| Program Number | Principal Investigator | Program Title |
|---|---|---|
| 12063 | Sandra M. Faber, University of California - Santa Cruz | Galaxy Assembly and the Evolution of Structure over the First Third of Cosmic Time - I |
| 12468 | Keith S. Noll, NASA Goddard Space Flight Center | How Fast Did Neptune Migrate? A Search for Cold Red Resonant Binaries |
| 12577 | Armin Rest, Space Telescope Science Institute | Spectral Time Series of the Cas A Supernova |
| 12791 | Marc Postman, Space Telescope Science Institute | Through a Lens, Darkly - New Constraints on the Fundamental Components of the Cosmos |
| 12870 | Boris T. Gaensicke, The University of Warwick | The mass and temperature distribution of accreting white dwarfs |
| 12872 | Nicola Da Rio, University of Florida | Characterizing the mass accretion rates in young low-mass stars at low metallicity |
| 12879 | Adam Riess, The Johns Hopkins University | A 1% Measurement of the Distance Scale with Perpendicular Spatial Scanning |
| 12880 | Adam Riess, The Johns Hopkins University | The Hubble Constant: Completing HST's Legacy with WFC3 |
| 12884 | Harald Ebeling, University of Hawaii | A Snapshot Survey of The Most Massive Clusters of Galaxies |
| 12893 | Ronald L Gilliland, The Pennsylvania State University | Study of Small and Cool Kepler Planet Candidates with High Resolution Imaging |
| 12903 | Luis C. Ho, Carnegie Institution of Washington | The Evolutionary Link Between Type 2 and Type 1 Quasars |
| 12908 | Paul Goudfrooij, Space Telescope Science Institute | What Causes Extended Main Sequence Turn-offs in Intermediate-Age Star Clusters? |
| 12939 | Elena Sabbi, Space Telescope Science Institute - ESA | Hubble Tarantula Treasury Project {HTTP: unraveling Tarantula's web} |
| 12964 | Marina Rejkuba, European Southern Observatory - Germany | Probing the outermost halo in a giant galaxy: is it metal-poor and where does it end? |
| 12969 | Peter Garnavich, University of Notre Dame | Global Properties Are Not Enough: Probing the Local Environments of Type Ia Supernovae |
| 12970 | Michael C. Cushing, University of Toledo | Completing the Census of Ultracool Brown Dwarfs in the Solar Neighborhood using HST/WFC3 |
| 12976 | Ian U. Roederer, Carnegie Institution of Washington | The Most Complete Template for r-process Nucleosynthesis beyond the Solar System |
| 12977 | Ivana Damjanov, Smithsonian Institution Astrophysical Observatory | Local Turbulent Disks: analogs of high-redshift vigorously star-forming disks and laboratories for galaxy assembly? |
| 12978 | Daniel E. Welty, University of Chicago | Properties of Diffuse Molecular Gas in the Magellanic Clouds |
| 12982 | Nicolas Lehner, University of Notre Dame | Are the Milky Way's High Velocity Clouds Fuel for Star Formation or for the Galactic Corona? |
| 12991 | Veronica Strazzullo, CEA/DSM/DAPNIA/Service d'Astrophysique | Red galaxies in CL J1449+0856 at z=2.07: the red sequence in the most distant galaxy cluster |
| 12999 | Ryan Foley, Smithsonian Institution Astrophysical Observatory | Are the Progenitors of SN 2002cx-like Objects Massive Stars or White Dwarfs? |
| 13000 | Sungryong Hong, National Optical Astronomy Observatory, AURA | Impact of Environments on Lyman alpha Emitting Galaxies at High Redshift {z ~ 2.7} |
| 13009 | Guido De Marchi, European Space Agency - ESTEC | Studying pre-main sequence stars across the metallicity ladder |
| 13023 | Marco Chiaberge, Space Telescope Science Institute - ESA | Universe in transition: powerful activity in the Bright Ages |
| 13025 | Andrew J. Levan, The University of Warwick | Unveiling the progenitors of the most luminous supernovae |
| 13031 | William M. Grundy, Lowell Observatory | Testing Collisional Grinding in the Kuiper Belt |
| 13051 | Jonathan D. Nichols, University of Leicester | Long term observations of Saturn's northern auroras |
| 13057 | Kailash C. Sahu, Space Telescope Science Institute | Detecting and Measuring the Masses of Isolated Black Holes and Neutron Stars through Astrometric Microlensing |
| 13061 | John A. Biretta, Space Telescope Science Institute | High-Precision Proper Motions in the M87 Jet |
| 13230 | Andrew J. Levan, The University of Warwick | A supernova in the brightest gamma-ray burst |
GO 12063: Galaxy Assembly and the Evolution of Structure over the First Third of Cosmic Time
Part of the GOODS/Chandra Deep Field South field, as imaged by HST |
CANDELS is one of three Multi-Cycle Treasury Program, whose observations will be executed over the next three HST Cycles. It builds on past investment of both space- and ground-based observational resources. In particular, it includes coverage of the two fields of the Great Observatory Origins Deep Survey (GOODS), centred on the northern Hubble Deep Field (HDF) in Ursa Major and the Chandra Deep Field-South in Fornax. In addition to deep HST data at optical and near-infrared wavelengths, the fields have been covered at X-ray wavelengths by Chandra (obviously) and XMM-Newton; at mid-infrared wavelengths with Spitzer; and ground-based imaging and spectroscopy using numerous telescopes, including the Kecks, Surbaru and the ESO VLT. This represents an accumulation of almost 1,000 orbits of HST time, and comparable scale allocations on Chandra, Spitzer and ground-based facilities. The CANDELS program is capitalising on