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Aas 221 abstracts

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Aas 221 abstracts

  1. 1. stAAS Winter Meeting Abstracts 90 – HAD I Special: Making Astronomy Public, Los Astrophysics with CCAT in the Next Decade 243 – Galaxy Clusters Angeles Style 151 – HAD IV History of Astronomy 244 – HEAD III: First Results from the NuSTAR 91 – HAD II Special: Preservation of Astronomical 152 – Large Scale Structure, Cosmic Distance Scale Mission Heritage and Archival Data and GRBs 245 – Intergalactic Medium, QSO Absorption Line 100 – Welcoming Address 153 – NASAs Physics of the Cosmos (PCOS) Systems 101 – Kavli Lecture: The Spitzer Space Telescope: Studies on Gravitational Wave and X-ray Mission 246 – K-12 Students Learning and Doing Astronomy Science Return and Impact Concepts 247 – Large Synoptic Survey Telescope 103 – AGN: Jets and Feedback 154 – Pulsars, Neutron Stars 248 – New Results from Astronomy Education 104 – Circumstellar Disks I 155 – Relativistic Astrophysics, Gravitational Lenses Research 105 – Cosmic Microwave Background I & Waves 249 – Planetary Nebulae, Supernova Remnants 106 – Cosmology I 156 – Specialized Observatories and Light Pollution 250 – Star Associations, Star Clusters - Galactic and 107 – Dwarf and Irregular Galaxies I: Origins and 157 – Starburst Galaxies Extra-galactic Dynamics 158 – Stars, Cool Dwarfs, Brown Dwarfs 251 – Star Formation 108 – Early Science Results from the Hydrogen 159 – The Sun 252 – Stellar Evolution, Stellar Populations Epoch of Reionization Arrays (HERA) 160 – A Moderated Discussion about Interesting 253 – Supernovae 109 – Extrasolar Planet Detection from Spectroscopy Careers in Aerospace and Mission Operations 254 – The Milky Way, The Galactic Center and Microlensing 200 – Finding the Next Earth 255 – Undergraduate and Graduate Teaching, 110 – From Star Formation to Cosmology: 201 – Astronomy Outreach for Non-traditional Learning and Research Astrophysics with CCAT in the Next Decade Audiences 256 – Young Stellar Objects, Very Young Stars, 111 – Galaxy Clusters I 202 – Binary Star Systems: Observations, Models, T-Tauri Stars, H-H Objects 112 – Galaxy Evolution at z~2 Origins 300 – Heineman Prize: Extreme Transients in the High 113 – HAD III/HEAD I Special: Fifty Years 203 – Black Holes II Energy Universe of Celestial X-ray Astronomy 204 – Circumnuclear Environments of AGN 301 – Astrophysics with Keplers High Precision 114 – Relativistic Astrophysics, Gravitational Lenses 205 – Circumstellar Disks II Photometry I & Waves 206 – Galaxies I 302 – Effective Education and Public Outreach 115 – Research Based Initiatives for Broadening the 207 – Galaxy Evolution at z = 4-12 303 – Galaxies III Participation of Women and Minorities in Astronomy 208 – HAD VI History of Astronomy 304 – Galaxy Evolution in Protogalaxy Clusters 116 – Science Highlights from NASAs Astrophysics 209 – HEAD III: First Results from the NuSTAR 305 – Instrumentation: Ground, Airborne and Space I Data Analysis Program I: Galactic Astrophysics Mission 306 – Molecular Clouds, HII Regions, Interstellar 117 – Young Stellar Objects, Very Young Stars, 210 – High Resolution Ultraviolet Imaging with the Medium T-Tauri Stars, H-H Objects Hubble Space Telescope I [low redshift] 307 – Multi-wavelength Observations of Quasars 118 – Galaxy Clusters in the Golden Age of 211 – Innovations in Teaching, Learning, and 308 – Planetary Systems Orbiting White Dwarfs High-Energy Astrophysics Mentoring 309 – QSO/AGN Engines and the Circumnuclear 122 – Andromeda and Local Group Dwarf Galaxies 212 – Intergalactic Medium, QSO Absorption Line Region 123 – Black Holes I Systems 310 – Reports from NASAs Program Analysis 124 – Cosmic Microwave Background II 213 – Stellar Evolution and Ages Groups 125 – Dark Matter Properties, Observations and 214 – Supernovae II 311 – Results from The Panchromatic Hubble Constraints 215 – Surveys and Large Programs Andromeda Treasury 126 – Exoplanet Interiors and Atmospheres 216 – Zeroing in on eta-Earth with NASAs Kepler 312 – Star Formation - Dark Clouds and Clumps 127 – Family Leave Policies and Childcare for Mission 313 – Structure and Evolution of Local Galaxies Graduate Students and Postdocs 217 – Cannon Award: Exploring the Diversity of 314 – The Solar System 128 – Galaxy Clusters II Exoplanetary Atmospheres 315 – Transit Detection of Extrasolar Planets 129 – Galaxy Evolution at z > 2 220 – Circumstellar Disks III 316 – Variable Stars 130 – HAD V History of Astronomy, with Osterbrock 221 – Cosmic Dawns: ALMA Early Science 317 – Warner Prize: A New View on Planetary Book Prize Commences Orbital Dynamics 131 – HEAD II: New Revelations from the Transient 222 – Dark Energy, Tests of Gravity and Fundamental 321 – Astrophysics with Keplers High Precision Sky Constants Photometry II 132 – Large Scale Structure, Cosmic Distance Scale 223 – Dust 322 – Circumgalactic Matter of Galaxies at z=2-3 and GRBs I 224 – Exoplanet Atmospheres 323 – Cosmology II 133 – Quasars and Their Hosts, Near and Far 225 – Galaxies II 324 – Direct Detection of Exoplanets, Faint 134 – Science Highlights from NASAs Astrophysics 226 – Galaxy Clusters III Companions, and Protoplanetary Disks Data Analysis Program II: Extragalactic Astrophysics 227 – Galaxy Evolution at z ~ 1 325 – Dusty Debris in the Terrestrial Planet Zone I 135 – Scientific Opportunities with the James Webb 228 – High Resolution Ultraviolet Imaging with the 326 – Evolution of Structure in Local Galaxies (z~0) Space Telescope Hubble Space Telescope II [high redshift] 327 – Galaxies IV 136 – Supernovae I 229 – Instrumentation, Data Handling, and Image 328 – Instrumentation: Ground, Airborne and Space II 137 – Young Stellar Objects, Very Young Stars, Analysis 329 – Joining the Electromagnetic and Gravitational T-Tauri Stars, H-H Objects - Disks 230 – New Insights into the Distribution of Stellar Wave Skies 138 – Henry Norris Russell Lecture: Thinking and Structure and Mass in Galaxies: Results from S^4G 330 – SNRs and PNe: Theory and Observation Computing 231 – Planets and Planetary Systems Identified by 331 – Star Associations, Star Clusters - Galactic and 139 – From Gas to Stars Over Cosmic Time Kepler Theory 141 – Astronomy Outreach to the Public 232 – Stars and the Galactic Halo 332 – Star Formation - Cores, Clouds and the IMF 142 – Binary Stellar Systems, X-ray Binaries 233 – Supernovae III 333 – Super-Earths, M Dwarfs, and Habitability 143 – Black Holes 234 – The Galaxy: Age, Structure and Evolution 334 – Surveys and Catalogs of Extrasolar Planet 144 – Circumstellar Disks 235 – Turbulence: Theory and Observation Hosts 145 – Dust 236 – Newton Lacy Pierce Prize: Hot on the Trail of 335 – The Dark Energy Survey 146 – Elliptical and Spiral Galaxies Warm Planets Orbiting Cool M Dwarfs 336 – The Elemental Compositions of Extrasolar 147 – Evolution of Galaxies 237 – HEAD Rossi Prize: The Flaring Crab Nebula: Planetesimals from Spectroscopy of Polluted White 148 – Evolved Stars, Cataclysmic Variables, Novae, Surprises and Challenges Dwarfs Wolf-Rayet Phenomena 240 – Computation, Data Handling, Image Analysis 337 – Computational Cosmology 149 – Extrasolar Planets: Detection 241 – Dark Matter and Dark Energy 339 – AGN, QSO, Blazars 150 – From Star Formation to Cosmology: 242 – Dwarf and Irregular Galaxies 340 – Catalogs
  2. 2. 341 – Cosmology 404 – Dwarf and Irregular Galaxies II: ISM/IGM and 425 – Star Associations, Star Clusters - Extra-galactic342 – Education and Professional Development the Magellanic Clouds 426 – Star Formation - Clusters and Cores343 – Extrasolar Planets: Characterization, Theory and 405 – Evolution of Galaxy Mergers, Black Hole 427 – The Role of Calibration in Modern Optical andDetection Formation, and Satellite Galaxies Infrared Astronomy344 – Hubble Space Telescope Instruments and 407 – Kepler Exoplanets 428 – Gas Flows and Galaxy EvolutionCalibration 408 – Laboratory Astrophysics and Pulsar Potpourri 429 – Lancelot M. Berkeley Prize: Results from the345 – Instrumentation: Ground and Airborne 409 – Large Scale Structure, Cosmic Distance Scale Wilkinson Microwave Anisotropy Probe (WMAP)346 – Joining the Electromagnetic and Gravitational and GRBs II 430 – AGN and FriendsWave Skies 410 – Massive Star Formation and Supernovae IV 431 – Computation and Other Topics347 – JWST Mission and Instrumentation 411 – Nearby Star Forming Galaxies 432 – Cosmology and Other Topics348 – Laboratory Astrophysics 412 – Pulsars, Neutron Stars 433 – Education and Public Outreach349 – Molecular Clouds, HII Regions, Interstellar 413 – Radio Surveys of Galactic Clouds 434 – Evolution of GalaxiesMedium 414 – Starburst Galaxies 435 – Extrasolar Planets350 – Space-Based Missions, Instruments and 415 – The Sun 436 – GalaxiesTechnology 416 – The Hubble Constant in the Era of Precision 437 – Galaxy Clusters351 – Stellar Atmospheres, Winds Cosmology 438 – GRBs352 – Surveys and Large Programs 418 – CO, Dust, Outflows, etc. in Galaxies 439 – Instrumentation, Missions and Surveys353 – The Solar System and Astrobiology 419 – Direct Imaging Methods for Extrasolar Planet 440 – Interstellar Medium354 – Variable Stars & White Dwarfs Detection 441 – Star Clusters400 – New Insights of Comets from the EPOXI 420 – Evolution in Compact Galaxy Clusters 442 – Star FormationMission 421 – High Energy Binaries 443 – Stellar Topics401 – Cataclysmic Variables and Compact Binaries 422 – Multi-wavelength Spectroscopy of AGN 444 – Supernovae402 – Cosmology, the Lyman-alpha Forest, 423 – Nearby Stars and Wide Binaries 445 – The Sun and Solar Systemand Intergalactic Medium from BOSS 424 – Planetary Systems Orbiting White Dwarfs and403 – Dusty Debris in the Terrestrial Planet Zone II Neutron Stars
