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We investigate the star-formation properties of dynamically relaxed galaxyclusters as a function of cluster mass for 308 low-redshift clusters drawn fromthe Sloan Digital Sky Survey (SDSS) C4 cluster catalog. It is important toestablish if cluster star-formation properties have a mass dependence beforecomparing clusters at different epochs, and here we use cluster velocitydispersion as a measure of cluster mass. We find that the total stellar mass,the number of star-forming galaxies, and total star-formation rate scalelinearly with the number of member galaxies, with no residual dependence oncluster velocity dispersion. With the mass-dependence of cluster star-formationrates established, we compare the SDSS clusters with a sample of z = 0.75clusters from the literature and find that on average the total H-alphaluminosity of the high-redshift clusters is 10 times greater than that of thelow-redshift clusters. This can be explained by a decline in the H-alphaluminosities of individual cluster galaxies by a factor of up to 10 since z =0.75. The magnitude of this evolution is comparable to that of field galaxiesover a similar redshift interval, and thus the effect of the clusterenvironment on the evolution of star-forming galaxies is at most modest. Ourresults suggest that the physical mechanism driving the evolution of clusterstar-formation rates is independent of cluster mass, at least for clusters withvelocity dispersion greater than 450 km/s, and operates over a fairly longtimescale such that the star-formation rates of individual galaxies decline byan order of magnitude over ~7 billion years. (Abridged)

Mass and Redshift Dependence of Star Formation in Relaxed Galaxy Clusters