this large investment, with new observations with WFC3 and ACS on both GOODS fields, and on three other fields within the COSMOS, EGS and UDS survey areas (see this link for more details). The prime aims of the program are twofold: reconstructing the history of galaxy formation, star formation and nuclear galactic activity at redshifts between z=8 and z=1.5; and searching for high-redshift supernovae to measure their properties at redshifts between z~1 and z~2. The program incorporates a tiered set of observations that complement, in areal coverage and depth, the deep UDF observations, while the timing of individual observations will be set to permit detection of high redshift SNe candidates for subsequent follow-up. The program has been executing since Cycle 18 and will be completed in this cycle. |
GO 12577: Spectral Time Series of the Cas A Supernova
Chandra X-ray imaging of the Cas A supernova remnant |
Cassiopeia A is one of the brightest celestial radio sources at high frequencies (>1 GHz) and the compact remnant of a relatively recent supernova explosion. With a current diameter of approximately 3 pc, the supernova explosion likely occured some 300-400 years ago, but seems to have largely escaped attention in contemporaneous accounts. The ongoing hypothesis is that the progenitor was a high mass star that, following a series of mass loss episodes, had succeeded in entombing itself in a dusty cocoon of material that absorbed most of the optical light emitted during the explosion. Tehre is a suggestion that John Flamsteed may haeve detected the star in 1680, since his catalogue includes a 6th magnitude star, 3 Cassiopeia, that has not been seen since then and whose position lies close to the radio source. The remnant has been studied extensively since its discovery, including both ground-based optical/IR/radio observations and space-based imaging with Chandra, Spitzer and HST. The present program aims to probe the nature of the supernova explosion itself through spectroscopic observations of bright filaments that are likely to be dusty regions that were illuminated by supernova explosion. those filaments lie at a sufficient spatial separation from the event itself that the light travel time is such that the reflected light from the supernova event is only now reaching Earth; that is, we can use these light echos to probe the spectroscopic signatures of the Cas A supernova, and perhaps finally confirm its nature. |
GO 12939: Hubble Tarantula Treasury Project, HTTP: unraveling Tarantula's web
Hubble image of the central regions, near NGC 2074, of 30 Doradus, the Tarantula Nebula |
The 30 Doradus region, also known as the Tarantula Nebula, is among the most active star-forming regions in the Local Group.
Lying within the Large Magellanic Cloud, the star-forming region has a diameter of 200 pc, a total mass around 106
solar masses and is sufficiently bright to be easily detectable to the naked eye (hence the stellar designation). The stelalr
complex includes a number of individual star clusters that are generally agreed to have ages from a few to ~20 million years.
As such, this region is noe of the most fruitful for studying both the detailed properties of
high mass stars and their overall mass distribution. The present program will obtain a mosaiced image of the full
200x200 parsec star forming region. The aim is to use deep, multi-wavelength
imaging with ACS and WFC3 to push observations into the sub-solar mass regime,
potentially reaching stars with masses as low as 0.4-0.5 M |
GO 13230: A supernova in the brightest gamma-ray burst
HST images of GRB-11121, linked with SN2001ke |
Gamma ray bursts are events that tap extraordinary energies (1045 to 1047 joules) in remarkably short periods of time. Several thousands bursts have been detected since their discovery in the late 1960s (by military satellites - there were some initial worries that they might be of sinister intent). Analyses of their properties suggest that GRBs can be divided into two basic caregories: short, hard bursts, that are likely due to component mergers in neutron star or black hole binaries; and long, soft bursts, which originate in the collapse of very massive stars. Over the last few years, it has become clear that a subset of GRBs are associated with a particular class of supernova, type IC SNe, sometimes termed hypernovae. The first clear example of this type of object was probably GRB 030329 (identified in 2003); an optical counterpart to the GRB was identified by ground-based telescopes within ~90 minutes, and monitoring over the next few days by the ESO Very Large Telescope showed the gradual energence of a supernovae spectrum, as the GRB afterglow faded. Subsequently, a number of other examples have been discovered, although all have fairly low energies for GRBs. A lingering question is whether the supernova mechanism that is now generally accepted for those sources is a reasonable explanation for much higher energy events. the present program aims to tackle that question through HST observations of GRB 130427A, the brightest burst so far observed by Swift. The host galaxy lies at a relatively low redshift, z=0.34, allowing clear separation of the supernova and the afterglow through ACS and WFC3 observations, and a characterisation of the underlying stellar population. |