| Program Number | Principal Investigator | Program Title |
|---|---|---|
| 13504 | Jennifer Lotz, Space Telescope Science Institute | HST Frontier Fields - Observations of MACSJ1149.5+2223 |
| 13642 | Nathalie Degenaar, University of Cambridge | The evolutionary link between low-mass X-ray binaries and millisecond radio pulsars |
| 13647 | Ryan Foley, University of Illinois at Urbana - Champaign | Testing the Standardizability of Type Ia Supernovae with the Cepheid Distance of a Twin Supernova |
| 13652 | Boris T. Gaensicke, The University of Warwick | The frequency and chemical composition of rocky planetary debris around young white dwarfs: Plugging the last gaps |
| 13667 | Marc W. Buie, Southwest Research Institute | Observations of the Pluto System During the New Horizons Encounter Epoch |
| 13668 | Marc W. Buie, Southwest Research Institute | Deep Search for Small Satellites of Eris and Makemake |
| 13671 | Harald Ebeling, University of Hawaii | Beyond MACS: A Snapshot Survey of the Most Massive Clusters of Galaxies at z>0.5 |
| 13677 | Saul Perlmutter, University of California - Berkeley | See Change: Testing time-varying dark energy with z>1 supernovae and their massive cluster hosts |
| 13689 | Aleksandar M. Diamond-Stanic, University of Wisconsin - Madison | How Compact is the Stellar Mass in Eddington-Limited Starbursts? |
| 13690 | Tanio Diaz-Santos, Universidad Diego Portales | Tracking the Obscured Star Formation Along the Complete Evolutionary Merger Sequence of LIRGs |
| 13691 | Wendy L. Freedman, University of Chicago | CHP-II: The Carnegie Hubble Program to Measure Ho to 3% Using Population II |
| 13694 | Amanda R. Hendrix, Planetary Science Institute | UV spectra of the icy Saturnian satellites: Understanding exogenic processes and NH3 in the system |
| 13695 | Benne W. Holwerda, Sterrewacht Leiden | STarlight Absorption Reduction through a Survey of Multiple Occulting Galaxies (STARSMOG) |
| 13700 | Carl Melis, University of California - San Diego | Confirming the most water-rich extrasolar rocky body |
| 13704 | Steven G. Parsons, Universidad de Valparaiso | Testing the single degenerate channel for supernova Ia |
| 13728 | Steven Kraemer, Catholic University of America | Do QSO2s have Narrow Line Region Outflows? Implications for quasar-mode feedback |
| 13741 | Thaisa Storchi-Bergmann, Universidade Federal do Rio Grande do Sul | Constraining the structure of the Narrow-Line Region of nearby QSO2s |
| 13750 | John M. Cannon, Macalester College | Fundamental Parameters of the SHIELD II Galaxies |
| 13760 | Derck L. Massa, Space Science Institute | Filling the gap --near UV, optical and near IR extinction |
| 13767 | Michele Trenti, University of Melbourne | Bright Galaxies at Hubble's Detection Frontier: The redshift z~9-10 BoRG pure-parallel survey |
| 13777 | Michael D. Gregg, University of California - Davis | Morphological Transformation in the Coma Cluster |
| 13784 | Robert M. Quimby, San Diego State University | The First UV Spectra of a Hydrogen-Rich Superluminous Supernova |
| 13793 | Rebecca A A Bowler, Royal Observatory Edinburgh | Unveiling the merger fraction, sizes and morphologies of the brightest z ~ 7 galaxies |
| 13804 | Kristen McQuinn, University of Minnesota - Twin Cities | Important Nearby Galaxies without Accurate Distances |
| 13821 | Andrew C. Fabian, University of Cambridge | H-alpha Filaments and Feedback in NGC4696 at the centre of the Centaurus cluster |
| 13826 | Massimo Robberto, Space Telescope Science Institute | The Orion Nebula Cluster as a Paradigm of Star Formation |
| 13833 | Nicolas Tejos, University of California - Santa Cruz | Characterizing the cool and warm-hot intergalactic medium in clusters at z < 0.4 |
| 14052 | Michael C. Cushing, University of Toledo | A Spitzer/HST Case Study of Weather on a Y Dwarf |
GO 13642: The evolutionary link between low-mass X-ray binaries and millisecond radio pulsars
Artist's impression of accretion within a low-mass X-ray binary system |
Low-mass X-ray binaries are generally believed to be binary systems where a compact, high-mass component, either a black hole or a neutron star, is accreting mass from a lower-mass component that is overflowing its Roche lobe. These systems are extremely luminous at short wavelengths, and are readily detected at X-ray wavelengths in nearby galaxies. Pulsars are also known to be associated with neutron stars, with the radio pulses generated as beamed radiation sweeps across our line of sight. Millisecond radio pulsars are generally believed to be associated with neutron stars in binary systems, with the rapid pulsar rotation tied to the transfer of orbital angular moment. The present program targets one such object, XSS J12270-4859, which recently transitioned states from a radio-quiet LMXB system to a millisecond pulsar.The present program aims to use the WFC3 UVIS camera and the UV-sensitive solar-blind channel on ACS (ACS/SBC) to search for UV radiation from the accertion disk expected to be associated with this object.The observations will be made at near-UV and far-UV wavelengths. |
