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We address the nature and origin of Super Star Clusters (SSCs) discovered byHoltzman et al. (1992) within a radius of $\sim$$5\,\rm kpc$ from the center ofNGC 1275, the giant elliptical galaxy at the center of the Perseus Cluster. Weshow that, in contrast with the much more numerous population of SSCssubsequently discovered up to $\sim$$30\,\rm kpc$ from the center of thisgalaxy, the central SSC population have maximal masses an order of magnitudehigher and a mass function with a shallower power-law slope. Furthermore,whereas the outer SSC population have ages spanning a few $\rm Myr$ to at least$\sim$$1\,\rm Gyr$, the central SSC population have ages strongly concentratedaround $\sim$$500 \rm \, Myr$ with a $1\,\sigma$ dispersion of $\sim$$100\,\rmMyr$. These SSCs share a close spatial and temporal relationship with the"central spiral," which also has a radius $\sim$$5\,\rm kpc$ centered on NGC1275 and a characteristic stellar age of $\sim$$150\,\rm Myr$ (Paper I). Weargue that both the central SSC population and the central spiral formed fromgas deposited by a residual cooling flow, with the SSCs forming first followedby the formation of the stellar body of the central spiral$\sim$$300$-$400\,\rm Myr$ later. The ages of the central SSC population implythat they are able to withstand very strong tidal fields near the center of NGC1275, making them genuine progenitor globular clusters. Evidently, a spiraldisk hosting progenitor globular clusters has recently formed at the center ofa giant elliptical galaxy.

astrophysical journal/the astrophysical journal

Recent Formation of a Spiral Disk Hosting Progenitor Globular Clusters  at the center of the Perseus Brightest Cluster Galaxy: II. Progenitor  Globular Clusters