Volume 578, June 2015
|Number of page(s)||17|
|Section||Galactic structure, stellar clusters and populations|
|Published online||15 June 2015|
The normal chemistry of multiple stellar populations in the dense globular cluster NGC 6093 (M 80)⋆,⋆⋆,⋆⋆⋆
1 INAF–Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, Italy
2 INAF–Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, 35122 Padova, Italy
3 Dept. of Physics and Astronomy, Macquarie University, NSW 2109 Sydney, Australia
4 Monash Centre for Astrophysics, Monash University, School of Mathematical Sciences, Building 28, Clayton VIC 3800, Melbourne, Australia
5 European Southern Observatory, Alonso de Cordova 3107, Vitacura, Santiago, Chile
6 INAF–Osservatorio Astrofisico di Catania, via S.Sofia 78, 95123 Catania, Italy
7 Dipartimento di Fisica e Astronomia, Università di Catania, via S.Sofia 78, 95123 Catania, Italy
Received: 24 February 2015
Accepted: 6 March 2015
We present the abundance analysis of 82 red giant branch stars in the dense, metal-poor globular cluster NGC 6093 (M 80), the largest sample of stars analysed in this way for this cluster. From high-resolution UVES spectra of 14 stars and intermediate resolution GIRAFFE spectra for the other stars we derived abundances of O, Na, Mg, Al, Si, Ca, Sc, Ti, V, Cr, Mn, Fe, Co, Ni, Cu, Zn, Y, Zr, Ba, La, Ce, Pr, Nd, Sm, Eu. On our UVES metallicity scale the mean metal abundance of M 80 is [Fe/H] = −1.791 ± 0.006 ± 0.076 (±statistical ±systematic error) with σ = 0.023 (14 stars). M 80 shows star-to-star variations in proton-capture elements, and the extension of the Na-O anti-correlation perfectly fit the relations with (i) total cluster mass; (ii) horizontal branch morphology; and (iii) cluster concentration previously found by our group. The chemistry of multiple stellar populations in M 80 does not look extreme. The cluster is also a representative of halo globular clusters concerning the pattern of α-capture and Fe-group elements. However we found that a significant contribution from the s-process is required to account for the distribution of neutron-capture elements. A minority of stars in M 80 seem to exhibit slightly enhanced abundances of s-process species, compatible with those observed in M 22 and NGC 1851, although further confirmation from larger samples is required.
Key words: stars: abundances / stars: Population II / globular clusters: general / globular clusters: individual: NGC 6093 (M 80) / stars: atmospheres
Full Tables 2, 3, 5–9 are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (18.104.22.168) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/578/A116
Appendix A is available in electronic form at http://www.aanda.org
© ESO, 2015
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