Other
Scientific paper
Jan 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21733501g&link_type=abstract
American Astronomical Society, AAS Meeting #217, #335.01; Bulletin of the American Astronomical Society, Vol. 43, 2011
Other
Scientific paper
The Lockman Hole has the lowest HI and Galactic Cirrus foreground of any location in the sky, and is therefore an optimal target for deep X-ray and IR observations. Unlike most other extragalactic deep survey fields in which astronomers have invested extensive amounts of observing time across the electromagnetic spectrum, the Lockman Hole had until recently lacked the comprehensive HST imaging essential to characterize the distant galaxies responsible for emission detected in sensitive imaging at other wavelengths. For example, although total IR flux is central to understanding star formation rates, multiwavelength morphology encodes crucial information necessary to understand galaxy formation history and the physical processes that drive galaxy evolution.
We have remedied this shortfall with one of the last large programs to be executed with HST/WFPC2: a 125-orbit survey of the Lockman Hole in early 2009. This survey comprises 25 WFPC2 pointings, nested into a circular arrangement of radius ≈7.2 arcmin centered at α = 10h52m43.2s, δ = +57d28m53s. This particular region of the Lockman Hole was chosen because it includes the deepest imaging with XMM and Herschel, ultra-deep Spitzer 24um imaging, and a wealth of ground-based imaging and spectroscopy. Our observations at each pointing are 2 orbits with F606W (wide V-band) and 3 orbits with F814W (I-band), allowing us to reach V ≈ 27 and I ≈ 26.2 AB mag. These sensitivities enable measurement of rest-frame optical+UV morphologies for several thousand galaxies in the field at z<1. We present initial findings from this survey, including characteristics of our detected HST sources, and results from matching to deep imaging at other wavelengths.
Casertano Sefano
Grogin Norman Andrew
Lucas Ray A.
Somerville Rachel S.
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