Volume 465, Number 1, April I 2007
|Page(s)||185 - 196|
|Section||Galactic structure, stellar clusters, and populations|
|Published online||29 January 2007|
INAF-Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy e-mail: [sestito;randich]@arcetri.astro.it
2 INAF-Osservatorio Astronomico “G.S. Vaiana” di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy
3 INAF-Osservatorio Astronomico di Bologna, Via C. Ranzani 1, 40127 Bologna, Italy e-mail: firstname.lastname@example.org
Accepted: 2 January 2007
Context.We have carried out a big FLAMES survey of 10 Galactic open clusters aiming at different goals. One of them is the determination of chemical abundances, to put constraints on the radial metallicity gradient in the disk and its evolution. One of the sample clusters is the very metal-rich NGC 6253.
Aims.We have obtained UVES high resolution spectra of seven candidate cluster members (from the turn off up to the red clump) with the goal of determining the chemical composition of NGC 6253 and of investigating its origin and role in the interpretation of the radial metallicity gradient in the disk.
Methods.Equivalent width analysis and spectral synthesis were performed using MOOG and Kurucz model atmospheres.
Results.We derived abundances of Fe, α-, and Fe-peak elements, the light element Na, and the s-process element Ba. Excluding two likely non-members and the clump giant, whose metallicity from equivalent widths is overestimated, we find an average [Fe/H] = +0.36±0.07 (rms) for the cluster. For most of the other elements we derive solar abundance ratios.
Key words: stars: abundances / Galaxy: evolution / Galaxy: disk / open clusters and associations: individual: NGC 6253 / Galaxy: abundances / open clusters and associations: general
© ESO, 2007
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