  3. 3. 90 – HAD I Special: Making Astronomy Public, Los Angeles StyleSpecial Session – Room 103B (Long Beach Convention Center) – 06 Jan 2013 01:30 PM to 03:30 PM This 120 minute special session will explore aspects of popular astronomy in the Los Angeles area over the past 150 years that stimulated public awareness and interest in astronomy. Topics include: (1) organized amateur astronomy in Los Angeles, (2) the growth of the amateur telescope industry in Los Angeles, (3) L.A. style astronomical evangelists, (4) the forces that created and shaped the Griffith Observatory and the Mt. Lowe Observatory, (5) the influence of astronomers ranging from George Ellery Hale to Frederick C. Leonard to Tommy Cragg in all these aspects of public astronomy in the Los Angeles area, (6) if there is a distinguishable L.A. style to public astronomy in Los Angeles. domestic and international research institutions. Among the most remarkable were large90.01 – Creating Griffith Observatory solar spars for Lockheed Solar Observatory in California and Ottawa River SolarA. Cook, Griffith Observatory, Pasadena, CA Observatory in Canada. His instrumentation also equipped educational facilities including01:30 PM-03:30 PM observatories at UCLA, Westmont College, Pasadena City College, Bevard Community College, and many others. A Carroll telescope boasting a particularly distinguishedGriffith Observatory has been the iconic symbol of the sky for southern California since educational history was a small astrograph built in 1953 for Professor George Moyen ofit began its public mission on May 15, 1935. While the Observatory is widely known as Hollywood and subsequently used for the long-running Summer Science Program inbeing the gift of Col. Griffith J. Griffith (1850-1919), the story of how Griffith’s gift Ojai, California. Later solar instruments built by Carson Instruments were closelybecame reality involves many of the people better known for other contributions that derivative of Carroll designs.made Los Angeles area an important center of astrophysics in the 20th century. Griffithbegan drawing up his plans for an observatory and science museum for the people of 90.04 – Los Angeles and Its Influence on Professional and Popular Astronomy - ALos Angeles after looking at Saturn through the newly completed 60-inch reflector on Hollywood Love Story, by Lewis Chilton, Past President, Optical Shop Director andMt. Wilson. He realized the social impact that viewing the heavens could have if made Historian, Los Angeles Astronomical Societyfreely available, and discussing the idea of a public observatory with Mt. WilsonObservatory’s founder, George Ellery Hale, and Director, Walter Adams. This resulted, L. Chilton, Los Angeles Astronomical Society, Los Angeles, CAin 1916, in a will specifying many of the features of Griffith Observatory, and 01:30 PM-03:30 PMestablishing a committee managed trust fund to build it. Astronomy popularizer Mars The purpose of this presentation is to show through visualizations how the Los Angeles,Baumgardt convinced the committee at the Zeiss Planetarium projector would be California milieu of the early 20th century benefited the advancement of astronomy andappropriate for Griffith’s project after the planetarium was introduced in Germany in captured the public consciousness through popular press accounts of these1923. In 1930, the trust committee judged funds to be sufficient to start work on creating advancements and of the scientists who made them. The thesis of this presentationGriffith Observatory, and letters from the Committee requesting help in realizing the purports that a symbiosis developed between astronomers of Los Angeles-areaproject were sent to Hale, Adams, Robert Millikan, and other area experts then engaged scientific and educational institutions and a local community of interested laypersons, andin creating the 200-inch telescope eventually destined for Palomar Mountain. A was the catalyst that sparked future generations to enter the fields of astronomy, theScientific Advisory Committee, headed by Millikan, recommended that Caltech Physicist allied sciences, education and technology. This presentation attempts to highlight theEdward Kurth be put in charge of building and exhibit design. Kurth, in turn, sought help importance of continued public outreach by the professional astronomical community, forfrom artist Russell Porter. The architecture firm of John C. Austin and Fredrick Ashley the ultimate benefit to itself, in Los Angeles and beyond.was selected to design the project, and they adopted the designs of Porter and Kurth.Philip Fox of the Adler Planetarium was enlisted to manage the completion of the 90.05 – Public PerformanceObservatory and become its temporary Director. E.C. Krupp, Griffith Obs., Los Angeles, CA90.02 – The Early Years of Amateur Astronomy in Los Angeles—Conflicts and 01:30 PM-03:30 PMContradictions America’s first planetaria all opened in the 1930s, and each was the distinctive productT.R. Williams, AAVSO, Cambridge, MA of local circumstances. In Los Angeles, the populist sensibilities of Griffith J. Griffith01:30 PM-03:30 PM prompted him to value the transformative power of a personal encounter with a telescope, and he quickly embraced the idea of a public observatory with free access toAstronomy had an active audience in Los Angeles from the latter years of the all. Griffith Observatory and its planetarium emerged from that intent. Authenticity,nineteenth century on. However, it is surprising that organized avocational astronomy did intelligibility, and theatricality were fundamental principles in Griffith’s thinking, and theynot really flower until the promotion of amateur telescope making as a hobby beginning were transformed into solid and enduring scientific and astronomical values by thosein the mid-1920s. Even though astronomy burgeoned as a local industry with the Mount who actually guided the Observatory’s design, construction, and programming. That said,Wilson Astronomical Observatory visible from much of the LA Basin on most days, the public profile of Griffith Observatory was most defined by its inspired hilltop location,astronomers from the observatory providing informative talks to local groups, and the its distinctive, commanding architecture, and its felicitous proximity to Hollywood. TheGriffith Observatory actively promoting interest in astronomy as well as science more Observatory is theatric in placement and in appearance, and before the Observatorygenerally, interest in telescope making and recreational observing continued to dominate even opened, it was used as a motion picture set. That continuing vocation turnedthe activities of Los Angeles amateurs for the first twenty-five years of the local Griffith Observatory into a Hollywood star. Because entertainment industry objectivessociety’s existence. Even the later active membership of outstanding scientific and resources were part of the Los Angeles landscape, they influenced Observatorycontributors like Tom Cave and Tom Cragg, and the participation of astronomy students programming throughout the Observatory’s history. Public astronomy in Los Angelesfrom UCLA and Cal Tech like George Herbig, yielded little change in direction over this has largely been framed by the Observatory’s fundamental nature. It has exhibits, but itperiod. is not a museum. It has a planetarium, but it is essentially an observatory. As a public observatory, it is filled with instruments that transform visitors into observers. This role90.03 – The Space-Age Legacy of Telescope Designer George A. Carroll emphasized the importance of personal experience and established the perception ofJ.W. Briggs, HUT Observatory, Eagle, CO Griffith Observatory as a place for public gathering and shared contact with the cosmos.01:30 PM-03:30 PM The Observatory’s close and continuous link with amateur astronomers made amateurs influential partners in the public enterprise. In full accord with Griffith J. Griffith’sRemembered particularly as a founding member of Stony Ridge Observatory near original intent, Griffith Observatory has all been about putting people eyeball to theMount Wilson, George A. Carroll (1902-1987) was legendary in the Southern California universe with authenticity, showmanship, and style.telescope making community. In Texas at the age of sixteen, Carroll built and flew hisown aircraft, becoming one of the youngest aviators in the country. He eventually 90.06 – Commentary on Making Astronomy Public, LA Stylebecame an employee of Lockheeds Skunk Works in Burbank. His earliest knowncommercial telescopes were high-end amateur instruments built by R. R. Cook. As D.H. De Vorkin, Smithsonian Inst., Washington, DCdescribed in a brochure describing his later telescope work, he had experience in so 01:30 PM-03:30 PMmany branches of technology that it is unbelievable. By the time Carrolls designs were Commentary based upon the papers in this session will focus on historical issuesbuilt by Thomas Tool & Die in Sun Valley, his telescopes were well known in the solar relevant to promoting science and in use at National Solar Observatory, Caltech, and at many other91 – HAD II Special: Preservation of Astronomical Heritage and Archival DataSpecial Session – Room 103B (Long Beach Convention Center) – 06 Jan 2013 04:00 PM to 06:00 PM This session will deal with preserving astronomy’s rich cultural heritage, including its largely untapped archival collections of
