  We present an analysis of compact star clusters in deep HST/WFPC2 images of
NGC 1275. B and R band photometry of roughly 3000 clusters shows a bimodality
in the B-R colors, suggesting that distinct old and young cluster populations
are present. The small spread in the colors of the blue clusters is consistent
with the hypothesis that they are a single age population, with an inferred age
of 0.1 to 1 Gyr. The luminosity function shows increasing numbers of blue
clusters to the limit of our photometry, which reaches several magnitudes past
the turnover predicted if the cluster population were identical to current
Galactic globulars seen at a younger age. The blue clusters have a spatial
distribution which is more centrally peaked than that of the red clusters. The
individual clusters are slightly resolved, with core radii <~ 0.75 pc if they
have modified Hubble profiles. We estimate the specific frequencies of the old
and young populations and discuss the uncertainties in these estimates. We find
that the specific frequency of the young population in NGC 1275 is currently
larger than that of the old population and will remain so as the young
population evolves, even if the majority of the low mass clusters are
eventually destroyed. If the young population formed during a previous merger,
this suggests that mergers can increase the specific frequency of globulars in
a galaxy. However, the presently observed young population likely contains too
few clusters to have a significant impact on the overall specific frequency as
it will be observed in the future.
