  Imaging data from the Sloan Digital Sky Survey are used to characterize the
population of galaxies in groups and clusters detected with the MaxBCG
algorithm. We investigate the dependence of Brightest Cluster Galaxy (BCG)
luminosity, and the distributions of satellite galaxy luminosity and satellite
color, on cluster properties over the redshift range 0.1 < z < 0.3. The size of
the dataset allows us to make measurements in many bins of cluster richness,
radius and redshift. We find that, within r_200 of clusters with mass above
3e13 h-1 M_sun, the luminosity function of both red and blue satellites is only
weakly dependent on richness. We further find that the shape of the satellite
luminosity function does not depend on cluster-centric distance for magnitudes
brighter than ^{0.25}M_i - 5log(h) < -19. However, the mix of faint red and
blue galaxies changes dramatically. The satellite red fraction is dependent on
cluster-centric distance, galaxy luminosity and cluster mass, and also
increases by ~5% between redshifts 0.28 and 0.2, independent of richness. We
find that BCG luminosity is tightly correlated with cluster richness, scaling
as L_{BCG} ~ M_{200}^{0.3}, and has a Gaussian distribution at fixed richness,
with sigma_{log L} ~ 0.17 for massive clusters. The ratios of BCG luminosity to
total cluster luminosity and characteristic satellite luminosity scale strongly
with cluster richness: in richer systems, BCGs contribute a smaller fraction of
the total light, but are brighter compared to typical satellites. This study
demonstrates the power of cross-correlation techniques for measuring galaxy
populations in purely photometric data.
