  We present age and metallicities determinations based on narrow band
continuum colors for the galaxies in the rich clusters A1185 and Coma. Using a
new technique to extract luminosity-weighted age and [Fe/H] values for
non-star-forming galaxies, we find that both clusters have two separate
populations based on these parameters. One population is old ($\tau >$ 11 Gyrs)
with a distinct mass-metallicity relation. The second population is slightly
younger ($\tau \approx$ 9 Gyrs) with lower metallicities and lower stellar
masses. We find detectable correlations between age and galaxy mass in both
populations such that older galaxies are more massive and have higher mean
metallicities, confirming previous work with line indices for the same type of
galaxies in other clusters (Kelson et al 2006, Thomas et al 2005). Our results
imply shorter durations for higher mass galaxies, in contradiction to the
predictions of classic galactic wind models. Since we also find a clear
mass-metallicity relation for these galaxies, then we conclude that star
formation was more efficient for higher mass galaxies, a scenario described
under the inverse wind models (Matteucci 1994). With respect to cluster
environmental effects, we find there is a significant correlation between
galaxy mean age and distance from the cluster center, such that older galaxies
inhabit the core. This relationship would nominally support hierarchical
scenarios of galaxy formation (younger age in lower density regions); however,
environmental effects probably have larger signature in the sample and
present-day galaxies are remnants from an epoch of quenching of initial star
formation, which would result in the same age gradients.
