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Program Number | Principal Investigator | Program Title | Links |
11107 | Timothy M. Heckman, The Johns Hopkins University | Imaging of Local Lyman Break Galaxy Analogs: New Clues to Galaxy Formation in the Early Universe | Abstract |
11113 | Keith S. Noll, Space Telescope Science Institute | Binaries in the Kuiper Belt: Probes of Solar System Formation and Evolution | Abstract |
11117 | David Kent Sing CNRS, Institut d'Astrophysique de Paris | The Search for Atmospheric Water in the Transiting Planet HD189733b | Abstract |
11120 | Daniel Wang, University of Massachusetts | A Paschen-Alpha Study of Massive Stars and the ISM in the Galactic Center | Abstract |
11122 | Bruce Balick, University of Washington | Expanding PNe: Distances and Hydro Models | Abstract |
11124 | David V. Bowen, Princeton University | The Origin of QSO Absorption Lines from QSOs | Abstract |
11130 | Luis Ho, Carnegie Institution of Washington | AGNs with Intermediate-mass Black Holes: Testing the Black Hole-Bulge Paradigm, Part II | Abstract |
11151 | Gregory J. Herczeg, California Institute of Technology | Evaluating the Role of Photoevaporation of Protoplanetary Disk Dispersal | Abstract |
11156 | Kathy Rages, SETI Institute | Monitoring Active Atmospheres on Uranus and Neptune | Abstract |
11164 | David A. Weintraub, Vanderbilt University | Molecular Hydrogen Disks Around T Tauri Stars | Abstract |
11176 | Andrew S. Fruchter, Space Telescope Science Institute | Location and the Origin of Short Gamma-Ray Bursts | Abstract |
11178 | William M. Grundy, Lowell Observatory | Probing Solar System History with Orbits, Masses, and Colors of Transneptunian Binaries | Abstract |
11195 | Arjun Dey, National Optical Astronomy Observatories | Morphologies of the Most Extreme High-Redshift Mid-IR-luminous Galaxies II: The `Bump' Sources | Abstract |
11196 | Aaron S. Evans, State University of New York at Stony Brook | An Ultraviolet Survey of Luminous Infrared Galaxies in the Local Universe | Abstract |
11202 | Leon Koopmans, Kapteyn Astronomical Institute | The Structure of Early-type Galaxies: 0.1-100 Effective Radii | Abstract |
11210 | George Fritz Benedict, University of Texas at Austin | The Architecture of Exoplanetary Systems | Abstract |
11212 | Douglas R. Gies, Georgia State University Research Foundation | Filling the Period Gap for Massive Binaries | Abstract |
11213 | Gerard T. van Belle, California Institute of Technology | Distances to Eclipsing M Dwarf Binaries | Abstract |
11227 | Jifeng Liu, Smithsonian Institution Astrophysical Observatory | The orbital period for an ultraluminous X-ray source in NGC1313 | Abstract |
11233 | Giampaolo Piotto, Universita di Padova | Multiple Generations of Stars in Massive Galactic Globular Clusters | Abstract |
11235 | Jason A. Surace, California Institute of Technology | HST NICMOS Survey of the Nuclear Regions of Luminous Infrared Galaxies in the Local Universe | Abstract |
11237 | Lutz Wisotzki, Astrophysikalisches Institut Potsdam | The origin of the break in the AGN luminosity function | Abstract |
11518 | Michael Brown, California Institute of Technology | Mutual eclipses of a Kuiper belt-satellite system | Abstract |
GO 11107: Imaging of Local Lyman Break Galaxy Analogs: New Clues to Galaxy Formation in the Early Universe
GO 11117: The Search for Atmospheric Water in the Transiting Planet HD189733b
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HD 198733 is a 7th magnitude G5 dwarf that lies at a distance of ~20 parsecs from the Sun, in the direction of the constellation of Vulpecula. Like many other nearby solar-type stars, HD 189733 has an associated planetary system, including a hot Jupiter, a ~1.15 MJ gas giant with an orbital period of 2.12 days. Most significantly, that inner planet transits the central star, making HD 189733 the closest transiting system found so far. Transiting systems offer a potential gold-mine for extrasolar planetary studies, since not only is the orbital inclination well defined, but the diameter (and hence the average density) is directly measureable form the eclipse depth, while the atmospheric composition can be probed through line absorption or re-radiated thermal flux. The results from these measurments can be used to test, and improve, theoretical models of extrasolar planets. These observations are best done from space (indeed, the only successful atmospheric observations to date have been with HST and Spitzer). Previous observations with HST have been used to determine accurate radii for HD 189733b (e.g. GO 10923 ); the present program aims to search for evidence of water absorption by differencing NICMOS narrowband images taken before, during and after primary transit. |
GO 11156: Monitoring Active Atmospheres on Uranus and Neptune
GO 11233: Multiple Generations of Stars in Massive Galactic Globular Clusters
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Globular clusters are remnants of the first substantial burst of star formation in the Milky Way. With typical masses of a few x 105 solar masses, distributed among several x 106 stars, the standard picture holds that these are simple systems, where all the stars formed in a single starburst and, as a consequence, have the same age and metallicity. Until recently, the only known exception to this rule was the cluster Omega Centauri, which is significantly more massive than most clusters and has both double main sequence and a range of metallicities among the evolved stars. Omega Cen has been joined by at least one more cluster, NGC 2808, which shows evidence for three distinct branches to the main sequence. The origin of this feature is notknown, but it may be significant that NGC 2808 is also one of the more massive clusters, and might therefore be able to survive several burst of star formation (or, conversely, be the product of a multi proto-globular merger). The present program aims to use WFPC2 to obtain high-precision photometry of other massive globulars, such as NGC 1851, M80 and M13. |