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230Th AAS Session Table of Contents

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230Th AAS Session Table of Contents 230th AAS Austin, TX – June, 2017 Meeting Abstracts Session Table of Contents 100 – Welcome Address by AAS President Christine Jones (Harvard-Smithsonian, CfA) 101 – Kavli Foundation Lecture: Dark Matter in the Universe, Katherine Freese (University of Michigan) 102 – Extrasolar Planets: Detection and Future Prospects 103 – Instrumentation, and Things to do with Instrumentation: From the Ground 104 – Topics in Astrostatistics 105 – Inner Solar Systems: Planet Compositions as Tracers of Formation Location 106 – Annie Jump Cannon Award: Origins of Inner Solar Systems, Rebekah Dawson (Penn State University) 108 – Astronomy Education: Research, Practice, and Outreach Across the Human Continuum 109 – Bridging Laboratory & Astrophysics: Atomic Physics 110 – Preparing for JWST Observations: Insights from First Light and Assembly of Galaxies GTO Programs I 111 – Inner Solar Systems: Super-Earth Orbital Properties: Nature vs. Nurture 112 – Plenary Talk: The Universe's Most Extreme Star-forming Galaxies, Caitlin Casey (University of Texas, Austin) 113 – Plenary Talk: Science Highlights from SOFIA, Erick Young (USRA) 114 – Preparing for JWST Observations Poster Session 115 – Astronomy Education: Research, Practice, and Outreach Across the Human Continuum Poster Session 116 – Societal Matters Poster Session 117 – Instrumentation Poster Session 118 – Extrasolar Planets Poster Session 119 – The Solar System Poster Session 200 – LAD Plenary Talk: The Rosetta Mission to Comet 67P/ Churyumov-Gerasimenko, Bonnie Buratti (JPL) 201 – Circumstellar Disks, Black Holes, and Binary Stellar Systems 202 – Bridging Laboratory & Astrophysics: Dust & Ices 203 – Preparing for JWST Observations: Insights from First Light and Assembly of Galaxies GTO Programs II 204 – Inner Solar Systems: Origins of Hot and Warm Jupiters 205 – Plenary Talk: Our Future in Space, Christopher Impey (University of Arizona) 207 – Supernovae 208 – Bridging Laboratory & Astrophysics: Molecules 209 – Preparing for JWST Observations: Insights from Birth of Stars and Protoplanetary Systems GTO Programs 210 – Inner Solar Systems: Connecting Inner Solar Systems to Outer Solar Systems 211 – Plenary Talk: Planet Nine from Outer Space, Konstantin Batygin (Caltech) 212 – Plenary Talk: Flows and Flares Around the Nearest Supermassive Black Hole -- Sgr A*, Daniel Wang (University of Massachusetts) 213 – Laboratory Astrophysics Division Poster Session 214 – Galaxies Poster Session 215 – Molecular Clouds and Dust Poster Session 216 – Catalogs, Surveys, and Computation Poster Session 217 – Binary Stellar Systems and Pulsating Variable Stars Poster Session 300 – George Ellery Hale Prize: The Solar Magnetic Field: From Complexity to Simplicity (and Back), Manfred Schüssler (Max Planck Institute) 301 – Stars and Stellar Evolution 302 – Bridging Laboratory & Astrophysics: Planetary Physics and Nuclear/Particle Physics 303 – Preparing for JWST Observations: Insights from Exoplanet, Debris Disk, and Brown Dwarf GTO Programs I 304 – Cosmic Microwave Background 305 – Plenary Talk: CANDELS: A Cosmic Quest for Distant Galaxies Offering Live Views of Galaxy Evolution, David Koo (University of California, Santa Cruz) 307 – Star Formation and Open Clusters 308 – Bridging Laboratory & Astrophysics: Plasma Physics 309 – Preparing for JWST Observations: Insights from Exoplanet, Debris Disk, and Brown Dwarf GTO Programs II 310 – Cosmology 311 – Plenary Talk: On the Explosion Geometry of Red Supergiant Stars, Doug Leonard (San Diego State University) 312 – AAS Members' Meeting 313 – AGN, QSO, and Blazars Poster Session 314 – Cosmology Poster Session 315 – Stars and Stellar Topics Poster Session 316 – Evolution of Galaxies Poster Session 317 – Black Holes and Cataclysmic Variables Poster Session 318 – Supernovae, Supernova Remnants and Planetary Nebulae Poster Session 400 – Plenary Talk: Space Weather: Linking Stellar Explosions to the Human Endeavor, Delores Knipp (University of Colorado) 401 – AGN and Galaxies 402 – Extrasolar Planets: Characterization and Theory 403 – Preparing for JWST Observations: Insights from Solar System GTO Programs 404 – AAS Education Prize: Growth of Astronomy Education in Chile: A Late But Successful Story, Hernán Quintana (Pontificia Universidad Catolica) 100 – Welcome Address by AAS 102 – Extrasolar Planets: Detection President Christine Jones (Harvard- and Future Prospects Smithsonian, CfA) 102.01 – M Dwarf Gas Giant Exoplanet 101 – Kavli Foundation Lecture: Surface Density Distribution: A Log- Normal Fit from 0.07-400 AU Dark Matter in the Universe, We fit a log-normal function to the orbital surface Katherine Freese (University of density distribution of exoplanet populations, over