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Program Number | Principal Investigator | Program Title | Links |
10782 | Imke de Pater, University of California - Berkeley | Quit winking: Jupiter opens its other eye | Abstract |
10792 | Matthias Dietrich, The Ohio State University Research Foundation | Quasars at Redshift z=6 and Early Star Formation History | Abstract |
10802 | Adam Riess, Space Telescope Science Institute | SHOES-Supernovae, HO, for the Equation of State of Dark energy | Abstract |
10807 | Matthias Stute, Jet Propulsion Laboratory | The knotty jet of He 2-90: An ideal laboratory for studying the formation and propagation of jets in dying stars | Abstract |
10836 | S. Stanford, University of California - Davis | The Red Sequence at 1.3 < z < 1.4 in Galaxy Clusters | Abstract |
10847 | Dean Hines, Space Science Institute | Coronagraphic Polarimetry of HST-Resolved Debris Disks | Abstract |
10862 | John Clarke, Boston University | Comprehensive Auroral Imaging of Jupiter and Saturn during the International Heliophysical Year | Abstract |
10918 | Wendy Freedman, Carnegie Institution of Washington | educing Systematic Errors on the Hubble Constant: Metallicity Calibration of the Cepheid PL Relation | Abstract |
10989 | George Benedict, University of Texas at Austin | Astrometric Masses of Extrasolar Planets and Brown Dwarfs | Abstract |
11080 | Daniela Calzetti, University of Massachusetts | Exploring the Scaling Laws of Star Formation | Abstract |
11083 | Pat Cote, Herzberg Institute | The Structure, Formation and Evolution of Galactic Cores and Nuclei | Abstract |
GO 10847: Coronagraphic Polarimetry of HST-Resolved Debris Disks
Artist's impression of one of the planets circling Epsion eridani (from Nova Celestia ) | The overwhelming majority of extrasolar planetary systems have been identified through radial velocity monitoring, and the detection of the reflex motion of the parent star as it orbits the common center of mass of the system. Just as radial velocities measure the stellar "wobble" introduced along the line of sight, so high precision astrometry can be used to measure motion in the plane of the sky. Combining these data gives the full three-dimensional motions of the system, and a direct measure of the mass of the planetary companion. The Fine Guidance Sensors on HST are the only system currently capable of making observations at the required sub-milliarcscond accuracy, and has already been used for astrometry of several systems, including the M dwarf Gl 876 and, most recently, Epsilon Eridani. The current GO program pursues observations of six planetary hosts, and FGS observations of HD 168443 and HD 38529, which has at least two planetary companions, are scheduled over the next week. |