On aging star clusters using red supergiants independent of the fraction of interacting binary stars

Abstract

We use the Binary Population and Spectral Synthesis (BPASS) models to test the recent suggestion that red supergiants can provide an accurate age estimate of a co-eval stellar population that is unaffected by interacting binary stars. Ages are estimated by using both the minimum luminosity red supergiant and the mean luminosity of red supergiants in a cluster. We test these methods on a number of observed star clusters and find our results in agreement with previous estimates. Importantly we find the difference between the ages derived from stellar population models with and without a realistic population of interacting binary stars is only a few 100,000 years at most. We find that the mean luminosity of red supergiants in a cluster is the best method to determine the age of a cluster because it is based o the entire red supergiant population rather than using only the least luminous red supergiant.

Accepted for publication in MNRAS, 7 pages, 3 pages, 2 tables

References in corpus (8)

• Binary Population and Spectral Synthesis Version 2.1: construction, observational verification and new results
• A new mass-loss rate prescription for red supergiants
• A third red supergiant rich cluster in the Scutum-Crux Arm
• The VLT-FLAMES Tarantula Survey. XXX. Red stragglers in the clusters Hodge 301 and SL 639
• Stellar rotation and the extended main sequence turnoff in the open cluster NGC 5822
• Extended main-sequence turnoffs in the double cluster $h$ and $\chi$ Persei: The complex role of stellar rotation
• Discrepancies in the ages of young star clusters; evidence for mergers?
• Disappearance of the extended main sequence turn-off in intermediate age clusters as a consequence of magnetic braking

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• Quantifying Systematic Age Discrepancies in Very Young Star Clusters