Astronomy and Astrophysics – Astronomy
Scientific paper
May 2005
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aas...206.1005w&link_type=abstract
American Astronomical Society Meeting 206, #10.05; Bulletin of the American Astronomical Society, Vol. 37, p.444
Astronomy and Astrophysics
Astronomy
Scientific paper
We combine data from the extremely deep HST U (F300W) image obtained using WFPC2 as part of the parallel observations of the Hubble Ultra Deep Field campaign, with BVi images from the HST/GOODS survey to identify a sample of Lyman break galaxies in the redshift range 2.0 ≤ z ≤ 3.5.
We use recent stellar population synthesis models with a wide variety of ages, metallicities, dust contents and redshifts to model the colors of galaxies in our combination of WFPC2/ACS filters. We model the H I\ cosmic opacity as a function of redshift including scattering in resonant lines of the Lyman series and Lyman continuum absorption. Using these models, we derive the color selection criteria that provide a clean selection of relatively unobscured, star forming galaxies in this redshift range.
The 10σ limiting magnitude measured over 0.2 arcsec2 is 27.5 magnitudes in the WFPC2/F300W image, about 0.5 magnitudes deeper than the F300W image in the HDF-N and 0.7 magnitudes deeper than that in the HDF-S. This extra depth relative to the HDFs allows us to probe the luminosity function about 0.5 magnitudes deeper than the depth accessible with the HDF data. This enables a better measurement of the luminosity function and star formation rate. Our sample of star-forming galaxies with 2.0 ≤ z ≤ 3.5 includes about 120 objects. We present a comparison of the number counts, morphology, luminosity function and star formation rate of our sample with the corresponding samples from the two HDFs.
Casertano Sefano
Wadadekar Yogesh
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