Chemical abundances in bright giants of the globular cluster M62 (NGC 6266)

Yong, D. and Alves, Brito A. and Da, Costa G. S. and Alonso-García, J. and Karakas, A. I. and Pignatari, Marco and Roederer, I. U. and Aoki, W. and Fishlock, Ch. K. and Grundahl, F. and Norris, J. E. (2014) Chemical abundances in bright giants of the globular cluster M62 (NGC 6266). MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 439 (3). pp. 2638-2650. ISSN 0035-8711

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Abstract

With the exception of Terzan 5, all the Galactic globular clusters that possess signif- icant metallicity spreads, such as ω Cen and M22, are preferentially the more lumi- nous clusters with extended horizontal branches. Here we present radial velocities and chemical abundances for seven bright giants in the globular cluster M62, a previously little-studied cluster. With MV = −9.18, M62 is the ninth most luminous Galactic globular cluster and has an extended horizontal branch. Within our sample, we find (i) no evidence for a dispersion in metallicity, [Fe/H], beyond the measurement un- certainties, (ii) star-to-star abundance variations for C, O, Na and Al with the usual correlations between these elements as seen in other globular clusters, and (iii) a global enrichment for the elements Zr, Ba and La at the level [X/Fe] ≃ +0.4 dex. For elements heavier than La, the abundance ratios are consistent with the scaled-solar r-process distribution. Below La, the abundances are anomalous when compared to the scaled- solar s-process or r-process distributions. For these elements, the abundance signature in M62 is in agreement with predictions of the s-process from fast-rotating massive stars, although the high [Rb/Y] ratio we measure may be a challenge to this scenario.

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