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The Gaia-ESO Survey: Detailed abundances in the metal-poor globular cluster NGC 4372
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2015 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 579, A6Article in journal (Refereed) Published
Abstract [en]

We present the abundance analysis for a sample of 7 red giant branch stars in the metal-poor globular cluster NGC 4372 based on UVES spectra acquired as part of the Gaia-ESO Survey. This is the first extensive study of this cluster from high-resolution spectroscopy. We derive abundances of O, Na, Mg, Al, Si, Ca, Sc, Ti, Fe, Cr, Ni, Y, Ba, and La. We find a metallicity of [Fe/H] = -2.19 +/- 0.03 and find no evidence of any metallicity spread. This metallicity makes NGC 4372 one of the most metal-poor Galactic globular clusters. We also find an a-enhancement typical of halo globular clusters at this metallicity. Significant spreads are observed in the abundances of light elements. In particular, we find a Na-O anticorrelation. Abundances of O are relatively high compared with other globular clusters. This could indicate that NGC 4372 was formed in an environment with high O for its metallicity. A Mg-Al spread is also present that spans a range of more than 0.5 dex in Al abundances. Na is correlated with Al and Mg abundances at a lower significance level. This pattern suggests that the Mg-Al burning cycle is active. This behavior can also be seen in giant stars of other massive, metal-poor clusters. A relation between light and heavy s-process elements has been identified.

Place, publisher, year, edition, pages
2015. Vol. 579, A6
Keyword [en]
globular clusters: individual: NGC 4372, stars: abundances
National Category
Physical Sciences
Identifiers
URN: urn:nbn:se:uu:diva-261309DOI: 10.1051/0004-6361/201525722ISI: 000358877100018OAI: oai:DiVA.org:uu-261309DiVA: diva2:851098
Funder
EU, FP7, Seventh Framework Programme, 320360
Available from: 2015-09-03 Created: 2015-09-01 Last updated: 2017-12-04Bibliographically approved

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Korn, Andreas J.Heiter, Ulrike

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