Photometric redshifts in the Hubble Deep Fields: evolution of extinction and the star-formation rate

Details Photometric redshifts in the Hubble Deep Fields: evolution of extinction and the star-formation rate Photometric redshifts in the Hubble Deep Fields: evolution of extinction and the star-formation rate

2003-07-30

arxiv.org/abs/astro-ph/0307529v1

Mon.Not.Roy.Astron.Soc.345:819,2003

Astronomy and Astrophysics

Astrophysics

18 pages, 29 figures, accepted for publication in MNRAS

Scientific paper

10.1046/j.1365-8711.2003.06996.x

Photometric redshifts are studied with a template approach using data from HDF-N and -S . The problem of aliasing in photometric redshift estimates is investigated in some detail and found not to be a significant problem if at least four photometric bands are available. The performance of the approach presented here appears to exceed that of others in the literature. With reasonable restrictions, it is possible to determine the dust extinction as well as the photometric redshift, provided five or more photometric bands are available. An important result is that evolution of with redshift is seen, with higher values than locally at z = 0.5-1.5, and lower values at z > 2. This is consistent with current models for the star formation history of the universe. Deconvolving the uv-to-ir seds into an old star and young star component allows determination of M_* and \dot{M}_* for each galaxy, as well as z_{phot} and A_V, provided that infrared photometric bands are available. The expected trend of b = M_*/\dot{M}_* t_0 increasing to the past is seen. However there is a great deal of scatter in the relation between b and sed type, showing that the recent star-formation history is not very well correlated with the long-term history of a galaxy. The 2800 A luminosity function and star-formation rate are calculated for a large sample of HDF-N (2490) and HDF-S (28719) galaxies, using photometric redshifts, for the redshift range 0.2-5. The star-formation rates agree reasonably well with those from a variety of other uv, $H_{\alpha}$, infrared and submillimetre estimates, and with star-formation histories used to model optical, infrared and submillimetre source-counts.

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