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In the lenticular galaxy NGC1023 a third population of globular clusters(GCs), called faint fuzzies (FFs), was discovered next to the blue and red GCpopulations by Larsen & Brodie. While these FFs have colors comparable to thered population, the new population is fainter, larger (R_eff > 7 pc) and, mostimportantly, shows clear signs of co-rotation with the galactic disk ofNGC1023. We present N-body simulations verifying the hypothesis that thesedisk-associated FFs are related to the young massive cluster complexes (CCs)observed by Bastian et. al in M51, who discovered a mass-radius relation forthese CCs. Our models have an initial configuration based on the observationsfrom M51 and are placed on various orbits in a galactic potential derived forNGC1023. All computations end up with a stable object containing 10 to 60% ofthe initial CC mass after an integration time of 5 Gyr. A conversion to visualmagnitudes demonstrates that the resulting objects cover exactly the observedrange for FFs. Moreover, the simulated objects show projected half-mass radiibetween 3.6 and 13.4 pc, in good agreement with the observed FF sizes. Weconclude that objects like the young massive CCs in M51 are likely progenitorsof the FFs observed in NGC1023.

Faint Fuzzy Star Clusters in NGC1023 as Remnants of Merged Star Cluster Complexes