Galaxy Spectral Energy Distributions at High Redshift

Details Galaxy Spectral Energy Distributions at High Redshift Galaxy Spectral Energy Distributions at High Redshift

Jul 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001hst..prop.9194c&link_type=abstract

HST Proposal ID #9194

Computer Science

Hst Proposal Id #9194 Galaxies

Scientific paper

The modeling of galaxy evolution {e.g. colors and spectral types} relies on a detailed understanding of the underlying galaxy spectral energy distributions {SEDs}. Comparison between the colors of galaxies and model SEDs work well for long lived stellar populations {i.e. restframe optical} but break down in the ultraviolet and near-infrared. This significantly limits our understanding of the evolution of high redshift galaxies {where the optical passbands sample the restframe ultraviolet}. To alleviate these problems we require a set of SEDs that can reproduce the observed UV colors of intermediate and redshift galaxies. Undertaking such a task through spectrophotometric observations would be prohibitive in terms of telescope time. We have, therefore, developed a technique for extracting the SEDs of galaxies directly from multicolor photometry. From a pilot study, using 127 HDF galaxies, we have shown we can derive SEDs that better match the colors of high redshift galaxies than existing SED models. The resolution and accuracy of our reconstructed SEDs are currently limited by the number of galaxies in the HDF. We propose here to extend our analysis to >2000 galaxies in the HST archive with multicolor photometry and published redshifts. We will derive a high resolution set of SEDs of galaxies at z>0.3 {the high redshift equivalent of the Kennicutt SED sample} and use these data to quantify the spectral evolution of galaxies.

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