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The chemical signatures of the Large Magellanic Cloud globular clusters

Published online by Cambridge University Press:  01 July 2008

Alessio Mucciarelli
Alessio Mucciarelli*
Affiliation:
Dipartimento di Astronomia, Università degli Studi di Bologna, Bologna, Italy email: [email protected]
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Abstract

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We present the first results of a long-term project based on the analysis of high-resolution optical spectra for a sample of Large Magellanic Cloud globular clusters. The final aim is to build a new, reliable metallicity scale for this cluster system and shed some light on the role played by the different chemical contributors (AGB, SN II and SN Ia), in order to understand the chemical enrichment history of the Large Magellanic Cloud. The analysis of 6 young and intermediate-age clusters and 11 field stars, observed with the UVES@FLAMES spectrograph, provides crucial information about the chemical composition of the dominant stellar population of the LMC. All these stars are metal-rich ([Fe/H]~ −0.4 dex), with solar-scaled [α/Fe] ratios, that point toward an enrichment from SN Ia. Moreover, we observed a general depletion for the [Al/Fe] ratio (indication of a chemical enrichment by metal-poor SN II) and a strong enhancement of the [Ba/Y] ratio (likely due to the enrichment by metal-poor AGB stars).

Keywords

techniques: spectroscopicstars: abundancesgalaxies: evolutiongalaxies: Individual (LMC)Magellanic Cloudsgalaxies: star clusters
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Symposium S256: The Magellanic System: Stars, Gas, and Galaxies , July 2008 , pp. 299 - 304
Copyright
Copyright © International Astronomical Union 2009

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