Mass-radius relation of intermediate-age disk super star clusters of M82

Abstract

We present a complete set of structural parameters for a sample of 99 intermediate-age Super Star Cluster (SSCs) in the disk of M82, and carry out a survival analysis using the semi-analytical cluster evolution code EMACSS. The parameters are based on the profile-fitting analysis carried out in a previous work, with the mass-related quantities derived using a mass-to-light ratio for a constant age of 100 Myr. The SSCs follow a power-law mass function with an index $\alpha$=1.5, and a log-normal size function with a typical half-light radius, Rh=4.3 pc, which are both comparable with the values for clusters in the Magellanic Clouds, rather than in giant spirals. The majority of the SSCs follow a power-law mass-radius relation with an index of b=0.29$\pm$0.05. A dynamical analysis of M82 SSCs using EMACSS suggests that 23% of the clusters are tidally-limited, with the rest undergoing expansion at present. Forward evolution of these clusters suggests that the majority would dissolve in ~2 Gyr. However, a group of four massive compact clusters, and another group of five SSCs at relatively large galactocentric distances, are found to survive for a Hubble time. The model-predicted mass, Rh, ${\mu }_V$ and core radius of these surviving SSCs at 12 Gyr are comparable with the corresponding values for the sample of Galactic globular clusters.

18 pages, 22 figures, Accepted to be published in MNRAS

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Cited by in corpus (2)

• Radii of Young Star Clusters in Nearby Galaxies
• On the formation of globular clusters: comparison with observations