. A. Strauss19, E. Treister20, D. E. Vanden Berk21 1University of Washington, 2Georgia Tech, 3UC Irvine, 4Penn State, 5University of Illinois, 6College of Charleston, 7Yale, 8LLNL, 9Arizona, 10LBTO, 11University of Washington, University of Zagreb, 12NRAO, 13Universidad de Chile, Chile, 14SLAC, 15University of Pittsburgh, 16Drexel University, 17CfA, 18University of North Texas, 19Princeton, 20IfA, Hawaii, 21St. Vincent College. Exhibit Hall The LSST survey will dramatically increase the number of known active galactic nuclei (AGN), cataloging over 10 million AGN across more than 20,000 square degrees of sky. Time-domain coverage, a hallmark of the LSST survey, will enable powerful new AGN selection criteria, including the lack of proper motion and especially variability, in addition to color-based selection in deep, coadded ugrizy (320--1090 nm) images. Most of the LSST sky will be observed about 1000 times over ten years, while AGN in "deep drilling" fields will receive intense monitoring on time scales of minutes to days. Distinguishing traits of the LSST AGN survey include its coverage of the luminosity-redshift plane, its reach to high redshifts (with over 1000 AGN at z > 6.5), and the use of difference imaging to detect faint AGN surrounded by host galaxy emission or in crowded environments that challenge traditional photometry. LSST AGN will be used to determine the accretion history of supermassive black holes over cosmic time, the interaction of AGN with their evolving host galaxies and environments, the physics of AGN emission revealed by variability, and the relationship between AGN and dark matter through measurements of clustering at high redshifts. Multiwavelength analyses will benefit from matching LSST source identifications, redshifts, and light curves to archives and contemporaneous missions, and real-time LSST alerts will trigger follow-up observations. Simulated LSST images and archived SDSS Stripe 82 data are now being used to demonstrate the capabilities of the LSST AGN survey, with a current emphasis on evaluating metrics that select AGN based on their variability. 252.18 Simulating Galaxies and Active Galactic Nuclei in the LSST Image Simulation Effort James Pizagno1, Z. Ahmad2, J. Bankert2, D. Bard3, A. Connolly1, C. Chang4, R. R. Gibson1, K. Gilmore5, E. Grace2, M. Hannel2, J. G. Jernigan6, L. Jones1, S. M. Kahn4, S. K. Krughoff1, S. Lorenz2, S. Marshall4, S. M. Shmakova3, N. Sylvestri1, N. Todd2, M. Young2 1University of Washington, 2Purdue University, 3Kavli Institute for Particle Astrophysics & Cosmology, 4Stanford University, 5University of Stanford, 6Space Science Laboratory. Exhibit Hall We present an extragalactic source catalog, which includes galaxies and Active Galactic Nuclei, that is used for the Large Survey Synoptic Telescope Imaging Simulation effort. The galaxies are taken from the De Lucia et. al. (2006) semi-analytic modeling (SAM) of the Millennium Simulation. The LSST Image Simulation effort requires full SED information and galaxy morphological information, which is added to the catalog by fitting Bruzual & Charlot (2003) stellar population models, with Cardelli, Clayton, Mathis (1989) dust models, to the BVRIK colors provided by the De Lucia et. al. (2006) SAM. Galaxy morphology is modeled as a double Sersic profile for the disk and bulge. Galaxy morphological information and number counts are matched to existing observations. The catalog contains galaxies with a limiting r-band magnitude of mr=28, which results in roughly 1E6 galaxies per square degree. An existing AGN catalog (MacLeod et. al. 2010) is matched to galaxy hosts in the galaxy catalog using SDSS observations. AGN are morphologically modeled as variable point sources located at the center of the host galaxy. We demonstrate how this extragalactic source catalog allows LSST to plan for extended object extraction, variable extragalactic source detection, sensitivity level determination after image stacking, and perform various other cosmological tests. 252.19 Baryon Acoustic Oscillations in the LSST Photometric Survey Alexandra Abate1, A. Gorecki2, R. Ansari1, A. Barrau2, S. Baumont2, L. Derome2, E. Gawiser3, C. Magneville4, M. Moniez1, J. A. Newman5, J. A. Tyson6, H. Zhan7, LSST LSS Science Collaboration 1Laboratoire De L'Accelerateur Lineaire, IN2P3-CNRS, Universite de Paris-Sud, France, 2Laboratoire de Physique Subatomique et de Cosmologie, CNRS/UJF/INPG, France, 3Rutgers, the State University of NJ, 4CEA, DSM/IRFU, Centre d'Etudes de Saclay, France, 5University of Pittsburgh, 6University of California, Davis, 7National Astronomical Observatories, Chinese Academy of Sciences, China. Exhibit Hall Baryon acoustic oscillation (BAO) studies provide an important probe of dark energy, yielding constraints that are highly complementary to other methods such as weak gravitational lensing and very competitive to other proposed large surveys. By measuring the BAO scale in ugrizy-band photometric redshift-selected samples, LSST will determine the angular diameter distance to each of a dozen redshifts with percent-level errors. However, photometric redshift (a.k.a. photo-z) errors can dilute the observed strength of the BAO signal. We therefore investigate the impact of simulated photo-z errors on the reconstruction of the BAO scale using Monte Carlo simulations of mock galaxy samples with luminosity-color-redshift distributions designed to agree with those from the GOODS survey. In this poster, we demonstrate the effects that (i) the level of statistical uncertainty in photo-z's, (ii) the fraction of catastrophic photometric redshift outliers, or (iii) the choice of galaxy sample population has on the significance with which the BAO signal is detected. 