The Star Cluster Population of M51
Astrophysics
2016-08-30 v1
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).
Cite
@article{arxiv.astro-ph/0403253,
title = {The Star Cluster Population of M51},
author = {M. Gieles and N. Bastian and H. J. G. L. M. Lamers},
journal= {arXiv preprint arXiv:astro-ph/0403253},
year = {2016}
}
Comments
2 pages, to appear in "The Formation and Evolution of Massive Young Star Clusters", 17-21 November 2003, Cancun (Mexico)