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: http://www.stsci.edu/~inr/thisweek1/thisweek337.html
Дата изменения: Sun May 18 19:50:55 2014 Дата индексирования: Sun Apr 10 15:31:41 2016 Кодировка: Поисковые слова: aldebaran |
Program Number | Principal Investigator | Program Title | Links | ||||||||||||||||||||||||||||||||||||||||||||||||||||
10787 | Jane Charlton, The Pennsylvania State University | Modes of Star Formation and Nuclear Activity in an Early Universe Laboratory | Abstract | ||||||||||||||||||||||||||||||||||||||||||||||||||||
10798 | Leon Koopmans, Kapteyn Astronomical Institute | Dark Halos and Substructure from Arcs & Einstein Rings | Abstract | ||||||||||||||||||||||||||||||||||||||||||||||||||||
10815 | Thomas M. Brown, Space Telescope Science Institute | The Blue Hook Populations of Massive Globular Clusters | Abstract | ||||||||||||||||||||||||||||||||||||||||||||||||||||
10829 | Paul Martini, The Ohio State University | Secular Evolution at the End of the Hubble Sequence | Abstract | ||||||||||||||||||||||||||||||||||||||||||||||||||||
10889 | Roelof de Jong, Space Telescope Science Institute | The Nature of the Halos and Thick Disks of Spiral Galaxies | Abstract | ||||||||||||||||||||||||||||||||||||||||||||||||||||
10890 | Arjun Dey, National Optical Astronomy Observatories | Morphologies of the Most Extreme High-Redshift Mid-IR-Luminous Galaxies | Abstract | ||||||||||||||||||||||||||||||||||||||||||||||||||||
10907 | Scott F. Anderson, University of Washington | New Sightlines for the Study of Intergalactic Helium: A Dozen High-Confidence, UV-Bright Quasars from SDSS/GALEX | Abstract | ||||||||||||||||||||||||||||||||||||||||||||||||||||
10915 | Julianne Dalcanton, University of Washington | ACS Nearby Galaxy Survey | Abstract | ||||||||||||||||||||||||||||||||||||||||||||||||||||
11002 | Peter Eisenhardt, Jet Propulsion Laboratory | A Census of LIRGs in Clusters of Galaxies in the First Half of the Universe from the IRAC Shallow Survey | Abstract | ||||||||||||||||||||||||||||||||||||||||||||||||||||
11080 | Daniela Calzetti, University of Massachusetts | Exploring the Scaling Laws of Star Formation | Abstract | ||||||||||||||||||||||||||||||||||||||||||||||||||||
11082 | Christopher Conselice, Univ. of Nottingham | NICMOS Imaging of GOODS: Probing the Evolution of the Earliest Massive Galaxies, Galaxies Beyond Reionization, and the High Redshift Obscured Universe | Abstract | ||||||||||||||||||||||||||||||||||||||||||||||||||||
11084 | Dan Zucker, Institute of Astronomy, Cambridge | Probing the Least Luminous Galaxies in the Local Universe | Abstract | ||||||||||||||||||||||||||||||||||||||||||||||||||||
11103 | Harald Ebeling, University of Hawaii | A Snapshot Survey of The Most Massive Clusters of Galaxies | 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 | ||||||||||||||||||||||||||||||||||||||||||||||||||||
11128 | David Bradley Fisher, University of Texas at Austin | Time Scales Of Bulge Formation In Nearby Galaxies | Abstract | ||||||||||||||||||||||||||||||||||||||||||||||||||||
11130 | Luis Ho, Carnegie Institution of Washington | AGNs with Intermediate-mass Black Holes: Testing the Black Hole-Bulge Paradigm, Part II | Abstract | ||||||||||||||||||||||||||||||||||||||||||||||||||||
11142 | Lin Yan, California Institute of Technology | Revealing the Physical Nature of Infrared Luminous Galaxies at 0.3Abstract |
11157 |
Joseph H. Rhee, University of California - Los Angeles |
NICMOS Imaging Survey of Dusty Debris Around Nearby Stars Across the Stellar Mass Spectrum |
Abstract |
11169 |
Michael E. Brown, California Institute of Technology |
Collisions in the Kuiper belt |
Abstract |
11178 |
William M. Grundy, Lowell Observatory |
Probing Solar System History with Orbits, Masses, and Colors of Transneptunian Binaries |
Abstract |
11197 |
Peter Garnavich, University of Notre Dame |
Sweeping Away the Dust: Reliable Dark Energy with an Infrared Hubble Diagram |
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 |
11211 |
George Fritz Benedict, University of Texas at Austin |
An Astrometric Calibration of Population II Distance Indicators |
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 |
11289 |
Jean-Paul Kneib, Laboratoire d'Astronomie Spatiale |
SL2S: The Strong Lensing Legacy Survey |
Abstract |
11309 |
Jacob L. Bean, University of Texas at Austin |
Chemical Composition of an Exo-Neptune |
Abstract |
11312 |
Graham Smith, University of Birmingham |
The Local Cluster Substructure Survey (LoCuSS): Deep Strong Lensing Observations with WFPC2 |
Abstract |
11361 |
Keith Noll, Space Telescope Science Institute |
Hubble Heritage Observations of Mars at 2007 Opposition |
Abstract |
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GO 11210: The Architecture of Exoplanetary Systems
GO 11213: Distances to Eclipsing M Dwarf Binaries
GO 11312: The Local Cluster Substructure Survey (LoCuSS): Deep Strong Lensing Observations with WFPC2
GO 11361: Hubble Heritage Observations of Mars at 2007 Opposition
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Mars lies at an average distance of 228 million kilometres, or 1.52 AU, from the Sun, and has an orbital period of 687 days. As a result, it comes into opposition with Earth (i.e. the Sun, Earth and Mars lie along a straight line) once every 780 days, or approximately every 2 years. At that time, Mars makes its closest approach, but the actual distance varies significantly from opposition to opposition since the Martian orbit has significant eccentricity (e=0.093, as compared with e=0.007 for Earth). HST has been systematically observing Mars at opposition since February 1995, 15 months after WFPC2 was installed in Servicing Mission 1. At that time, the planet lay at a distance of 101 million kilometres from Earth and subtended a diameter less than 14 arcseconds. Succeeding oppositions were at increasingly smaller separations, until the opposition of August 28 2003, when Mars was only 55.8 million miles away with an angular diameter of 25.1 arcseconds, its closest approach since 57,617 BCE (but we won't have to wait quite so long - Mars passes even closer on August 28 2287). As in past years, HST will take a series of images of Mars as it approaches opposition, which, this year, will be at 19:47 UT (2:47 pm EST) on Christmas Eve. At that time, Mars will lie at a distance of 88.2 million kilometres with a diameter of 15.2 arcseconds. |