GO 13694: UV spectra of the icy Saturnian satellites: Understanding exogenic processes and NH3 in the system
Cassini image of Saturn's satellite, Mimas |
The Saturnian planetary system includes seven major satellites with diameters exceeding 300 kilometres,together with 50 or more smaller bodies. The largest satellite, Titan, is bigger than Mercury; the remaining satellites have diameters between ~400 km (Mimas) and ~1,500 km (Iapetus and Rhea). These satellites have been studied extensively with ground- and space-based observatories and, since 2004, through in situ measurements made by the Cassini mission. Those observations have provided clues to the surface composition, specifically the likely presence of ices. However, current estimates remain inconclusive due to relatively poor spectral coverage at wavelengths between 1900 and 3500 Angstroms. the present program aims to remedy this defect by using STIS to obtain spectra covering that wavelength raneg for Mimas, Dione and Rhea. Ammonia is suspected as being a key contributor to the icy surfaces; if so, characteristic absorption features should be evident near 2000 Angstroms. |
GO 13767: Bright Galaxies at Hubble's Detection Frontier: The redshift z~9-10 BoRG pure-parallel survey
 The ACS optical/far-red image of the Hubble Ultra Deep Field |
Galaxy evolution in the early Universe is a discipline of astronomy that has been transformed by observations with the Hubble Space Telescope. The original Hubble Deep Field, the product of 10 days observation in December 1995 of a single pointing of Wide Field Planetary Camera 2, demonstrated conclusively that galaxy formation was a far from passive process. The images revealed numerous blue disturbed and irregular systems, characteristic of star formation in galaxy collisions and mergers. Building on this initial progam, the Hubble Deep Field South (HDFS) provided matching data for a second southern field, allowing a first assessment of likely effects due to field to field cosmic variance, and the Hubble Ultra-Deep Field (UDF) probed to even fainter magitude with the Advanced Camera for Surveys (ACS). The highest redshift objects found in the UDF have redshifts approaching z~7. Pushing to larger distances, and greater ages, demands observatons at near-infrared wavelengths, as the characteristics signatures of star formation are driven further redward in the spectrum. Wide Field Camera 3, installed in Servicing Mission 4, is well suited to these observations, and a number of programs are in place in Cycle 17 that address these issues. Indeed, WFC3 is employed in pure parallel mode by several programs. These take advantage of other science programs, usually with COS, that involve 2-5 orbit pointings on sources at high galactic latitude. The WFC3 pointing is unplanned, since it depends on the orientation adopted for the prime observations, but 2-5 orbits of IR imaging can reach galaxies at redshifts exceeding z=7 (potentially even z~8) in high latitude fields. The present program builds on similar programs in Cycles 17 and 19, and aims to detect the brightest galaxies at z~9, within 600 Myrs of the Big Bang. |
GO 13826: The Orion Nebula Cluster as a Paradigm of Star Formation
Combined Hubble and Spitzer images of the Orion Nebula Cluster ). |
The Orion association is the largest nearby star-forming complex, providing a key laboratory for unlocking the secrets of star formation.The Orion Nebula Cluster (ONC) lies within that complex, associated with the Orion A molecular cloud. The ONC includes several thousand members, ranging in mass from the 15-20 solar mass O-type stars in the Trapezium to brown dwarfs with sub-stellar masses. As the nearest massive star-formng region, Orion has been observed intensively from both ground and space, including surveys by NASA's Great Observatories, Chandra, Spitzer and Hubble. Indeed, the ONC was the target of a Hubble Treasury program in Cycle 13 (GO 10246), including observations with ACS, NICMOS and WFPC2 carried out in 2004. The region has also been surveyed at near-infrared and mid-infrared wavelengths, notably by Spitzer, and those observations have revealed extensive numbers of embedded sources, young stellar object within the surrounding molecular clodus. The present program builds on that solid foundation, adding deep, high spatial-resolution imaging of the ONC with the WFC3 IR camera. The aim is to extend coverage to the lowest mass members of the ONC, pushing to brown dwarfs with masses as low as a few times that of Jupiter. The observations include both wide-band data and imaging in narrower bands centred on the near-IR water features that are known to be present in these cool, low-mass objects. |