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The Star Cluster Population of M51

M. Gieles·N. Bastian·H. J. G. L. M. Lamers
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Abstract

We present the age and mass distribution of star clusters in M51. The structural parameters are found by fitting cluster evolution models to the spectral energy distribution consisting of 8 HST-WFPC2 pass bands. There is evidence for a burst of cluster formation at the moment of the second encounter with the companion NGC5195 (50-100 Myr ago) and a hint for an earlier burst (400-500 Myr ago). The cluster IMF has a power law slope of -2.1. The disruption time of clusters is extremely short (< 100 Myr for a 10^4 Msun cluster).

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M. Gieles, N. Bastian, H. J. G. L. M. Lamers. 2004-03-10. The Star Cluster Population of M51. https://arxiv.org/abs/astro-ph/0403253

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