Volume 548, December 2012
|Number of page(s)||11|
|Section||Galactic structure, stellar clusters and populations|
|Published online||27 November 2012|
1 Universidad de Concepción, Departamento de Astronomia, Fac. Cs. Físicas y Matemáticas. Barrio Universitario, Concepción, Chile
e-mail: firstname.lastname@example.org; email@example.com; firstname.lastname@example.org
2 European Southern Observatory, Alonso de Cordova 3107, Vitacura, Santiago, Chile
3 Space Telescope Science Institute, 3700 San Martin Dr., Baltimore, MD 21218, USA
4 Department of Astronomy, University of Florida, Gainesville, FL 32611, USA
5 School of Mathematics & Physics, University of Tasmania, Private Bag 37, Hobart, TAS, Australia
6 National Optical Astronomy Observatories, PO Box 26732, Tucson, AZ 85726, USA
7 Dipartimento di Astronomia, Università di Padova, Vicolo Osservatorio 3, 35122 Padova, Italia
8 Astronomy Department, Yale University, New Haven, CT 06520, USA
Received: 4 June 2012
Accepted: 13 August 2012
Context. The study of globular clusters is one of the most powerful ways to learn about a galaxy’s chemical evolution and star formation history. They preserve a record of chemical abundances at the time of their formation and are relatively easy to age date. The most detailed knowledge of the chemistry of a star is given by high resolution spectroscopy, which provides accurate abundances for a wide variety of elements, yielding a wealth of information on the various processes involved in the cluster’s chemical evolution.
Aims. We studied red giant branch (RGB) stars in an old, metal-poor globular cluster of the Large Magellanic Cloud (LMC), Hodge 11 (H11), in order to measure as many elements as possible. The goal is to compare its chemical trends to those in the Milky Way halo and dwarf spheroidal galaxies in order to help understand the formation history of the LMC and our own Galaxy.
Methods. We have obtained high resolution VLT/FLAMES spectra of eight RGB stars in H11. The spectral range allowed us to measure a variety of elements, including Fe, Mg, Ca, Ti, Si, Na, O, Ni, Cr, Sc, Mn, Co, Zn, Ba, La, Eu and Y.
Results. We derived a mean [Fe/H] = −2.00 ± 0.04, in the middle of previous determinations. We found low [α/Fe] abundances for our targets, more comparable to values found in dwarf spheroidal galaxies than in the Galactic halo, suggesting that if H11 is representative of its ancient populations then the LMC does not represent a good halo building block. Our [Ca/Fe] value is about 0.3 dex less than that of halo stars used to calibrate the Ca IR triplet technique for deriving metallicity. A hint of a Na abundance spread is observed. Its stars lie at the extreme high O, low Na end of the Na:O anti-correlation displayed by Galactic and LMC globular clusters.
Key words: stars: abundances / Magellanic Clouds / globular clusters: individual: Hodge 11
Based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere, Chile (proposal ID 082.B-0458).
Table 4 is only available in electronic form at http://www.aanda.org
© ESO, 2012
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