Change dither pattern to recommended default.
Merge all relevant observations of each field in one visit.
Replace GRB050319 in the original target list with GRB060607.
----- Submission 1 (Mon May 15 00:14:28 GMT 2006) -----
Phase II Proposal 10817 (graasp2) successfully submitted.
----- Submission 2 (Tue May 16 17:08:45 GMT 2006) -----
Phase II Proposal 10817 (graasp2) successfully submitted.
----- Submission 3 (Sun Jul 16 02:18:42 GMT 2006) -----
Phase II Proposal 10817 (graasp2) successfully submitted.
Error connecting to STScI submission server:
java.rmi.UnknownHostException: Unknown host: clotho.stsci.edu; nested exception is:
java.net.UnknownHostException: clotho.stsci.edu
----- Submission 4 (Mon Jul 17 15:31:26 GMT 2006) -----
Phase II Proposal 10817 (graasp2) successfully submitted.
----- Submission 5 (Tue Jul 18 17:12:13 GMT 2006) -----
Assigned ID: 234
----- Submission 1 (Fri Jan 27 15:22:26 GMT 2006) -----
Unveiling Starburst Morphology of Distant Damped Ly-alpha Galaxies Hosting Gamma-Ray Bursts
The damped Lya systems (DLAs), `clouds' with high columns of neutral hydrogen, dominate the neutral gas mass at z>2 and are believed to be the building blocks of galaxies like the Milky Way. At present, high resolution spectroscopy of the DLAs provide the only detailed study of the ISM of young galaxies during early epochs. Yet by the very nature of their discovery - along bright quasar sightlines - direct imaging of the stellar counterparts presents a major obstacle. The use of gamma-ray bursts (GRBs) presents a novel new alternative: GRB afterglows are temporarily as bright as quasars, allowing for high-quality spectroscopy to identify and study new DLAs out to redshifts comparable to those probed by quasars. Afterglows then disappear after a few weeks, affording a direct and unimpeded view of the faint DLAs free from a glaring background source. Through an extensive ground-based program in 2005, we have now obtained early-time high-resolution echelle spectra of several NASA/Swift GRB afterglows. These data reveal that nearly all GRB host galaxies produce a DLA feature. Furthermore, the associated metal absorption lines indicate an ISM environment around the GRB progenitors --- extremely dense gas and warm temperature --- that has never been seen beyond the local universe. We request ACS late-time imaging of fields surrounding nine GRBs, all of which exhibit a strong DLA signature or strong metal absorption lines that indicate a DLA at the redshift of the host. In concert with our afterglow absorption line studies and stellar properties of both the GRB host galaxies and galaxies that give rise to strong intervening absorbers, these proposed observations will provide an unprecedented glimpse into the nature of DLAs beyong redshift of unity. As a complete sample, this study will provide robust measurements of the morphology and luminosity of DLA galaxies in a manner inaccessible to QSO lines of sight.
We propose to obtain deep optical images of the fields surrounding nine Swift-GRBs discovered at z_GRB>2. The
GRBs are selected to exhibit either a strong DLA signature or metal absorption features that are indicative of a DLA in their afterglow spectra. We note that by the time when Cycle15 starts these bursts will be more than 10 months old and that the optical afterglows will not interfere the imaging search of the DLA galaxies.
The imaging program is optimized to reach the required depths for finding the galaxies that give rise to the classical-DLA and host-DLA at different redshift range. Our assessments for the required imaging depths are guided by prior knowledge of z>2 DLA galaxies and expectations from simple spectral modeling of the observed optical photometry. The majority of the known DLA galaxies have AB(F160W)~25.6 at z~3 (Moller et al. 2002). To reach the same depth in the NICMOS/F(160W) band would require more than 10 orbits to achieve our goal.
We compare predicted redshift evolution of observed AB(F814W) - AB(F160W) color for galaxies of different spectral type. Starforming galaxies exhibit observed optical and near-infrared color F814W-F160W > 0.8 at 2<=z<=3, suggesting that these DLA galaxies would be no brighter than AB(F814W)= 26.4 at z=3. Given that these previously known DLA galaxies are likely among the brightest, we target our imaging goal at a 5-sigma limit of AB(F814W) = 27.5 for the GRB fields. These brightness limits will allow us to uncover galaxies as faint as 0.1 L_* at z=3.
The exposure times necessary to reach the goals are estimated according to previous experiences (Warren et al. 2001) and the Exposure Time Calculator at the ACS instrument webpage. For the z_DLA ~ 2.5 fields, we find that 12,000 seconds would be required for ACS/WFC to reach AB(F814W) = 27.5 at the 5-sigma level of significance over a 0.5-arcsecond diameter aperture. We therefore request five orbits of imaging in ACS/WFC with the F814W filter to
complete one field, and 45 orbits total to complete the proposed imaging program.
For each visit with the ACS, a four-point ``expanded'' ACS-WFC-DITHER-BOX pattern will be used. With linearly spaced
sampling, it will help cosmic-ray removal and improve the final point spread function in the stacked images
ISM IN EXTERNAL GALAXIES
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GAMMA RAY EMITTER
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UNIDENTIFIED
GAMMA RAY EMITTER
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z_GRB = 2.17
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GAMMA RAY EMITTER
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ACS/WFC
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ACS/WFC
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