The cluster is around 25 million years old with 600 times themass of the Sun. It spans a radius of 24 ly (7.3 pc). Themetallicity of the cluster, what astronomers term the abundance of elements more massive than helium, is almost identical to that of the Sun.[4] The cluster is old enough that the stellar winds from the most massive members has dispersed all of the original dust and gas. Hence, star formation has come to a halt.[6] Twoeclipsing binaries and one probableBe star have been identified, but the cluster is lacking any low-amplitudepulsating variables.[8]
^abSabbi, E.; et al. (2007). "Star formation in the Small Magellanic Cloud: the youngest star clusters". In Elmegreen, B. G.; Palous, J. (eds.).Proceedings of the International Astronomical Union 2: Triggered Star Formation in a Turbulent ISM. IAU Symposium #237, held 14–18 August 2006 in Prague, Czech Republic. Cambridge: Cambridge University Press. pp. 199–203.Bibcode:2007IAUS..237..199S.doi:10.1017/S1743921307001469.
^Sanders, R. J.; et al. (April 2013). "Photometric Analysis of Variable Stars in NGC 299".Information Bulletin on Variable Stars.6054: 1.arXiv:1302.6943.Bibcode:2013IBVS.6054....1S.
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