  4. 4. scientific data, sites of historical importance and the many historical papers and instruments that have yet to be scholarly discussed. In January 2007, in response to concerns that parts of the heritage was in serious danger of being lost, the AAS created the Working Group on the Preservation of Astronomical Heritage (WGPAH) charged with “developing and disseminating procedures, criteria and priorities for identifying, designating, and preserving astronomical structures, instruments, and records so that they will continue to be available for astronomical and historical research, for the teaching of astronomy, and for outreach to the general public.” In 2008 the IAU and UNESCO’s World Heritage Committee approved the Astronomy and World Heritage Initiative (AWHI) which aims to “identify, safeguard and promote cultural properties connected with astronomy.” Now five years on with WGPAH and AWHI it is an appropriate time to see what has been accomplished.91.01 – UNESCOs Astronomy and World Heritage Initiative: Progress to Date and 91.03 – Issues and Challenges in the Protection of Different Categories of AstronomicalFuture Priorities Heritage: A Report from Beijing 2012C. Ruggles, University of Leicester, Leicester, Leics, UNITED S. Schechner, Harvard Univ., Cambridge, MAKINGDOM 04:00 PM-06:00 PM04:00 PM-06:00 PM On the occasion of the IAU’s General Assembly in Beijing in 2012, the Working Groups for Astronomy and World Heritage (WG-AWH) and Historical Instruments (WG-HI) ofUNESCO’s thematic initiative on Astronomy and World Heritage was created in 2005 Commission 41 (History of Astronomy)—led by Clive Ruggles and Sara“to establish a link between science and culture on the basis of research aimed at Schechner—held a joint science meeting concerning shared issues in the “Conservationacknowledging the cultural and scientific values of properties connected with and Protection of Different Categories of Astronomical Heritage.” Since 2008, theastronomy”. Since 2008, when a formal Memorandum of Understanding (MoU) was WG-AWH had been working with UNESCO and its advisory bodies to identify andsigned between the IAU and UNESCO to work together to advance the Initiative, the safeguard significant astronomical sites and assist in their eventual nomination forIAU, through its Working Group on Astronomy and World Heritage, has been working inclusion on the World Heritage List. That initiative was restricted to fixed sites andto help identify, safeguard and promote the world’s most valuable cultural properties monuments. Moveable, tangible objects, such as scientific instruments, could not beconnected with astronomy. The Working Group’s first major deliverable was the included even though their significance was often interconnected with that of immovableThematic Study on the Heritage Sites of Astronomy and Archaeoastronomy, which was sites. To address this concern, the 2012 joint science meeting convened internationalprepared in collaboration with ICOMOS, the Advisory Body to UNESCO that assesses experts in the history, scientific, and cultural value of astronomical buildings, instruments,World Heritage List applications relating to cultural heritage. Published in 2010, this has photographic plates, archives, and meteorites in order to discuss ways to develop andbeen endorsed by the World Heritage Centre as a basis for developing specific coordinate integrated approaches to the documentation and protection of these valuableguidelines for UNESCO member states on the inscription of astronomical properties. things. A wide range of materials was discussed. It was evident that the historical,The IAU’s General Assembly in Beijing saw the launch of perhaps the most significant scientific, and cultural value assigned to any particular item might differ from onedeliverable from the Initiative to date, the Portal to the Heritage of Astronomy community to the next, and that the question of whom or what ultimately will determine( which is a dynamic, publicly accessible database, how any heritage item is treated is complex, political, and negotiated. An important pointdiscussion forum, and document-repository on astronomical heritage sites throughout the of agreement was the idea of developing a “science heritage” (rather than “architecturalworld, whether or not they are on UNESCO’s World Heritage List. In recent months heritage”) approach in which the value is enhanced (rather than diminished) by changesthe Working Group has completed a set of nine “Extended Case Studies, which raise a to a facility that could lead to further scientific discoveries. It was hoped that such anwide range of general issues, varying from the integrity of astronomical sightlines at approach would make observatory directors and others more comfortable with outsideancient sites to the preservation of dark skies at modern observatories. Given the recognition of the heritage value of their working institutions.progress that has been made to date, how would we wish to see the Initiative develop inthe future and what should be the Working Group’s priorities in the coming months andyears? Among the suggestions I shall be discussing is that the WG should find ways to 91.04 – AAS Working Group on the Preservation of Astronomical Heritage: Thework more directly with national State Parties to encourage and help them prepare Preservation of Astronomical Plates and Other Effortsviable nominations for astronomical heritage sites on the World Heritage List. W. Osborn, AAS WGPAH, Washington, DC; W. Osborn, Yerkes Observatory, Willams Bay, WI91.02 – Preserving a Piece of the True Cross 04:00 PM-06:00 PMD.H. De Vorkin, Smithsonian Inst., Washington, DC The WGPAH was created in 2007 in response to concerns that parts of astronomy’s04:00 PM-06:00 PM rich heritage were in serious danger of being lost. Three classes of heritage were listedI will discuss shared concerns of Curators and Collections Management Specialists at as of concern: (1) historically significant astronomical sites, (2) historically significantthe National Air and Space Museum over the proper methods for identifying, instruments, and (3) archives of historical documents and observations. During its sixdocumenting and preserving astronomical instrumentation in the Museums purview as years the WG’s efforts have been directed mainly toward the third area, and inwell as in the realm of modern astronomical research. Questions of what and how will particular toward the preservation of astronomical plates. This talk first provides anbe raised and discussed, including the issue of preserving the historical character of overview of the WGPAH – charge, structure and membership. It then describes theinstrumentation deemed still useful to astronomy. As part of this discussion, we will also results from its two major initiatives – the census of North American astronomical platesconsider: why make the effort to preserve? What is the value of a personal physical carried out in 2008 and the Workshop on Developing a Plan for preserving Astronomy’sencounter with the real thing? Archival Records held in 2012. It concludes with the WG’s future challenges.100 – Welcoming AddressPlenary Session – Grand Ballroom (Long Beach Convention Center) – 07 Jan 2013 08:00 AM to 08:30 AM 08:00 AM-08:30 AM– Welcome Address by AAS President David Helfand101 – Kavli Lecture: The Spitzer Space Telescope: Science Return and ImpactPlenary Session – Grand Ballroom (Long Beach Convention Center) – 07 Jan 2013 08:30 AM to 09:20 AM
