Helium enrichment in intermediate-age Magellanic Clouds clusters: towards an ubiquity of multiple stellar populations?

• Published in: Monthly notices of the Royal Astronomical Society Vol. 484; no. 4; pp. 5236 - 5244
• Main Authors: Chantereau, W, Salaris, M, Bastian, N, Martocchia, S
• Format: Journal Article
• Language: English
• Published: Oxford University Press 21.04.2019
• Subjects: stars: horizontal branch; stars: chemically peculiar; stars: abundances; galaxies: individual: LMC; Hertzsprung–Russell and colour–magnitude diagrams; galaxies: individual: SMC
• ISSN: 0035-8711; 1365-2966
• DOI: 10.1093/mnras/stz378

Abstract Intermediate-age star clusters in the Magellanic Clouds harbour signatures of the multiple stellar populations long thought to be restricted to old globular clusters. We compare synthetic horizontal branch models with Hubble Space Telescope photometry of clusters in the Magellanic Clouds, with age between ∼2 and ∼10 Gyr, namely NGC 121, Lindsay 1, NGC 339, NGC 416, Lindsay 38, Lindsay 113, Hodge 6, and NGC 1978. We find a clear signature of initial helium abundance spreads (ΔY) in four out of these eight clusters (NGC 121, Lindsay 1, NGC 339, NGC 416) and we quantify the value of ΔY. For two clusters (Lindsay 38, Lindsay 113), we can only determine an upper limit for ΔY, whilst for the two youngest clusters in our sample (Hodge 6 and NGC 1978) no conclusion about the existence of an initial He spread can be reached. Our ΔY estimates are consistent with the correlation between maximum He abundance spread and mass of the host cluster found in Galactic globular clusters. This result strengthens the emerging view that the formation of multiple stellar populations is a standard process in massive star clusters, not limited to a high-redshift environment.