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While the star formation rates and morphologies of galaxies have long beenknown to correlate with their local environment, the process by which thesecorrelations are generated is not well understood. Galaxy groups are thought toplay an important role in shaping the physical properties of galaxies beforeentering massive clusters at low redshift, and transformations of satellitegalaxies likely dominate the buildup of local environmental correlations. Toilluminate the physical processes that shape galaxy evolution in denseenvironments, we study a sample of 116 X-ray selected galaxy groups at z=0.2-1with halo masses of 10^13-10^14 M_sun and centroids determined with weaklensing. We analyze morphologies based on HST imaging and colors determinedfrom 31 photometric bands for a stellar mass-limited population of 923satellite galaxies and a comparison sample of 16644 field galaxies. Controllingfor variations in stellar mass across environments, we find significant trendsin the colors and morphologies of satellite galaxies with group-centricdistance and across cosmic time. Specifically at low stellar mass(log(M_stellar/M_sun) = 9.8-10.3), the fraction of disk-dominated star-forminggalaxies declines from >50% among field galaxies to <20% among satellites nearthe centers of groups. This decline is accompanied by a rise in quenchedgalaxies with intermediate bulge+disk morphologies, and only a weak increase inred bulge-dominated systems. These results show that both color and morphologyare influenced by a galaxy's location within a group halo. We suggest thatstrangulation and disk fading alone are insufficient to explain the observedmorphological dependence on environment, and that galaxy mergers or close tidalencounters must play a role in building up the population of quenched galaxieswith bulges seen in dense environments at low redshift.

Galaxies in X-ray Groups. III. Satellite Color and Morphology Transformations