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: http://www.stsci.edu/~inr/thisweek1/2010/thisweek193.html
Дата изменения: Wed Jul 21 22:28:09 2010 Дата индексирования: Mon Sep 13 07:19:37 2010 Кодировка: Поисковые слова: moon |
| Program Number | Principal Investigator | Program Title |
|---|---|---|
| 11142 | Lin Yan, California Institute of Technology | Revealing the Physical Nature of Infrared Luminous Galaxies at 0.3 |
| 11360 | Robert W. O'Connell, The University of Virginia | Star Formation in Nearby Galaxies |
| 11527 | James C. Green, University of Colorado at Boulder | COS-GTO: An absorption study of galactic intermediate velocity clouds using hot stars in globular clusters |
| 11556 | Marc W. Buie, Southwest Research Institute | Investigations of the Pluto System |
| 11565 | Sebastien Lepine, American Museum of Natural History | A search for astrometric companions to very low-mass, Population II stars |
| 11567 | Charles R. Proffitt, Computer Sciences Corporation | Boron Abundances in Rapidly Rotating Early-B Stars. |
| 11576 | Jean-Michel Desert, Harvard University | Physical parameters of the upper atmosphere of the extrasolar planet HD209458b |
| 11577 | Brad C. Whitmore, Space Telescope Science Institute | Opening New Windows on the Antennae with WFC3 |
| 11592 | Nicolas Lehner, University of Notre Dame | Testing the Origin{s} of the Highly Ionized High-Velocity Clouds: A Survey of Galactic Halo Stars at z>3 kpc |
| 11594 | John M. O'Meara, Saint Michaels College | A WFC3 Grism Survey for Lyman limit absorption at z=2 |
| 11595 | John M. O'Meara, Saint Michaels College | Turning out the Light: A WFC3 Program to Image z>2 Damped Lyman Alpha Systems |
| 11598 | Jason Tumlinson, Space Telescope Science Institute | How Galaxies Acquire their Gas: A Map of Multiphase Accretion and Feedback in Gaseous Galaxy Halos |
| 11599 | Richard A. Wade, The Pennsylvania State University | Distances of Planetary Nebulae from SNAPshots of Resolved Companions |
| 11605 | Travis Stuart Barman, Lowell Observatory | Obtaining the Missing Links in the Test of Very Low Mass Evolutionary Models with HST |
| 11613 | Roelof S. de Jong, Astrophysikalisches Institut Potsdam | GHOSTS: Stellar Outskirts of Massive Spiral Galaxies |
| 11630 | Kathy Rages, SETI Institute | Monitoring Active Atmospheres on Uranus and Neptune |
| 11631 | Iain Neill Reid, Space Telescope Science Institute | Binary brown dwarfs and the L/T transition |
| 11644 | Michael E Brown, California Institute of Technology | A dynamical-compositional survey of the Kuiper belt: a new window into the formation of the outer solar system |
| 11658 | David A. Turnshek, University of Pittsburgh | Probing the Outer Regions of M31 with QSO Absorption Lines |
| 11661 | Misty C. Bentz, University of California - Irvine | The Black Hole Mass - Bulge Luminosity Relationship for the Nearest Reverberation-Mapped AGNs |
| 11663 | Mark Brodwin, Smithsonian Institution Astrophysical Observatory | Formation and Evolution of Massive Galaxies in the Richest Environments at 1.5 < z < 2.0 |
| 11666 | Adam J. Burgasser, University of California - San Diego | Chilly Pairs: A Search for the Latest-type Brown Dwarf Binaries and the Prototype Y Dwarf |
| 11687 | Thomas R. Ayres, University of Colorado at Boulder | SNAPing Coronal Iron |
| 11696 | Matthew A. Malkan, University of California - Los Angeles | Infrared Survey of Star Formation Across Cosmic Time |
| 11697 | Slawomir Stanislaw Piatek, New Jersey Institute of Technology | Proper Motion Survey of Classical and SDSS Local Group Dwarf Galaxies |
| 11699 | Thomas Rauch, Universitat Tubingen, Institut fur Astronomie & Astrophysik | On the evolutionary status of extremely hot helium stars - are the O{He} stars successors of the R CrB stars? |
| 11712 | John P. Blakeslee, Dominion Astrophysical Observatory | Calibration of Surface Brightness Fluctuations for WFC3/IR |
| 11721 | Richard S. Ellis, California Institute of Technology | Verifying the Utility of Type Ia Supernovae as Cosmological Probes: Evolution and Dispersion in the Ultraviolet Spectra |
| 11728 | Timothy M. Heckman, The Johns Hopkins University | The Impact of Starbursts on the Gaseous Halos of Galaxies |
| 11838 | Herman L. Marshall, Massachusetts Institute of Technology | Completing a Flux-limited Survey for X-ray Emission from Radio Jets |
| 12018 | Andrea H. Prestwich, Smithsonian Institution Astrophysical Observatory | Ultra-Luminous x-Ray Sources in the Most Metal-Poor Galaxies |
| 12019 | Christy A. Tremonti, University of Wisconsin - Madison | After the Fall: Fading AGN in Post-starburst Galaxies |
| 12057 | Julianne Dalcanton, University of Washington | A Panchromatic Hubble Andromeda Treasury - I |
