Astronomy and Astrophysics – Astronomy
Scientific paper
Jan 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21733518c&link_type=abstract
American Astronomical Society, AAS Meeting #217, #335.18; Bulletin of the American Astronomical Society, Vol. 43, 2011
Astronomy and Astrophysics
Astronomy
Scientific paper
As part of the WFC3 Early Release Science observations, a portion of the GOODS-S field was observed with both the UVIS and IR Channels of the WFC3. The full data set of 100 orbits covers 50 square arcminutes on the sky at 0.09 arcseconds per pixel with ten broad bands covering 0.2-1.7 microns. The field was observed in F225W, F275W, and F336W to 10 sigma point source flux limits of 26.0, 26.1, and 25.7 AB-mag, respectively. In this poster, we will emphasize the results enabled by these UV observations of faint galaxies. We demonstrate that these UV observations are extremely useful, even for galaxies of intermediate redshifts (z<1), in terms of SED fittings, photometric redshifts, dropout galaxies, AGN, etc. In particular, optical and near-IR studies only measure the rest-frame UV properties of the highest redshift galaxies, and for comparison these UV observations are needed to properly study galaxy evolution near the peak of the global star formation rate density. In fact, deeper UV observations, below the atmospheric cutoff, and with space-based resolution, are need to properly study galaxies at the faint-end of the luminosity function at z 1.
This paper is based on Early Release Science observations made by the WFC3 Scientific Oversight Committee. We are grateful to the Director of the Space Telescope Science Institute for awarding Director's Discretionary time for this program. Support for program #11359 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555.
Cohen Seth H.
Hathi Nimish P.
Koekemoer Anton M.
McCarthy Patrick. J.
O'Connell Robert West
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