ACS imaging of star clusters in M51 II. The luminosity function and mass function across the disk

Details ACS imaging of star clusters in M51 II. The luminosity function and mass function across the disk ACS imaging of star clusters in M51 II. The luminosity function and mass function across the disk

2008-06-23

arxiv.org/abs/0806.3752v2

Astronomy and Astrophysics, Volume 487, Issue 3, 2008, pp.937-949

Astronomy and Astrophysics

Astrophysics

15 pages, 9 figures, accepted for publication in Astronomy and Astrophysics, replaced equation 3

Scientific paper

10.1051/0004-6361:20078831

Whether or not there exists a physical upper mass limit for star clusters is still unclear. HST/ACS data for the rich cluster population in the interacting galaxy M51 enables us to investigate this in more detail. We investigate whether the cluster luminosity function (LF) in M51 shows evidence for an upper limit to the mass function. The variations of the LF parameters with position on the disk are addressed. We determine the cluster LF for all clusters in M51 falling within our selection criteria, as well as for several subsets of the sample. In that way we can determine the properties of the cluster population as a function of galactocentric distance and background intensity. By comparing observed and simulated LFs we can constrain the underlying cluster initial mass function and/or cluster disruption parameters. A physical upper mass limit for star clusters will appear as a bend dividing two power law parts in the LF, if the cluster sample is large enough to sample the full range of cluster masses. The location of the bend in the LF is indicative of the value of the upper mass limit. The slopes of the power laws are an interplay between upper masses, disruption and fading. The LF of the cluster population of M51 is better described by a double power law than by a single power law. We show that the cluster initial mass function is likely to be truncated at the high mass end. We conclude from the variation of the LF parameters with galactocentric distance that both the upper mass limit and the cluster disruption parameters are likely to be a function of position in the galactic disk. At higher galactocentric distances the maximum mass is lower, cluster disruption slower, or both.

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