Evolution of the Galaxy Population Based on Photometric Redshifts in the Hubble Deep Field

Abstract

This paper presents the results of a photometric redshift study of galaxies in the Hubble Deep Field (HDF). The method of determining redshifts from broadband colors is described, and the dangers inherent in using it to estimate redshifts, particularly at very high z, are discussed. In particular, the need for accurate high-z spectral energy distributions is illustrated. The validity of our photometric redshift technique is demonstrated both by direct verification with available HDF spectroscopic data and by comparisons of luminosity functions and luminosity densities with those obtained from z < 1 spectroscopic redshift surveys. Evolution of the galaxy population is studied over 0 ∼ < z < 4. Brightening is seen in both the luminosity function and the luminosity density out to z ≈ 3; this is followed by a decline in both at z > 3. A population of z < 0.5 star-forming dwarfs is observed to M F450W AB = −11. Our results are discussed in the context of recent developments in the understanding of galaxy evolution.

The impact of starbursts and post-starbursts on the photometric evolution of high redshift galaxies

“…A comparison between our set of undisturbed, chemically consistent galaxy models E through Sd over the redshift range from z > 4 through z > ∼ 0 and the Hubble Deep Field North (HDF-N) galaxies with photometric redshifts from Sawicki et al (1997) was presented in Bicker et al (2004). We recall that the agreement between our chemically consistent models, which account for the increasing metallicities of successive stellar generations, and the data was much better than for any earlier models using solar metallicity input physics alone.…”

Star formation histories versus redshift: consequences for overall metallicity and deuterium destruction

“…The HDF data of Madau et al (1996) at 0.15 at z > 2, is difficult to use for our purpose here because of the effects of extinction which may range from a factor of ∼ 3 (Pettini et al 1997b) to as much as a factor of ∼ 15 (Meurer 1997). For completeness, we also compare our results with the HDF data of Sawicki et al (1997) which are at the slightly different wavelengths of 0.3 and 0.45 µm (we will ignore this difference with the other data) and in the redshift bins, 0.2 -0.5, 0.5 -1.0, 1 -2, 2 -3, and 3 -4.…”

“…As indicated in section 1, we compare the results of our model calculations to the high redshift data of Lilly et al (1996), Connolly et al (1997), and Sawicki et al (1997). Lilly et al used the CFRS galaxy sample for which both redshift and B,V,K and I band photometry was available.…”

“…Recent observations of the luminosity density at high redshift (Lilly et al 1996, Madau et al 1996, Connolly et al 1997, Sawicki , Lin, & Yee 1997 are making it possible for the first time to test models of cosmic chemical evolution. Madau et al (1997) tested several models of cosmic chemical evolution by varying the IMF.…”

A Review of High-Redshift Merger Observations

“…Imaging follow-up observations of Lyman-limit systems have in turn yielded views of systems at z > 2 . Because of their unprecedented depth, and intensive spectroscopic and photometric redshift follow-ups (Cohen et al 1996;Lanzetta et al 1996;Mobasher et al 1996;Phillips et al 1997;Sawicki et al 1997), Hubble Deep Field observation of faint galaxy morphology are the likely to yield the greatest insights into evolving distribution of morphological types at high redshifts for some time to come van den Bergh et al 1996;Bouwens et al 1997;Guzman et al 1997). Eagerly anticipated are the results from high-resolution infrared observations in the HDF with NICMOS, and forthcoming observations of the HDF South.…”