GO 11556: Investigations of the Pluto System
Hubble Space Telescope image of Pluto, Charon and the two new moons, Nix & Hydra |
Pluto, one of the largest members of the Kuiper Belt and, until recently (still, for some), the outermost planet in the solar system, has been in the news over the last year or two. Besides the extended "planet"/"dwarf planet" debate, Pluto is the primary target of the New Horizons Mission, and Hubble observations in 2005 led to the discovery of two small moons. Together with Charon, itself only discovered in 1978, these additions make Pluto a 4-body system. Christened Nix and Hydra, the two new moons are 5,000 fainter than Pluto itself, implying diameters as small as ~30-50 km if the surface composition is similar to Pluto itself. The present program aims to better characterise these bodies through multicolour observations with WFC3. The observations are phased with a cadence that samples the different orbital periods: 6.4 days for Pluto/Charon; 24.9 days for Nix/Pluto; and 38 days for Hydra/Pluto. The goal is to identify systematic photometric variations that might probe the rotation period, testing whether these moons are in synchronous rotation with Pluto itself. |
GO 11594: A WFC3 Grism Survey for Lyman limit absorption at z=2
HRC grism image of SN 1987A, as displayed in the Hubble Legacy Archive
|
Grisms are optical components with finely ruled gratings that canbe introduced into the beam of an imaging camera to produce low-resolution spectra of objects within the field of view. Wide Field Camera 3 on HST has three such components: an ultraviolet grism, G280, providing spectroscopy from ~2100 to 3900 Angstroms; and two grisms, G102 and G141, for use at near-infrared wavelengths. The present program aims to use the UV grism to search for galaxies at redshifts in the range 1.8 < z < 2.5. The observations target 64 quasars, drawn from the Sloan Digital Sky Survey, that have absorption features that are characteristic of that redshift range. Those features are likely due to foreground galaxies, whose extended gaseous halos absorb light from the QSO. The grism data will used to search for sources with emission lines that indciate that they are at the appropriate redshift. |
GO 11599: Distances of Planetary Nebulae from SNAPshots of Resolved Companions
HST image of the Eskimo planetary nebula, NGC 2392
|
Planetary nebulae are the spectacular results of the penultiumate evoutionary phase of intermediate-mass stars. Towards the conclusion of the second, or asymptotic, giant branch, ~1 to ~7 solar mass stars have achieved radii exceeding 100 RSun and their extensive envelopes are subject to long-period, opacity-driven pulsations and substantial mass loss. AGB evolution terminates with the ejection of the stellar envelope, revealing the bare core, with an initial surface temperature approaching 100,000K. The core cools to become a white dwarf but, during the initial phase, its luminosity is sufficient to excite gases in the expanding envelope, producing a planetary nebula. These objects are extremely spectacular, but also, in Galactic terms, rare. As a result, we only know reliable distances to a handful of such systems. The present program aims to tackle this issue through observations of planetary nebulae with known or suspected lower-mass companions. Once confirmed as binaries, distances can be estimated using the companions, which still reside on the main sequence. |
GO 11697: Proper Motion Survey of Classical and SDSS Local Group Dwarf Galaxies
The low-mass dwarf galaxy, Leo II
|
The Milky Way, m31 and M33 are the three largest galaxies in the Local Group. The system, however, includes more than 25 other members, the majority being dwarf spheroidal galaxies that are satellites of either M31 or the Milky Way. Those galaxies have old, evolved stellar populations, and even the most prominent have masses that are less than a few x 107 MSun, or 10-4 that of the Milky Way. All of these galaxies are moving in the potential set by the overall Local Group system, but dominated by M31 and the Milky Way. Determining full space motions for the dwarfs therefore provide a means of constraining that potential. Even thought the galaxies, and their brightest stellar constituents, are faint, measuring radial velocity is a relatively straightforward procedure. Deriving tangential motions is not, since the typical proper motions of these systems are a few mas/year at best. The present proposal aims to capitalise on the exceptional resolution and high stability of HST to address this issue. WFC3 will target 7 dwarf galaxies, imaging fields that are centred on a background QSO. That QSO serves as a reference point for measurement of the transverse motion of stars in the foreground dwarf galaxy. |