  There has been plenty of observational evidence of cluster galaxy evolution
such as the Butcher-Oemler effect and the decrease in S0 fraction with
increasing redshift. As a modern version, the redshift evolution of total star
formation rate (SFR) in clusters has been actively debated recently. However,
these studies of redshift trend have been always hampered by the possible mass
dependence; due to the observational selection effects, clusters found at
higher redshift inevitably tend to be more massive and luminous than local
counterparts. Consequently, one has to correct for the mass trend before
interpreting the redshift trend.
  As an attempt to break this degeneracy, we investigate the mass dependence of
blue/late-type fractions and total SFR of 115 clusters at $z\leq 0.09$ selected
from the Sloan Digital Sky Survey. We find that none of blue/late-type
fractions, total SFR and total SFR normalized by cluster mass shows significant
dependence on cluster virial mass. The scatter is much larger at each cluster
mass than a possible trend. Our results indicates that physical mechanisms that
depend on cluster mass (such as the ram-pressure stripping) are not likely to
be solely responsible for cluster galaxy evolution. Our results also provide an
excellent low redshift comparison sample for future high redshift cluster SFR
studies.
