Volume 458, Number 1, October IV 2006
|Page(s)||121 - 134|
|Section||Galactic structure, stellar clusters, and populations|
|Published online||16 October 2006|
Old open clusters as key tracers of Galactic chemical evolution
I. Fe abundances in NGC 2660, NGC 3960, and Berkeley 32
INAF - Osservatorio Astronomico “G.S. Vaiana” di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy e-mail: email@example.com
2 INAF - Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy
3 INAF - Osservatorio Astronomico di Bologna, via C. Ranzani 1, 40127 Bologna, Italy
Accepted: 14 June 2006
Aims.We obtained high-resolution UVES/FLAMES observations of a sample of nine old open clusters spanning a wide range of ages and Galactocentric radii. The goal of the project is to investigate the radial metallicity gradient in the disk, as well as the abundance of key elements (α and Fe-peak elements). In this paper we present the results for the metallicity of three clusters: NGC 2660 (age ~1 Gyr, Galactocentric distance of 8.68 kpc), NGC 3960 (~1 Gyr, 7.80 kpc), and Be 32 (~6-7 Gyr, 11.30 kpc). For Be 32 and NGC 2660, our study provides the first metallicity determination based on high-resolution spectra.
Methods.We performed equivalent width analysis with the spectral code MOOG, which allows us to define a metallicity scale and build a homogeneous sample.
Results.We find that NGC 3960 and NGC 2660 have a metallicity that is very close to solar ([Fe/H] = +0.02 and +0.04, respectively), while the older Be 32 turns out to have [Fe/H] = -0.29.
Key words: stars: abundances / stars: evolution / Galaxy: disk / open clusters and associations: individual: NGC 2660 / open clusters and associations: individual: NGC 3960 / open clusters and associations: individual: Berkeley 32
© ESO, 2006
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