  5. 5. the first direct detection of light from a planet orbiting another star and obtaining the first101.01 – The Spitzer Space Telescope: Science Return and Impact thermal infrared spectrum of an exoplanet, to identifying the most distant galaxiesB.T. Soifer, Spitzer Science Center, Pasadena, CA; B.T. Soifer, known. Spitzer observations have defined the timescale of planetary system formation,Caltech, Pasadena, CA as well as the timescale for buildup of stellar mass in galaxies. Its spectroscopic observations have discovered water raining down on forming planetary systems and08:30 AM-09:20 AM buckyballs in space as well as tracing aromatic molecules in dusty galaxies to look-backThe Spitzer Space Telescope is NASA’s Great Observatory for infrared astronomy. It times of ~ 12 Gyr. Its most important contributions were not anticipated before itswas launched on August 25, 2003 after a more than three decade gestation. As a launch, with the most striking example being its major impact on exoplanet studies, itselfcryogenic mission it operated from 3-160 microns and included imaging and an area that was unknown when the mission was being formulated and designed. In thisspectroscopy. Its cryogenic mission ended on May 15, 2009 when the last of its talk I will describe a few of the major scientific contributions of the Spitzer mission tosuperfluid Helium evaporated. Since then Spitzer has operated in its “warm” phase, astrophysics, and its impact on the field. I will also describe the prospects for futurewhere the 3.6 and 4.5 micron imaging channels continue to operate at full sensitivity. contributions in the Spitzer Warm mission, which will extend through at least the end ofSpitzer has made major discoveries in virtually all areas of astrophysics, ranging from 2014.103 – AGN: Jets and FeedbackOral Session – Room 101A (Long Beach Convention Center) – 07 Jan 2013 10:00 AM to 11:30 AM103.01D – Spectroscopy of the Largest Ever Gamma-Ray Selected AGN Sample 103.04 – Acceleration of Relativistic Jets in the MOJAVE ProgramM.S. Shaw, R.W. Romani, S.E. Healey, P.F. Michelson, Stanford D.C. Homan, Denison Univ., Granville, OHUniversity, Stanford, CA; A.C. Readhead, W. Max-Moerbeck, O.G. 10:40 AM-10:50 AMKing, California Institute of Technology, Pasadena, CA; G. Cotter, We present results and analysis on the acceleration of extra-galactic radio jets on parsecW.J. Potter, University of Oxford, Oxford, UNITED KINGDOM; J. scales as measured by the MOJAVE program: Monitoring Of Jets in AGN with VLBA Experiments. We have added almost four years of kinematic data, expanding theRichards, Purdue University, West Lafayette, IN number of jet features with high quality motions suitable for acceleration analysis to 327,10:00 AM-10:20 AM a 60% increase from our previous study. We confirm our previous result thatWe report on new optical spectroscopy of 459 Fermi blazars---164 Flat Spectrum Radio accelerations parallel to the velocity of jet features are larger on average thanQuasars (FSRQs) and 295 BL Lacertae Objects (BL Lacs) drawn from the First and perpendicular accelerations, indicating that changes in the Lorentz factors of theSecond Fermi LAT AGN Catalogs. Including archival measurements (correcting several features, rather than simple jet bending, are required to explain much of the observederroneous literature values) we have spectroscopic redshifts for 62% (46%) of the LAT accelerations. We perform a more detailed analysis of our earlier result linking theAGN (BL Lacs). We establish firm lower redshift limits via intervening absorption acceleration of jet features with projected distance along the jet. By analyzing jetsystems and statistical lower limits via searches for host galaxies. This provides redshift features with parallel acceleration at least twice the magnitude of their perpendicularconstraints for an additional 49% of the BL Lac sample leaving only 5% of the BL Lacs acceleration, we select the features most likely to have experienced Lorentz factorunconstrained. The new redshifts raise the median spectroscopic z of the BL Lacs from changes. Features with positive accelerations, indicating increasing Lorentz factor, occur0.23 to 0.33 and includes redshifts as large as z=2.2. Spectroscopic absorption limits at shorter projected distances in the jet than features with negative accelerations.have z= 0.70, showing a substantial fraction at large z and arguing against strong Features with positive and negative accelerations form distinct populations in terms of jetnegative evolution. We find that detected BL Lac hosts are bright ellipticals with hole distance with a probability of less than one in a million of being drawn from the samemasses ~ 10^{8.5-9} M_{sun}, substantially larger than the mean of optical AGN. The distribution. If the motion of jet features reflects the underlying jet flow, our resultsFSRQs have smaller virial estimates of black hole mass than the optical quasar sample. indicate that the transition from positive acceleration out of the SMBH/accretion diskThis appears to be largely due to a preferred (axial) view of the gamma-ray FSRQ and system to deceleration of the larger scale jet occurs at projected distances in the rangenon-isotropic (H/R ~ 0.4) distribution of broad-line velocities. The power-law dominance ~10-20 pc, corresponding to de-projected distances of order 102 pc from the centralof the optical spectrum extends to extreme values, but within the BL Lac class, this does engine. The MOJAVE project is supported under NASA-Fermi grants NNX08AV67Gnot strongly correlate with the gamma-ray properties, suggesting that strong beaming is and 11-Fermi11-0019.the primary cause of the range in continuum dominance. This substantially completesurvey provides new opportunities for understanding blazar evolution and their role in 103.05 – A Universal Scaling for the Energetics of Black Hole Jetscontributions to, and probes of, the cosmic extragalactic background. R. Nemmen, S. Guiriec, N. Gehrels, NASA GSFC, Greenbelt, MD;103.02 – Correlation Between Black Hole Mass and Bulge Luminosity in 235 Nearby M. Georganopoulos, University of Maryland Baltimore County,Active Galaxies Baltimore, MD; E.T. Meyer, Rice University, Houston, TX; R.M.M. Kim, L.C. Ho, Carnegie Observatory, Pasadena, CA; M. Kim, Sambruna, George Mason University, Virginia, VAKASI, Daejeon, KOREA, REPUBLIC OF; C.Y. Peng, Giant 10:50 AM-11:00 AMMagellan Telescope Organization, Pasadena, CA; A.J. Barth, Active galactic nuclei (AGNs) and gamma-ray bursts (GRBs) produce powerfulUniversity of California at Irvine, Irvine, CA; M. Im, Seoul National relativistic jets and their central engines share the same basic astrophysical ingredients,University, Seoul, KOREA, REPUBLIC OF despite the vastly different mass scales of the accreting black holes. An outstanding question is how the jet physics scales from stellar to supermassive black holes. In this10:20 AM-10:30 AM talk, I will report the discovery of a universal scaling for the energetics of relativistic jetsWe present the correlation between the bulge luminosity of host galaxies and the black based on observations of AGNs and GRBs made with the Fermi and Swifthole (BH) masses of nearby (z < 0.35) type I active galactic nuclei (AGNs) from the observatories. I will discuss how this result paves the road to an unified understanding of2-D image composition of HST archival images for 235 objects. We find that the zero black hole activity across the mass scale.point of the relation for AGNs is significantly smaller than that for quiescent galaxies.We also find that the zero point is highly sensitive to accretion rate and BH mass, while 103.06 – Radiative Transfer, Black Hole Growth, AGN Feedback in Galaxiesit appears to be independent of other properties of AGNs and galaxies, such as radio-loudness, presence of a bar, or signs of interactions. We show that the offset in the BH G. Novak, Paris Observatory, Paris, FRANCEmass-bulge luminosity relation can be explained in three ways: (1) bulge luminosity is 11:00 AM-11:10 AMenhanced by recent star formation, (2) BH is rapidly growing during the AGN phase, or We have performed 3D hydrodynamic simulations of black hole fueling and AGN(3) BH mass is underestimated and the scaling factor increases with increasing feedback using a novel method for treating the radial forces on interstellar gas due toaccretion rate. absorption of photons by dust grains. The method provides a solution to the radiative transfer equation and hence computes forces on the gas self-consistently by first solving103.03 – Sub-mm Observations of Low-luminosities AGNs for a Complete SED for the radiation field taking into account radiation sources, absorption, and scattering.H. Flohic, Universidad de Chile, Santiago, CHILE The algorithm gives the correct behavior in all of the relevant limits (dominated by the central point source; dominated by the distributed isotropic source; optically thin;10:30 AM-10:40 AM optically thick to UV/optical; optically thick to IR) and reasonably interpolates betweenWith APEX, we measured the sub-mm flux of 5 low-luminosity AGNs in order to fill the the limits when necessary. The simulations allow us to study gas flows and feedbackgap in the spectral energy distribution (SED). With a more complete SED, we are now processes over length scales from ~1 pc to ~100 kpc. We find that the dynamics andable to better determine the relative contribution of jet and accretion power to the final state of simulations are measurably but only moderately affected by radiativeluminosity, and to assess the structure of the accretion flow. forces on dust, even when assumptions about the dust-to-gas ratio are varied from zero to a value appropriate for the Milky Way. In simulations with high gas densities designed