252.20 Tracing the Supernovae of LSST W. Michael Wood-Vasey1, R. Kessler2, R. Biswas3, D. Cinabro4, B. Dilday5, S. Kuhlmann3, LSST Supernova Collaboration 1University of Pittsburgh, 2University of Chicago, 3Argonne National Lab, 4Wayne State, 5Las Cumbres Observatory Global Telescope. Exhibit Hall The LSST will discover over one million supernovae during its 10-year survey. This overwhelming compendium of stellar death throes will allow for novel techniques and insights in our study of the evolution of the Universe, large-scale structure, supernova explosion physics, and star formation and evolution. We here present our most detailed simulations to date of the lightcurves and properties of the supernovae that will be found by LSST using the LSST operations and cadence simulation and the SNANA supernova survey modeling code. The largest uncertainty in our results is due to the lack of large samples of non-Type Ia supernovae and the uncertainty in the type-dependent supernovae rate as a function of redshift. We argue for increased observations of all types of supernovae in the nearby Universe and programs to investigate what spectroscopic subsamples will be necessary to enable photometric classification of the supernovae to be found by LSST. 252.21 Strong Lenses with LSST: Simulated 10-year Movies of Multiply-Imaged Quasars Jesse Garrett Jernigan1, P. J. Marshall2, M. Oguri3, R. Gibson4, J. Pizagno4, A. Connolly4, J. R. Peterson5, Z. Ahmad5, J. Bankert5, D. Bard6, C. Chang7, E. Grace5, K. Gilmore8, M. Hannel5, L. Jones4, S. M. Kahn8, S. Krughoff4, S. Lorentz5, S. Marshall8, S. Nagarajan5, A. P. Rasmussen8, M. Shmakova6, N. Sylvestre4, N. Todd5, M. Young5, LSST Strong Lensing Science Collaboration 1Space Sciences Laboratory, UC Berkeley, 2Oxford/KIPAC, United Kingdom, 3NAOJ, Japan, 4U. Washington, 5Purdue, 6KIPAC/SLAC, 7Stanford, 8Stanford/SLAC. Exhibit Hall We use the LSST image simulator to generate realistic 10-year datasets for 100 of the strong galaxy-scale gravitational lenses expected to be measurable with the universal survey data. The 200 mock i-band images have sky brightness and atmospheric seeing drawn from plausible distributions for the Cerro Pachon site, and we use plausibly varying telescope optics and detector response to fully represent the expected image quality. Passing the simulated images through a standard astronomical object detection pipeline gives us our first view of what these rare and valuable objects will look like in the LSST database. We also investigate the recovery of the input lightcurves. 252.22 Accurate Cosmography with LSST Time Delay Lenses Philip J. Marshall1, C. P. Sandford2, C. D. Fassnacht3, D. R. Meldgin3, M. Oguri4, S. H. Suyu3, M. W. Auger3, LSST Strong Lensing Science Collaboration 1Stanford University, 2Imperial College, United Kingdom, 3University of California, 4NAOJ, Japan. Exhibit Hall LSST will discover several thousand lensed quasars and supernovae, and provide high signal-to-noise ratio, well-sampled lightcurves for each. We explore the potential of the expected sample of 400 well-measured 4-image (quad) lens systems for constraining cosmological parameters, via measurements of the "time delay distance" to each one. Based on recent experience with individual lenses studied in great detail with the VLA, Keck and HST, we make plausible assumptions about our likely knowledge of the lens model and lens environment to quantify the largest sources of systematic error, and use simulations of LSST lightcurves to estimate the expected time delay precision. We find that the resulting constraints on the parameters of the Dark Energy equation of state are competitive with and complementary to those from other LSST cosmological probes. 252.23 Probing Dark Energy with Weak Lensing with LSST Ian P. Dell'Antonio1, D. Wittman2, B. Jain3, J. Bosch2, D. Clowe4, M. Jarvis3, M. Jee2, J. Tyson2, H. Zhan5, LSST Weak Lensing Science Collaboration 1Brown University, 2UC Davis, 3Univ. of Pennsylvania, 4Ohio University, 5NAOC, China. Exhibit Hall LSST will measure the shape, magnitude, and colors of more than 3x109 galaxies over 20,000 square degrees. These data will be used in several complementary ways to measure the properties of dark energy. Reconstruction of the shear power spectrum on linear and non-linear scales l~/< 2000, and of the cross-correlation of shear measured in different photometric redshift bins, provides a constraint on the evolution of dark energy that is complementary to the purely geometric measures provided by Supernovae and BAO. Combining weak lensing and BAO measurements breaks degeneracies and results in tighter constraints on dark energy than each method can provide individually. Cross-correlation of the shear and galaxy number density signal within redshift