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Galaxy clusters provide powerful laboratories for the study of galaxyevolution, particularly the origin of correlations of morphology and starformation rate (SFR) with density. We construct visible to MIR spectral energydistributions (SEDs) of cluster galaxies and use them to measure stellar massesand SFRs in eight low redshift clusters, which we examine as a function ofenvironment. A partial correlation analysis indicates that SFR depends stronglyon R/R200 (>99.9% confidence) and is independent of projected local density atfixed radius. SFR also shows no residual dependence on stellar mass. Wetherefore conclude that interactions with the intra-cluster medium drive theevolution of SFRs in cluster galaxies. A merged sample of galaxies from thefive most complete clusters shows <SFR>\propto(R/R200)^(1.3+/-0.7) for galaxieswith R/R200<0.4. A decline in the fraction of SFGs toward the cluster centercontributes most of this effect, but it is accompanied by a reduction in SFRsamong star-forming galaxies (SFGs) near the cluster center. The increase in thefraction of SFGs toward larger R/R200 and the isolation of SFGs with reducedSFRs near the cluster center are consistent with ram pressure stripping as themechanism to truncate star formation in galaxy clusters. We conclude thatstripping drives the properties of SFGs over the range of radii we examine. Wealso find that galaxies near the cluster center are more massive than galaxiesfarther out in the cluster at ~3.5\sigma, which suggests that cluster galaxiesexperience dynamical relaxation during the course of their evolution.

A Multi-Wavelength Study of Low Redshift Cluster of Galaxies II. Environmental Impact on Galaxy Growth