An HST/WFPC2 Survey of Bright Young Clusters in M31 III. Structural Parameters

Details An HST/WFPC2 Survey of Bright Young Clusters in M31 III. Structural Parameters An HST/WFPC2 Survey of Bright Young Clusters in M31 III. Structural Parameters

2009-09-22

arxiv.org/abs/0909.4053v1

Astron. J. 138:1667-1680 (2009)

Astronomy and Astrophysics

Astrophysics

Galaxy Astrophysics

AJ in press; 37 pages, 12 figures

Scientific paper

10.1088/0004-6256/138/6/1667

Surface brightness profiles for 23 M31 star clusters were measured using images from the Wide Field Planetary Camera 2 on the Hubble Space Telescope, and fit to two types of models to determine the clusters' structural properties. The clusters are primarily young (~10^8 yr) and massive (~10^4.5 solar masses), with median half-light radius 7 pc and dissolution times of a few Gyr. The properties of the M31 clusters are comparable to those of clusters of similar age in the Magellanic Clouds. Simulated star clusters are used to derive a conversion from statistical measures of cluster size to half-light radius so that the extragalactic clusters can be compared to young massive clusters in the Milky Way. All three sets of star clusters fall approximately on the same age-size relation. The young M31 clusters are expected to dissolve within a few Gyr and will not survive to become old, globular clusters. However, they do appear to follow the same fundamental plane relations as old clusters; if confirmed with velocity dispersion measurements, this would be a strong indication that the star cluster fundamental plane reflects universal cluster formation conditions.

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