  6. 6. to mimic ULIRGs with a star formation rate of several hundred solar masses per year, 103.08 – Re-examining the Black Hole in M87 Through Gas-dynamical Modelingdust makes a more substantial contribution to the dynamics and outcome of thesimulation. J. Walsh, The University of Texas at Austin, Austin, TX; A.J. Barth, University of California, Irvine, Irvine, CA; L.C. Ho, Carnegie103.07 – Measuring Feedback from Mass Outflows of Ionized Gas in Nearby AGN Observatories, Pasadena, CA; M. Sarzi, University of Hertfordshire,D.M. Crenshaw, T.C. Fischer, Georgia State Univ., Atlanta, GA; Hatfield, UNITED KINGDOMS.B. Kraemer, The Catholic University of America, Washington, 11:20 AM-11:30 AMDC; H.R. Schmitt, Naval Research Laboratory, Washington, DC; J. M87 is one of the most luminous nearby galaxies and hosts one of the most massiveTurner, University of Maryland, Baltimore County, Baltimore, MD black holes known, making it a very important target for extragalactic studies. The11:10 AM-11:20 AM supermassive black hole has been the subject of several stellar and gas-dynamical mass measurements; however the best current measurements disagree by a factor of 2,We present an investigation into the impact of feedback from outflows of ionized gas in corresponding to a 2-sigma discrepancy. Given the uncertainties associated with thenearby (z < 0.04) AGN. From our studies of outflowing UV a and X-ray absorbers, we sparsely populated upper end of the relationships between black hole mass and hostfound that most Seyfert 1 galaxies with moderate bolometric luminosities have mass galaxy bulge properties, resolving this disagreement in the M87 black hole mass isoutflow rates that are 10 - 1000 times the mass accretion rates needed to generate their crucial. Here, we present newly acquired multi-slit Space Telescope Imagingobserved luminosities, indicating that most of the mass outflow originates from outside Spectrograph observations from the Hubble Space Telescope. We measure thethe inner accretion disk. We also found that many of these AGN have kinetic emission-line kinematics within ~40 pc of the M87 nucleus, fully mapping out the nuclearluminosities in the range 0.5 to 5% bolometric, which is in the range often suggested by gas disk. We will present preliminary results from the comprehensive gas-dynamicalfeedback models needed for efficient self-regulation of black-hole and galactic bulge modeling and constraints on the black hole mass.growth. We investigate the possibility that mass outflows on larger scales (hundreds ofparsecs) may provide similar or even larger mass outflow rates and kinetic luminositiesin nearby, moderate luminosity AGN.104 – Circumstellar Disks IOral Session – Room 202B (Long Beach Convention Center) – 07 Jan 2013 10:00 AM to 11:30 AM104.01 – Weak Accretion in the Outer Regions of Protoplanetary Disks 104.03 – From Dust to Planetesimals: Criteria for Gravitational Instability of Small Particles in GasJ.B. Simon, P.J. Armitage, K. Beckwith, University of Colorado,Boulder, CO; X. Bai, J.M. Stone, Princeton University, Princeton, J. Shi, E. Chiang, UC Berkeley, Berkeley, CA; J. Shi, E. Chiang,NJ; X. Bai, Harvard-Smithsonian Center for Astrophysics, Center for Integrative Planetary Science, Berkeley, CACambirdge, MA; K. Beckwith, Tech-X Corporation, Boulder, CO 10:30 AM-10:40 AM10:00 AM-10:10 AM Dust particles sediment toward the midplanes of protoplanetary disks, forming dust-rich sublayers encased in gas. What densities must the particle sublayer attain before it canI will present numerical simulations of turbulence in the outer regions of protoplanetary fragment by self-gravity? We describe various candidate threshold densities. One ofdisks. In these regions, low ionization levels and gas densities lead to weak coupling these is the Roche density, which is that required for a strengthless satellite to resist tidalbetween neutral and ionized gas, enhancing the effect of ambipolar diffusion drastically. disruption by its primary. Another is the Toomre density, which is that required forOnly very thin surface layers of the disk are well ionized due to FUV photons from the de-stabilizing self-gravity to defeat the stabilizing influences of pressure and rotation. Wecentral star. Our simulations focus on turbulent accretion driven by the show that for sublayers containing aerodynamically well-coupled dust, the Toomremagnetorotational instability (MRI) in the absence of a vertical magnetic field density exceeds the Roche density by many (up to about 4) orders of magnitude. Wepenetrating the disk. The result is a form of layered accretion, akin to the Ohmic dead present 3D shearing box simulations of self-gravitating, stratified, dust-gas mixtures tozone paradigm relevant to smaller disk radii; gas is only accreted through very thin test which of the candidate thresholds is relevant for collapse. All our simulationssurface layers that surround a magnetically inactive ambipolar dead zone. We find that indicate that the larger Toomre density is required for collapse. This result is sensiblethe measured accretion rates due to this strong ambipolar diffusion are too small, by at because sublayers are readily stabilized by pressure. Sound-crossing times for thinleast an order of magnitude, to account for observations. I will discuss the implications layers are easily shorter than free-fall times, and the effective sound speed in dust-gasof these results for disk evolution, and a promising solution to the problem by including a suspensions decreases only weakly with the dust-to-gas ratio (as the inverse squarevertical magnetic field. root). Our findings assume that particles are small enough that their stopping times in gas are shorter than all other timescales. Relaxing this assumption may lower the104.02D – The Earliest Stage of Planet Formation: Disk-Planet Interactions in threshold for gravitational collapse back down to the Roche criterion. In particular, if theProtoplanetary Disks and Observations of Transitional Disks particle stopping time becomes longer than the sound-crossing time, sublayers may loseR. Dong, R. Rafikov, J.M. Stone, Princeton University, Princeton, pressure support and become gravitationally unstable.NJ; L.W. Hartmann, University of Michigan, Ann Arbor, MI 104.04 – The Effect of Dust Self-Gravity on the Kelvin-Helmholtz Instability of Settled10:10 AM-10:30 AM Dust Layers in Protoplanetary DisksI will first talk about numerical simulations of disk-planet interactions in protoplanetary J.A. Barranco, San Francisco State University, San Francisco, CA;disks. Particularly, I’ll discuss the damping of the density waves excited by planets dueto the nonlinearity in their propagation, which can result in gap opening in a low viscosity E. Chiang, University of California, Berkeley, Berkeley, CAdisk by low mass planets. Ill also discuss the effects of various numerical algorithms 10:40 AM-10:50 AMand parameters in simulations of disk-planet interaction, and address the question of how It is a remarkable fact that planets start out as microscopic grains within protoplanetaryto produce correct simulations. Then I’ll move on to recent Subaru observations of disks of gas and dust in orbit around newly-formed protostars, somehow growing by atransitional disks, which are protoplanetary disks with central depleted regions (cavities).Several ideas on the formation of transitional disks have been proposed, including gaps factor of 1040 in mass in a period no more than 107 years. In the early stages of theopened by planet(s). Recently, Subaru directly imaged a number of such disks at near planet formation, small dust grains settle into the midplane of the disk in a few thousandinfrared (NIR) wavelengths (the SEEDS project) with high spatial resolution and small years. As the dust layer gets thinner, a vertical shear develops between the dust-richinner working angles. Using radiative transfer simulations, we study the structure of layer at the midplane and the dust-poor gas above and below. Of great interest istransitional disks by modeling the NIR images, the SED, and the sub-mm observations whether such a layer will be unstable to Kelvin-Helmholtz instability (KHI), which willfrom literature (whenever available) simultaneously. We obtain physical disk+cavity remix the dust with the gas, thwarting the formation of planets. We work in thestructures, and constrain the spatial distribution of the dust grains, particularly inside the single-fluid limit in which the local dust-to gas ratio is an advectively conserved quantitycavity and at the cavity edge. Interestingly, we find that in some cases cavities are not (valid when the dust-gas friction time is very short). Here, we present new simulationspresent in the scattered light. In such cases we present a new transitional disk model to which include the effect of dust self-gravity on the stability of the dust layer and exploresimultaneously account for all observations. Decoupling between the sub-um-sized and parameter space to determine under what conditions further settling may triggermm-sized grains inside the cavity is required, which may necessitate the dust filtration gravitational instability and the direct formation of planetesimals.mechanism. For another group of transitional disks in which Subaru does reveal thecavities at NIR, we focus on whether grains at different sizes have the same spatial 104.05 – Probing for Exoplanets Hiding in Dusty Debris Disks III: Disk Imaging,distribution or not. We use our modeling results to constrain transitional disk formation Characterization, and Exploration with HST/STIS Multi-Roll Coronagraphy - Completingtheories, particularly to comment on their possible planets origin. the Survey G. Schneider, Univ. of Arizona, Tucson, AZ
