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The cluster is around 25 million years old with 600 times the mass of the Sun. It spans a radius of 24 ly (7.3 pc). The metallicity of the cluster, what astronomers term the abundance of elements more massive than helium, is almost identical to that of the Sun. 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. Two eclipsing binaries and one probable Be star have been identified, but the cluster is lacking any low-amplitude pulsating variables.
^ Sabbi, 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.
Hubble Space Telescope image of the cluster NGC 299
Media related to NGC 299 at Wikimedia Commons
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