the mass range 1-10 times that of Jupiter, surrounding M Michigan) dwarfs from 0-400 AU. This fit is consistent with 101.01 – Dark Matter in the Universe radial velocity, micro-lensing, and direct imaging “What is the Universe made of?” This question is the observations, is well-motivated from theoretical and longest outstanding problem in all of modern physics, phenomenological viewpoints, and makes predictions and it is one of the most important research topics in of future surveys. We use a Markov Chain Monte cosmology and particle physics today. The ordinary Carlo approach to explore the likelihoods of various atoms that make up the known universe, from our parameter values consistent with point estimators of bodies and the air we breathe to the planets and stars, the available data given our assumed functional form. constitute only 5% of all matter and energy in the We present probability distributions for each cosmos. The remaining 95% is made up of a recipe of parameter as well as a Maximum Likelihood 25% dark matter and 70% dark energy, both Estimation solution. We suggest this function makes nonluminous components whose nature remains a more physical sense than other widely used functions, mystery. I’ll begin by discussing the evidence that and explore the implications of our results on the dark matter is the predominant mass in galaxies, and design of future exoplanet surveys. then turn to the hunt to understand its nature. Author(s): Michael Meyer3, Adam Leading candidates are fundamental particles Amara1, Maddalena Reggiani2, Sascha P. Quanz1 including WIMPs (weakly interacting massive Institution(s): 1. ETH Zürich, 2. Institute of particles), axions, and sterile neutrinos. There are Astrophysics and Geophysics, 3. University of three approaches in the experimental searches for Michigan WIMPs: at the Large Hadron Collider at CERN in Geneva; in underground laboratory experiments; and 102.02 – Exploring the Effects of Stellar with astrophysical searches for dark matter Multiplicity on Exoplanet Occurrence annihilation products. If WIMPs do constitute the dark matter, they would have been the power source Rates for the first stars to form in the Universe; these Dark Determining the frequency of habitable worlds is a Stars may be detectable with the upcoming James key goal of the Kepler mission. During Kepler's four Webb Space Telescope. At the end of the talk I'll turn year investigation it detected thousands of transiting to dark energy and its effect on the future of the exoplanets with sizes varying from smaller than Universe. Mercury to larger than Jupiter. Finding planets was Author(s): Katherine Freese1 just the first step to determining frequency, and for Institution(s): 1. Univ. of Michigan the past few years the mission team has been modeling the reliability and completeness of the Kepler planet sample. One effect that has not typically been built into occurrence rate statistics is that of made to our fully automated candidate vetting stellar multiplicity. If a planet orbits the primary star procedure, which yields specific categories of false in a binary or triple star system then the transit depth positives and a disposition score value to indicate will be somewhat diluted resulting in a modest decision confidence. We present the use of light curve underestimation in the planet size. However, if a inversion and scrambling, in addition to our detected planet orbits a fainter star then the error in continued use of pixel-level transit injection, to measured planet radius can be very significant. We produce artificial planet candidates and false have taken a hypothetical star and planet population positives. Since these simulated data sets were and passed that through a Kepler detection model. subjected to the same automated vetting procedure as From this we have derived completeness corrections the real data set, we are able to measure both the for a realistic case of a Universe with binary stars and completeness and reliability of the catalog. The DR25 compared that with a model Universe where all stars catalog, source code, and a multitude of completeness are single. We report on the impact that binaries have and reliability data products are available at the on exoplanet population statistics. Exoplanet Archive Author(s): Thomas Barclay2, Megan Shabram1 (http://exoplanetarchive.ipac.caltech.edu). The DR25 Institution(s): 1. NASA Ames Research Center, 2. light curves and pixel-level data are available at MAST NASA Goddard Space Flight Center (http://archive.stsci.edu/kepler). Author(s): Jeffrey Coughlin1, Susan E. 102.03 – Determining Statistically Thompson1 Optimal Metric Thresholds for the Final Institution(s): 1. SETI Institute Kepler Planet Candidate Catalog Contributing team(s): Kepler Team The goal of the final
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