shells minimizes the sensitivity to photo-z errors. Measurements of the shear bispectrum constrain dark energy and allow an independent test of theories of gravity. In addition to the galaxy shape correlations, LSST will detect ~ 50,000 shear peaks with significance greater than 4?, and ~ 10,000 securely detected clusters of galaxies with line-of-sight velocity dispersions greater than 700 km/s. These allow independent constraints on the dark energy signature in the growth of structure. Tomographic study of the shear of background galaxies as a function of redshift allows the a geometric test of dark energy to be extracted from the weak lensing data. Finally, lensing signatures beyond the shear (magnification and flexion) will be accessible with LSST with unprecedented statistical power. The ability of LSST to extract the dark energy signal will depend on the accuracy with which the stellar PSF can be determined, and on the unbiased reconstruction of object shapes from long sequences of exposures in which the objects are detected at low significance. We discuss the prospects for cosmological constraints from weak lensing studies with LSST. 252.24 Weak Lensing Galaxy Shear Extraction Testing for LSST Myungkook J. Jee1, J. A. Tyson1, D. Wittman1, A. J. Connolly2, G. Jernigan3, J. R. Peterson4, Z. Ivezic2 1UC Davis, 2U. Washington, 3UC Berkeley, 4Purdue U.. Exhibit Hall The accuracy and reliability of weak-lensing measurement for LSST depend on the level of the atmospheric turbulence of the site, the integrity of the design and fabrication of the optical system, the ability to describe and model both the atmospheric and instrumental characteristics, and the accuracy of the algorithm to remove these systematics and extract gravitational shears of galaxies. Of course, at the core of this removal of the systematics is the high-fidelity modeling and correction of the point spread function (PSF) on the delivered images. In this poster, we present the results of our on-going end-to-end shear extraction simulation efforts to investigate the impacts of the above factors on lensing signal measurement. First, we review our past accomplishments on the issue of accurate description and removal of the PSF effects using a principal component analysis method. Then, we present the results of our current shear extraction simulation using artificially sheared galaxy images. Finally, we discuss some key issues that need to be addressed in order to meet the requirement of the LSST weak-lensing science. 252.25 Shear Systematics in LSST Simulated Images Chihway Chang1, S. M. Kahn1, G. Jernigan2, J. R. Peterson3, A. P. Rasmussen1, Z. Ahmad3, J. Bankert3, D. Bard1, A. Connolly4, R. R. Gibson4, K. Gilmore1, E. Grace3, M. Hannel3, L. Jones4, S. Krughoff4, S. Lorenz3, S. Marshall1, S. Nagarajan3, J. Pizagno4, M. Shmakova1, N. Sylvestre4, N. Todd3, M. Young3 1SLAC/Stanford, 2SSL/UC Berkeley, 3Purdue University, 4U. Washington. Exhibit Hall The Large Synoptic Survey Telescope (LSST) is a large-aperture, wide-field, ground-based telescope designed to provide a complete survey of 20,000 square degrees of sky in six optical bands every few nights. Over ten years of operation, it will measure the magnitudes, colors, and shapes of several billion galaxies. As such, LSST will probe cosmic shear down to levels far beyond those accessible with current surveys. The unprecedented statistical power of LSST will impose new requirements on the control of weak lensing systematics. Various noise sources become important in this context, associated with counting statistics, atmospheric effects, and wavefront errors introduced by the telescope and camera systems. We are studying these various noise components and their impact on shear measurements using simulated LSST images produced by a prototype high fidelity photon-by-photon Monte Carlo code. The code includes the most significant physical effects associated with photon propagation through the atmosphere, reflection off of the three mirror surfaces of the telescope, and propagation through the elements of the camera and on into the detector. We report on preliminary results from this program, including plots of residual shear error correlation functions due to errors in the object shape estimation for realistic LSST operating conditions. 253 Exoplanet Detection: Techniques & Observations Poster Session Exhibit Hall 253.01 HATSouth Operations and Data Processing Kaloyan Penev1, Z. Csubry2, G. Bakos2 1Harvard Univ., 2Harvard Smithsonian Center for Astrophysics. Exhibit Hall The HAT-South network consists of three pairs of identical, fully automated, wide-field telescopes, each equipped with 4 optics and CCDs forming a mosaic image. The instruments are located at Las Campanas in Chile, Siding Springs in Australia, and the HESS site in Namibia, and are jointly operated by the CfA, MPIA and ANU. Its primary purpose is to search for and characterize extra-solar planets around nearby bright stars. In this presentation I will discuss two aspects of the HAT-South system. First, in order to achieve the high photometric precision necessary for detecting transiting planets, the observing systems needs to be as stable as possible to minimize systematic noise. Here I will detail the methods u