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 \buildrel < \over { \sim } 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 .