  7. 7. 10:50 AM-11:00 AM 104.06 – A Search for Exozodis with KeplerSpatially resolved images of light-scattering circumstellar debris in exoplanetary systems C.C. Stark, A.P. Boss, A.J. Weinberger, B. Jackson, Carnegieconstrain the physical properties and orbits of the dust grains in these systems. Such Institution of Washington, Washington, DC; M. Endl, W.D.images also inform on co-orbiting (but unseen) planets and the systemic architectures.Using HST/STIS broadband optical coronagraphy, we have recently (Nov. 2012) Cochran, C. Caldwell, University of Texas, Austin, TX; E. Agol,completed the observational phase of a program to study the spatial distribution of dust University of Washington, Seattle, WA; E.B. Ford, University ofin a well-selected sample of 11 circumstellar debris disks, all with HST pedigree, using Florida, Gainesville, FL; J. Hall, K. Ibrahim, Orbital SciencesSTIS visible-light PSF-subtracted multi-roll coronagraphy. In many cases, these new Corporation/NASA Ames Research Center, Moffett Field, CA; J. Li,observations probe the interior regions of these debris systems, with inner working SETI Institute/NASA Ames Research Center, Moffett Field, CAdistances < app 8 AU for half the stars in this sample, corresponding to the giant planetand Kuiper belt regions within our own solar system. These observations also reveal 11:00 AM-11:10 AMdiffuse low-surface brightness dust at larger stellocentric distances, observations of Planets embedded within exozodiacal dust disks may form large scale clumpy dustwhich remain a technical challenge to the most aggressive and advanced ground based structures by trapping dust into resonant orbits. When viewed edge-on, these clumpytechniques and facilities We have previously reported preliminary observational results dust structures periodically pass in front of their host star, creating orbit-long light curvefrom this program of a subset of the brighter disks (in both surface brightness and variations potentially detectable with Kepler. Here I present the first search for thesef_disk/f_star scattering fraction). Here in present new results, including fainter disks resonant structures in the inner regions of planetary systems by analyzing the lightsuch as HD 92945 (f_disk/f_star approximately 5E-5) for which we confirm (and better curves of planet candidate host stars identified by the Kepler mission. Our detectionreveal) the existence of an inner dust ring within a larger diffuse dust disk as suggested routine produced one promising candidate disk structure associated with a hot Jupiterfrom earlier ACS observations. These new images from our HST/STIS GO 12228 planet candidate. However, radial velocity measurements show this planet candidate toprogram enable direct inter-comparison of the architectures of these exoplanetary debris be an eclipsing binary with an unusual periodic signal. We use our null result to place ansystems in the context of our own Solar System. Based on observations made with the upper limit on the frequency of high contrast resonant dust clumps, a useful metric forNASA/ESA Hubble Space Telescope obtained at, and with support for program #12228 future missions that aim to image extrasolar planets in the inner regions of theirfrom, the STScI, which is operated by the AURA, Inc., under NASA contract NAS planetary systems.5-26555. These observations are associated with program #12228.105 – Cosmic Microwave Background IOral Session – Grand Ballroom (Long Beach Convention Center) – 07 Jan 2013 10:00 AM to 11:30 AM105.01 – New Results from the Atacama Cosmology Telescope (ACT): Maps and 105.04 – ACTPol: A New Instrument to Measure CMB Polarization with the AtacamaPower Spectra Cosmology TelescopeJ.L. Sievers, Princeton University, Princeton, NJ; J.L. Sievers, M. Niemack, Cornell University, Ithaca, NY; M. Niemack, NationalUKZN, Durban, SOUTH AFRICA Institute of Standards and Technology, Boulder, CO10:00 AM-10:10 AM 10:40 AM-10:50 AMThe Atacama Cosmology Telescope (ACT) observed the Cosmic Microwave We are in the process of building and deploying ACTPol: a new polarization-sensitiveBackground from high in the Chilean Andes from 2007-2010. We present the final 148 receiver for the six-meter Atacama Cosmology Telescope. ACTPol will be used toand 220 GHz maximum-likelihood maps and power spectra from data taken along two measure the CMB polarization on arcminute scales in two frequency bands centeredstripes of constant declination. The maps cover ~1300 square degrees, the deepest 600 near 90 and 150 GHz. These measurements will provide improved constraints onof which are used in power spectrum estimation. Typical depths for the power spectrum cosmological parameters as well as measurements of the projected mass distribution viaregions are 20-25 uK-arcmin (CMB) for the 148 GHz mps and 35-40 uK-arcmin gravitational lensing of the CMB, which can be used to probe early dark energy,(CMB) for the 220 GHz maps. curvature, and the sum of the neutrino masses. In addition, we project that ACTPol will be ~4x more sensitive than the previous ACT receiver at 150 GHz, enabling improved105.02D – New Results from the Atacama Cosmology Telescope (ACT): Cosmological CMB temperature science, such as surveys for galaxy clusters via the Sunyaev-Parameters from the Complete ACT Survey Zeldovich effect. We will describe the science goals and status of the instrument.R. Hlozek, Princeton University, Princeton, NJ 105.05D – Measuring the Cosmic Microwave Background Polarization with SPT-POL10:10 AM-10:30 AM A. Crites, University of Chicago, Chicago, ILThe Atacama Cosmology Telescope (ACT) has mapped the microwave sky to 10:50 AM-11:10 AMarcminute scales. We present constraints on parameters from the observations at 148and 217 GHz respectively by ACT from 2007-2010. Efficient map-making and A new polarization-sensitive camera, SPT-POL, designed to measure the polarization ofspectrum-estimation techniques allow us to probe the acoustic peaks deep into the the cosmic microwave background (CMB), was deployed on the 10 meter South Poledamping tail, and allow for confirmation of the concordance model, and tests for Telescope in January 2012. The goal of the project is to exploit the high resolution of thedeviations from the standard cosmological picture. We fit a model of primary telescope (1 arcminute beam) and the high sensitivity afforded by the 1536 detectorcosmological and secondary foreground parameters to the dataset, including camera to characterize the B-mode polarization induced by the gravitational lensing ofcontributions from both the thermal and kinetic Sunyaev-Zeldovich effect, Poisson the primordial E-mode CMB polarization, as well as to detect or set an upper limit on thedistributed and correlated infrared sources, radio sources and a term modeling the level of the B-mode polarization from inflationary gravitational waves. The lensingcorrelation between the thermal SZ effect and the Cosmic Infrared Background. We B-modes will be used to constrain the sum of the neutrino masses by measuring largewill describe the multi-frequency likelihood for the ACT data, and present constraints on scale structure, while the inflationary B-modes are sensitive to the energy scale ofa variety of cosmological parameters using this complete dataset. inflation. I will discuss the development of the SPT-POL camera including the cryogenic design and the transition edge sensor (TES) detectors as well as the science goals and105.03 – New Results from the Atacama Cosmology Telescope (ACT): The Kinematic status of the ongoing of the SPT-POL program.Sunyaev-Zeldovich Effect 105.06D – The Atacama Cosmology Telescope: Mapping Dark Matter with CMBN. Hand, University of California Berkeley, Berkeley, CA Lensing10:30 AM-10:40 AM B. Sherwin, Princeton University, Princeton, NJUsing the millimeter-wavelength data from the Atacama Cosmology Telescope (ACT), 11:10 AM-11:30 AMthe motions of galaxy clusters and groups were detected for the first time through theirtemperature distortions of the cosmic microwave background (CMB) due to the Measurements of lensing in the cosmic microwave background (CMB) directly probekinematic Sunyaev-Zeldovich effect. The positions of galaxy clusters in the ACT data the projected distribution of dark matter out to high redshifts. I will describe the firstwere identified by their constituent luminous galaxies, as observed by the Baryon detection of the power spectrum of CMB lensing with the Atacama CosmologyOscillation Spectroscopic Survey (BOSS). I will describe the initial measurement of the Telescope (ACT) and its cosmological implications, and will show results from cross-mean pairwise momentum, and subsequent attempts to use this result to provide an correlations of ACT CMB lensing maps with quasars, galaxies and other tracers of darkestimate of the average baryon mass fraction on cluster length scales for our galaxy matter. I will then explain the great scientific potential of upcoming polarization lensingsample. measurements with ACTPol, and will discuss the development of a lensing pipeline for this experiment.
