Session 51 - Galaxy Evolution and the Intergalactic Medium.
Display session, Wednesday, June 10
Atlas Ballroom,

## [51.04] Evolution in Emission-line and Broad-band Galaxy Luminosity Functions to Redshift Unity

D. W. Hogg (IAS), R. Blandford, J. G. Cohen (Caltech), M. A. Pahre (CfA)

An analysis of spectroscopic data on faint galaxies in an 8-arcmin diameter region centered on the Hubble Deep Field is presented. Source detection and photometry is performed in the U_n, G, \cal R and K_s-band images to create catalogs complete to U_n=25, G=26, \cal R=25.5 and K_s=20 mag. Keck Telescope spectroscopy exists for over 500 sources in the sample; the median redshift is 0.6.

The rest-frame equivalent widths of the \rm\left[O\,II\right] 3727\,Å\ emission line are measured as a function of galaxy flux, color and redshift. The probability that a source of a given flux, color and redshift has its \rm\left[O\,II\right] line detected is estimated. \rm\left[O\,II\right] line luminosity functions and integrated \rm\left[O\,II\right] line luminosity densities are computed; they show strong evolution, implying a much higher star formation rate density at redshifts z\sim 1 than locally.

The B-band luminosity function for the \cal R-selected sample is computed using an estimate of the probability that a source is assigned a redshift given that it has been observed spectroscopically, based on the \rm\left[O\,II\right] detection probability. The luminosity function is flat (constant number per log luminosity) and consistent with local determinations except for a higher overall normalization. No evidence is found for dependence of the luminosity function on redshift or environment, but the blue galaxy luminosity function is more dwarf-rich than the red.