Astronomy and Astrophysics – Astrophysics
Scientific paper
2006-07-19
Astron.Astrophys.458:121-134,2006
Astronomy and Astrophysics
Astrophysics
accepted by A&A, 17 pages, 8 ps figures
Scientific paper
10.1051/0004-6361:20065175
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 (alpha 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. We performed equivalent width analysis with the spectral code MOOG, which allows us to define a metallicity scale and build a homogeneous sample. 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.
Bragaglia Angela
Carretta Eugenio
Prisinzano Loredana
Randich Sofia
Sestito Paola
No associations
LandOfFree
Old open clusters as key tracers of Galactic chemical evolution. I. Fe abundances in NGC 2660, NGC 3960, and Berkeley 32 does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Old open clusters as key tracers of Galactic chemical evolution. I. Fe abundances in NGC 2660, NGC 3960, and Berkeley 32, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Old open clusters as key tracers of Galactic chemical evolution. I. Fe abundances in NGC 2660, NGC 3960, and Berkeley 32 will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-625991