  8. 8. 106 – Cosmology IOral Session – Room 103B (Long Beach Convention Center) – 07 Jan 2013 10:00 AM to 11:30 AM 10:30 AM-10:40 AM106.01 – A New, Precise Measurement of the Primordial Abundance of DeuteriumR. Cooke, M. Pettini, Institute of Astronomy, Cambridge, UNITED Weak gravitational lensing due to large scale structure (cosmic shear) has been shown to be contaminated by the intrinsic alignment (IA) of galaxies, which poses a barrier toKINGDOM; R. Cooke, Astronomy & Astrophysics, UC Santa Cruz, precision weak lensing measurements in planned surveys. To address this contamination,Santa Cruz, CA we have extended the 2-point self-calibration techniques to the cosmic shear bispectrum,10:00 AM-10:10 AM using information already measured in a weak lensing survey to self-calibrate the IA contamination. The 3-point self-calibration techniques use the redshift separationWe are currently in an exciting era of precision cosmology. With the imminent release of dependencies of the IA bispectra and the non-linear galaxy bias in order to isolate andthe cosmic microwave background data recorded by the Planck satellite, we will soon remove the impact of the IA correlations on the cosmic shear signal. Using conservativebe presented with an opportunity to accurately test the standard model of Big Bang estimates of photo-z accuracy, we find that planned surveys will be able to measure theNucleosynthesis. However, independent measures of the primordial deuterium IA redshift separation dependence over ranges in photo-z of 0.2 in the 3-point ellipticityabundance, to be analysed in conjunction with the baryon density determined by Planck, auto-correlation. For the 3-point cross-correlations, we find that the self-calibrationare vital in order to achieve this goal. In this talk, I will present a new, precise measure technique allows for reductions in the IA contamination by a factor of 10 or more overof the primordial abundance of deuterium - the most accurate measurement to date - most scales and redshift bin choices and in all cases by a factor of 3-5 or more. Thederived from the spectrum of a redshift ~ 3 metal-poor damped Lyman-alpha system. 3-point self-calibration techniques thus provide a means to greatly reduce the impact ofSuch accurate measures are now able to place strong limits on the effective number of IA contamination of the bispectrum in future measurements of cosmic shear.neutrino species in the early Universe, which depends only on the primordial deuteriumabundance and the baryon density of the Universe. Using our measure of the deuteriumabundance in conjunction with the WMAP 7 year data release, we find that the number 106.05 – Cosmology from SALT II Fitted Supernovae Ia: A Bayesian Hierarchicalof neutrino families = 3.0 +/- 0.5, in good agreement with both the standard model and Analysis of the Supernovae Systematic Uncertainties and Statistical Properties of thethat measured with particle colliders. Finally, I shall discuss an ongoing survey to search Light-curve Stretch and Color Parametersfor additional damped Lyman-alpha systems where such precise measurements of M. March, University of Sussex, Brighton, East Sussex, UNITEDdeuterium are available. With just a small handful of systems, we may soon be able to KINGDOM; R. Trotta, Imperial College , London, Greater London,pin down the number of neutrino families when the Universe was in its infancy. UNITED KINGDOM; M. Smith, University of Cape Town, Cape Town, SOUTH AFRICA; G.D. Starkman, Case Western Reserve106.02 – The WiggleZ Dark Energy Survey: Final Results University, Cleveland, OHT. Davis, D. Parkinson, S. Riemer-Sørensen, M. Drinkwater, 10:40 AM-10:50 AMUniversity of Queensland, Brisbane, Queensland, AUSTRALIA; C.Blake, G.B. Poole, E. Kazin, K. Glazebrook, W. Couch, Swinburne The Supernova Bayesian Hierarchical Model (SNBHM) provides a framework for cosmological parameter inference and model selection in which the statistical propertiesUniversity of Technology, Melbourne, Victoria, AUSTRALIA; M. of the SNIa population are fully modeled. We demonstrate how the SNBHM can beScrimgeour, F. Beutler, University of Western Australia, Perth, used to extract information about the statistical properties of the SNIa population.Western Australia, AUSTRALIA Supernovae Ia light-curves fitted with the SALT II fitter are each characterized by a10:10 AM-10:20 AM colour c and stretch x1 parameter and an absolute B-band magnitude mB. These fitted parameters, along with the SN global parameters α and β are used to reduce the scatterObservations are now complete for the WiggleZ dark energy survey and we have in the Hubble diagram in order that constraints on the cosmological parameters may bemapped the positions of ~220,000 bright blue galaxies out to a redshift of z~1, over a obtained. The SNBHM can be used to obtain an estimate for the unknown systematiccubic giga-parsec of space. I will present the full complement of cosmological results uncertainty which characterizes the residual scatter about the Hubble diagram whichcoming out of this data set. With the addition of WiggleZ data, baryon acoustic remains even after application of the stretch and color correction. We show how theoscillations are now able to confirm the acceleration of the expansion of the universe, mean and variance of the underlying stretch and color parameters which characterizeindependent of any supernova data, and this has since been further strengthened by the the SALT II fitted SN light curves can be recovered using the SNBHM, either for theaddition of Baryon Oscillation Spectroscopic Survey data. Arguably the most exciting whole SN sample or as a function of survey or redshift. We investigate the effect aresults are our measurements of the growth of structure out to z~0.8, and measurements non-Gaussian distribution of color parameters has on the ability of the SNBHM toof the Alcock-Paczynski effect (sphericity of spheres) that allow us to measure the rate recover the cosmological parameters. We apply the SNBHM to both simulated and realof expansion at different redshifts H(z) without needing a cosmological model. These data sets, and we present results of the SNBHM cosmological analysis of the combinedallow us to distinguish between non-standard models of gravity that are indistinguishable Low Z, Sloan Digital Sky Survey (SDSS), Supernova Legacy Survey (SNLS3) andusing only measurements of expansion rate. I will also cover our constraints on the mass Hubble Space Telescope (HST) data sets, and its statistical properties.of the neutrino and the effective number of neutrinos, which are amongst the tightestconstraints available from any experiment. Finally, I will show how the large volume we 106.06D – Correlations Between Type Ia Supernovae and Their Host Galaxies Usinghave sampled has allowed us to detect the scale at which the universe transitions from the SDSS and Multi-wavelength Photometryclustered to homogeneous, confirming one of the cornerstones of modern cosmology.The WiggleZ data have now been made public, and include data, random catalogues, R. Gupta, C. DAndrea, M. Sako, University of Pennsylvania,and lognormal realizations. With it we have also released our CosmoMC module so our Philadelphia, PA; C. Conroy, Harvard-Smithsonian Center fordata can easily be included in your own cosmological analyses. Astrophysics, Cambridge, MA; M. Smith, Astrophysics, Cosmology and Gravity Centre, Cape Town, SOUTH AFRICA; B. Bassett,106.03 – Interactive Cosmological Data Fitting Simulations: A Further Examination of South African Astronomical Observatory, Cape Town, SOUTHCosmoEJS AFRICA; B. Bassett, Dept. of Mathematics and AppliedJ. Moldenhauer, L. Engelhardt, K.M. Stone, E. Shuler, Francis Mathematics, University of Cape Town, Cape Town, SOUTHMarion University, Florence, SC AFRICA; J. Frieman, R. Kessler, Department of Astronomy &10:20 AM-10:30 AM Astrophysics, University of Chicago, Chicago, IL; J. Frieman, J.We discuss usage and development of a collection of cosmological modeling programs Marriner, Fermilab, Batavia, IL; P.M. Garnavich, Department ofbuilt with Easy Java Simulations. These interactive programs allow for modeling of theaccelerated expansion of the universe (cosmic acceleration). The simulations compare Physics, University of Notre Dame, Notre Dame, IN; S. Jha,theoretical models to experimental data sets with real-time plotting and numerical fitting. Department of Physics & Astronomy, Rutgers, the State UniversityWe include several models for the user to choose, or design their own. We also provide of New Jersey, Piscataway, NJ; R. Kessler, Kavli Institute fora range of surveys from different observations. We have simple versions of the Cosmological Physics, The University of Chicago, Chicago, IL; C.programs available for teaching and more sophisticated versions for research. All of the DAndrea, H. Lampeitl, R. Nichol, Institute of Cosmology andprograms can be found at Compadre Open Source Physics website, Gravitation, University of Portsmouth, Portsmouth, UNITED KINGDOM; D.P. Schneider, Department of Astronomy &106.04 – Self-Calibration Techniques for 3-point Intrinsic Alignment Correlations in Astrophysics, The Pennsylvania State University, University Park,Weak Gravitational Lensing Surveys PAM.A. Troxel, M.B. Ishak-Boushaki, University of Texas at Dallas, 10:50 AM-11:10 AMRichardson, TX We improve estimates of the stellar mass and mass-weighted average age of Type Ia
