Environment and galaxy evolution at intermediate redshift in the CNOC2 survey

The systematic variation of galaxy colors and types with clustering environment could either be the result of local conditions at formation or subsequent environmental effects as larger scale structures draw together galaxies whose stellar mass is largely in place. Below redshift 0.7 galaxy luminosities (k-corrected and evolution compensated) are relatively invariant, whereas galaxy star formation rates, as reflected in their colors, are a "transient" property that have a wide range for a given luminosity. The relations between these galaxy properties and the clustering properties are key statistics for understanding the forces driving late-time galaxy evolution. At z similar to 0.4 the comoving galaxy correlation length, r(o), measured in the CNOC2 sample is strongly color dependent, rising from 2 h(-1) Mpc to nearly 10 h(-1) Mpc as the volume-limited subsamples range from blue to red. The luminosity dependence of r(o) at z similar to 0.4 is weak below L-* in the R band, although there is an upturn at high luminosity, where its interpretation depends on separating it from the r(o)-color relation. In the B band there is a slow, smooth increase of r(o) with luminosity, at least partially related to the color dependence. Study of the evolution of galaxies within groups, which create much of the strongly nonlinear correlation signal, allows a physical investigation of the source of these relations. The dominant effect of the group environment on star formation is seen in the radial gradient of the mean galaxy colors, which on the average become redder than the field toward the group centers. The color differentiation begins around the dynamical radius of virialization of the groups. The redder-than-field trend applies to groups with a line-of-sight velocity dispersion, sigma (1) > 150 km s(-1). There is an indication, somewhat statistically insecure, that the high-luminosity galaxies in groups with sigma (1) < 125 km s(-1) become bluer toward the group center. Monte Carlo orbit integrations initiated at the measured positions and velocities show that the rate of galaxy merging in the <sigma>(1) > 150 km s(-1) groups is very low, whereas for sigma (1) < 150 km s(-1) about 25% of the galaxies will merge in 0.5 Gyr. We conclude that the higher velocity dispersion groups largely act to suppress star formation relative to the less clustered field, leading to "embalmed" galaxies. On the other hand, the low velocity dispersion groups are prime sites of both strong merging and enhanced star formation that leads to the formation of some new massive galaxies at intermediate redshifts. The tidal fields within the groups appear to be a strong candidate for the physical source of the reduction of star formation in group galaxies relative to field. Tides operate effectively at all velocity dispersions to remove gas-rich companions and low-density gas in galactic halos. We find a close resemblance of the color-dependent galaxy luminosity function evolution in the field and groups, suggesting that the clustering-dependent star formation reduction mechanism is important for the evolution of field galaxies as a whole.