Volume 592, August 2016
|Number of page(s)||12|
|Section||Galactic structure, stellar clusters and populations|
|Published online||26 July 2016|
Sodium abundances of AGB and RGB stars in Galactic globular clusters
1 European Southern Observatory (ESO), Karl-Schwarschild-Str. 2, 85748 Garching b. München, Germany
2 Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Science, 100012 Beijing, PR China
3 School of Astronomy and Space Science, University of Chinese Academy of Sciences, 100049 Beijing, PR China
4 Department of Astronomy, University of Geneva, Chemin des Maillettes 51, 1290 Versoix, Switzerland
5 IRAP, UMR 5277 CNRS and Université de Toulouse, 14 Av. E. Belin, 31400 Toulouse, France
6 Institut d’Astronomie et d’Astrophysique, Université Libre de Bruxelles, CP 226, Boulevard du Triomphe, 1050 Brussels, Belgium
7 Dipartimento di Fisica, Università di Roma Tor Vergata, via della Ricerca Scientifica 1, 00133 Rome, Italy
8 INAF–Osservatorio Astronomico di Roma, via Frascati 33, Monte Porzio Catone, 00133 Rome, Italy
Received: 14 March 2016
Accepted: 22 May 2016
Context. Galactic globular clusters (GC) are known to have multiple stellar populations and be characterised by similar chemical features, e.g. O−Na anti-correlation. While second-population stars, identified by their Na overabundance, have been found from the main sequence turn-off up to the tip of the red giant branch (RGB) in various Galactic GCs, asymptotic giant branch (AGB) stars have rarely been targeted. The recent finding that NGC 6752 lacks an Na-rich AGB star has thus triggered new studies on AGB stars in GCs, since this result questions our basic understanding of GC formation and stellar evolution theory.
Aims. We aim to compare the Na abundance distributions of AGB and RGB stars in Galactic GCs and investigate whether the presence of Na-rich stars on the AGB is metallicity-dependent.
Methods. With high-resolution spectra obtained with the multi-object high-resolution spectrograph FLAMES on ESO/VLT, we derived accurate Na abundances for 31 AGB and 40 RGB stars in the Galactic GC NGC 2808.
Results. We find that NGC 2808 has a mean metallicity of −1.11 ± 0.08 dex, in good agreement with earlier analyses. Comparable Na abundance dispersions are derived for our AGB and RGB samples, with the AGB stars being slightly more concentrated than the RGB stars. The ratios of Na-poor first-population to Na-rich second-population stars are 45:55 in the AGB sample and 48:52 in the RGB sample.
Conclusions. NGC 2808 has Na-rich second-population AGB stars, which turn out to be even more numerous − in relative terms − than their Na-poor AGB counterparts and the Na-rich stars on the RGB. Our findings are well reproduced by the fast rotating massive stars scenario and they do not contradict the recent results that there is not an Na-rich AGB star in NGC 6752. NGC 2808 thus joins the larger group of Galactic GCs for which Na-rich second-population stars on the AGB have recently been found.
Key words: stars: abundances / globular clusters: general / globular clusters: individual: NGC 2808
Based on observations made with ESO telescopes at the La Silla Paranal Observatory under programme ID 093.D-0818(A).
Full Tables 2, 4, 6 are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (126.96.36.199) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/592/A66
© ESO, 2016
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