  9. 9. supernova (SN Ia) host galaxies by combining UV and near-IR photometry with optical A&M University, College Station, TX; J. Hennawi, Max Planckphotometry in our analysis. Using 206 SNe Ia drawn from the full three-year Sloan Institute for Astronomy, Heidelberg, GERMANY; C. Lidman,Digital Sky Survey (SDSS-II) Supernova Survey (median redshift of z ≈ 0.2) and multi-wavelength host-galaxy photometry from SDSS, the Galaxy Evolution Explorer, and the Australian Astronomical Observatory, Epping, New South Wales,United Kingdom Infrared Telescope Infrared Deep Sky Survey, we present evidence of AUSTRALIA; J. Mendez, P. Ruiz-Lapuente, University ofa correlation (1.9σ confidence level) between the residuals of SNe Ia about the best-fit Barcelona, Barcelona, SPAIN; E.S. Rykoff, Stanford LinearHubble relation and the mass-weighted average age of their host galaxies. The trend is Accelerator Center, Menlo Park, CAsuch that older galaxies host SNe Ia that are brighter than average after standardlight-curve corrections are made. We also confirm, at the 3.0σ level, the trend seen by 11:10 AM-11:30 AMprevious studies that more massive galaxies often host brighter SNe Ia after light-curve We have obtained deep, very high signal-to-noise ratio spectra of a sample of 40 hostcorrection. galaxies of Type Ia supernovae (SNe). The host galaxies are chosen from the Nearby SN Factory, the SDSS SN Survey, and Swift-observed SNe, with the requirement that106.07D – Correlations Between Type Ia Supernova Properties and Early-type Host they have passive stellar populations. We perform a detailed stellar population analysisGalaxy Spectra of the SN host galaxies, measuring their ages and the abundances of multiple elements, including Fe, Mg, C, N, and Ca. We find that the age and abundance patterns of the SNJ. Meyers, G. Graves, H. Fakhouri, J. Nordin, S. Perlmutter, D. hosts are similar to those of a control sample of early-type SDSS galaxies. WeRubin, C. Saunders, University of California Berkeley, Berkeley, rediscover the correlation between the SN decline rate and host galaxy age, and showCA; J. Meyers, G. Graves, G.S. Aldering, H. Fakhouri, J. Nordin, that host [Mg/Fe], [C/Fe], and [N/Fe] enhancement are also correlated with SN declineS. Perlmutter, D. Rubin, C. Saunders, A.L. Spadafora, N. Suzuki, rates. In contrast to studies of SNe with mixed host types, however, we do not see anyLawrence Berkeley National Laboratory, Berkeley, CA; R. evidence for correlations between SN Hubble residuals and early-type host galaxy properties, suggesting that Hubble residual correlations with host properties saturate atAmanullah, Stockholm University, Stockholm, SWEDEN; K.H. the domains of early-type galaxies.Barbary, Argonne National Lab, Argonne, IL; P.J. Brown, Texas107 – Dwarf and Irregular Galaxies I: Origins and DynamicsOral Session – Room 104A (Long Beach Convention Center) – 07 Jan 2013 10:00 AM to 11:30 AM V(Rd)/Rd, where Rd is the galaxy scale-length. We find that V(Rd)/Rd correlates with107.01D – The Origin of Dwarf Early-Type Galaxies i) the central surface brightness; ii) the mean HI surface density over the stellar disk;E. Toloba, University of California Santa Cruz, Santa Cruz, CA; E. and iii) the SFR density. BCDs have higher V(Rd)/Rd than typical irregulars, suggestingToloba, Carnegie Observatories, Pasadena, CA; A. Boselli, that the starburst activity is closely linked with the gravitational potential and the concentration of gas. We decompose the rotation curves of BCDs into massLaboratoire dAstrophysique de Marseille-LAM, Marseille, components and find that baryons (stars and gas) are dynamically important. This isFRANCE; J. Gorgas, Universidad Complutense de Madrid, remarkable, as dwarf galaxies are commonly thought to be entirely dominated by darkMadrid, SPAIN matter. We discuss the implications of these results on the evolution of dwarf galaxies10:00 AM-10:20 AM and in particular on the properties of the progenitors and descendants of BCDs.The physical mechanisms involved in the formation and evolution of dwarf early-type 107.03 – Dark Matter Profiles in Late-type Dwarf Galaxies from Stellar Kinematicsgalaxies (dEs) are not well understood yet. Whether these objects, that outnumber anyother class of object in clusters, are the low luminosity extension of massive early-type J.J. Adams, J.D. Simon, Observatories of the Carnegie Institution ofgalaxies, i.e. formed through similar processes, or are a different group of objects Washington, Pasadena, CA; M.H. Fabricius, Max-Planck Institutpossibly formed through the transformation of low luminosity spiral galaxies, is still an für extraterrestrische Physik, München, GERMANY; K. Gebhardt,open debate. Studying the kinematic properties of dEs is a powerful way to distinguishbetween these two scenarios. In my PhD, awarded with a Fulbright postdoctoral University of Texas at Austin, Austin, TXFellowship and with the 2011 prize to the best Spanish PhD dissertation in Astronomy, 10:30 AM-10:40 AMwe used this technique to make a spectrophotometric analysis of 18 dEs in the Virgo We present new stellar and gaseous velocity fields for thirteen late-type dwarf galaxies,cluster. I found some differences for these dEs within the cluster. The dEs in the outer primarily to study the density distributions of their baryons and dark matter. A subset ofparts of Virgo have rotation curves with shapes and amplitudes similar to late-type our targets reach high enough signal-to-noise that the central dark matter density profilegalaxies of the same luminosity. They are rotationally supported, have disky isophotes, slope can be reliably estimated from the stellar kinematics alone. Most previousand younger ages than those dEs in the center of Virgo, which are pressure supported, observations have been based on kinematics from atomic or ionized gas and haveoften have boxy isophotes and are older. Ram pressure stripping, which removes the gas derived best-fit profiles much shallower than those predicted by pure N-body simulationsof galaxies leaving the stars untouched, explains the properties of the dEs located in the in ΛCDM. In contrast to those results, we find from the stellar kinematics that galaxiesoutskirts of Virgo. However, the dEs in the central cluster regions, which have lost their contain a wide variety of density profiles ranging from completely cored halos up toangular momentum, must have suffered a more violent transformation. A combination of cuspy r^-1 profiles comparable to the predicted NFW form. We present ourram pressure stripping and harassment is not enough to remove the rotation and the measurements, demonstrate cases where the gas gives a biased inference on the darkdisky structures of these galaxies. I am conducting new analysis with 20 new dEs to matter properties, and fit Jeans models to the data with baryonic and dark components.throw some light in this direction. I also analysed the Faber-Jackson and the For the cases that deviate from an NFW profile, we search our data for unusual orbitalFundamental Plane relations, and I found that dEs deviate from the trends of massive structure (anisotropies) and chemical abundance gradients in order to constrain theelliptical galaxies towards the position of dark matter dominated systems such as the proposed mechanisms that may alter the initial configuration of the dark matter halo.dwarf spheroidal satellites of the Milky Way and M31. This indicates that dEs have anon-negligible dark matter fraction within their half light radius, we used these diagrams 107.04D – Dynamically Extreme Stellar and Galactic Populations in the Via Lactea IIto quantify this dark matter content, which is ~40%, significantly larger than previously Cosmological Simulation and Their Observable Counterpartsthought for these kind of objects. M. Teyssier, Columbia University, New York, NY107.02 – Dynamics of Starbursting Dwarf Galaxies 10:40 AM-11:00 AMF. Lelli, M.A. Verheijen, F. Fraternali, R. Sancisi, Kapteyn We describe dynamically unusual populations with observable counterparts (backsplashAstronomical Institute, University of Groningen, Groningen, galaxies, wandering stars and high velocity stars) in the environment in and outside of a Milky Way-like object. Analysis of VLII halo histories and z=0 distribution allows us toNETHERLANDS; F. Fraternali, Department of Astronomy, distinguish which Local Group field galaxies may have passed through the virial volumeUniversity of Bologna, Bologna, ITALY; R. Sancisi, INAF - of the Milky Way. We find it likely that Tucana, Cetus, NGC3109, SextansA, SextansB,Astronomical Observatory of Bologna, Bologna, ITALY Antlia, NGC6822, Phoenix, LeoT, and NGC185 have passed through the Milky Way.10:20 AM-10:30 AM Several of these galaxies contain signatures in their morphology, star formation history, and/or gas content, that are indicative of evolution seen in simulations of satellite/parentThe mechanisms that trigger strong bursts of star formation in dwarf galaxies are poorly galactic interactions. We use the histories of VLII particles that are far outside Rvir atunderstood. Blue Compact Dwarfs (BCDs) are nearby starburst galaxies that may hold z=0 to estimate the likelihood of observing inter-galactic supernovae in current andthe key to understand these mechanisms. We are studying a sample of 18 BCDs using near-future large-scale time-domain surveys. Finally, we ask whether a merger historyboth new and archival HI data. In several cases we find that BCDs have a steeply- similar to what is seen in VLII should lead to a significant population of old high-velocityrising rotation curve that flattens in the outer parts. This points to a strong central stars associated with dark matter flows.concentration of mass. We introduce a new parameter to quantify the central massconcentration in dwarf galaxies (BCDs and irregulars): the circular-velocity gradient

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