Galaxy Groups at 0.3 <= z <= 0.55. I. Group Properties

Abstract

The evolution of galaxies in groups may have important implications for the evolution of the star formation history of the universe, since many processes which operate in groups may suppress star formation and the fraction of galaxies in bound groups grows rapidly between z=1 and the present day. In this paper, we present an investigation of the properties of galaxies in galaxy groups at intermediate redshift (z ~ 0.4). The groups were selected from the CNOC2 redshift survey as described in Carlberg et al., 2001, with further spectroscopic follow-up undertaken at the Magellan telescope in order to improve the completeness and depth of the sample. We present the data for the individual groups, and find no clear trend in the fraction of passive galaxies with group velocity dispersion and group concentration. We stack the galaxy groups in order to compare the properties of group galaxies with those of field galaxies at the same redshift. The groups contain a larger fraction of passive galaxies than the field, this trend being particularly clear for galaxies brighter than M_{B_J} < -20 in the higher velocity dispersion groups. In addition, we see evidence for an excess of bright passive galaxies in the groups relative to the field. In contrast, the luminosity functions of the star forming galaxies in the groups and the field are consistent. These trends are qualitatively consitent with the differences between group and field galaxies seen in the local universe.