  We investigate the extent to which galaxies' star-formation histories and
morphologies are determined by their clustocentric distance and their nearest
cluster's richness. We look at three tracers of star-formation history (i-band
absolute magnitude M_i, [g-r] color, and Halpha emission line equivalent width)
and two indicators of galaxy morphology (surface brightness and radial
concentration) for 52,569 galaxies in the redshift range of 0.015<z<0.068. We
find that our morphology indicators relate to the clustocentric distance only
indirectly through their relationships with stellar population and
starformation rate. Galaxies that are near the cluster center tend to be more
luminous, redder and have lower Halpha EW (ie, lower star-formation rates) than
those that lie near or outside the virial radius of the cluster. The detailed
relationships between these galaxy properties and clustocentric distance depend
on cluster richness. For richer clusters, we find that (i) the transition in
color and Halpha EW from cluster center to field values is more abrupt and
occurs closer to the cluster virial radius, and (ii) the color and Halpha EW
distributions are overall narrower than in less rich clusters. We also find
that the radial gradient seen in the luminosity distribution is strongest
around the smaller clusters and decreases as cluster richness increases. We
find there is a `characteristic distance' at around one virial radius (the
infall region) where the change with radius of galaxy property distributions is
most dramatic, but we find no evidence for infall-triggered star bursts. These
results suggest that galaxies `know' the distance to, and the size of, their
nearest cluster and they express this information in their star-formation
histories.
