Elemental abundance trends in the Galactic thin and thick disks as traced by nearby F and G dwarf stars

Free access article

Issue		A&A Volume 410, Number 2, November I 2003


Page(s)		527 - 551
Section		Stellar clusters and associations
DOI		http://dx.doi.org/10.1051/0004-6361:20031213

A&A 410, 527-551 (2003)
DOI: 10.1051/0004-6361:20031213

Elemental abundance trends in the Galactic thin and thick disks as traced by nearby F and G dwarf stars

T. Bensby, S. Feltzing and I. Lundström

Lund Observatory, Box 43, 221 00 Lund, Sweden
(Received 14 April 2003 / Accepted 5 August 2003)

Abstract
Based on spectra from F and G dwarf stars, we present elemental abundance trends in the Galactic thin and thick disks in the metallicity regime $\rm -0.8\lesssim [Fe/H] \lesssim +0.4$ . Our findings can be summarized as follows. 1) Both the thin and the thick disks show smooth and distinct abundance trends that, at sub-solar metallicities, are clearly separated. 2) For the $\alpha$ -elements the thick disk shows signatures of chemical enrichment from SNe type Ia. 3) The age of the thick disk sample is in the mean older than the thin disk sample. 4) Kinematically, there exist thick disk stars with super-solar metallicities. Based on these findings, together with other constraints from the literature, we discuss different formation scenarios for the thick disk. We suggest that the currently most likely formation scenario is a violent merger event or a close encounter with a companion galaxy. Based on kinematics the stellar sample was selected to contain stars with high probabilities of belonging either to the thin or to the thick Galactic disk. The total number of stars are 66 of which 21 belong to the thick disk and 45 to the thin disk. The analysis is based on high-resolution spectra with high signal-to-noise ( $R\sim 48\,000$ and $S/N \gtrsim 150$ , respectively) recorded with the FEROS spectrograph on La Silla, Chile. Abundances have been determined for four $\alpha$ -elements (Mg, Si, Ca, and Ti), for four even-nuclei iron peak elements (Cr, Fe, Ni, and Zn), and for the light elements Na and Al, from equivalent width measurements of ~ $30\,000$ spectral lines. An extensive investigation of the atomic parameters, $\log gf$ -values in particular, have been performed in order to achieve abundances that are trustworthy. Noteworthy is that we find for Ti good agreement between the abundances from $\ion{Ti}{i}$ and $\ion{Ti}{ii}$ . Our solar Ti abundances are in concordance with the standard meteoritic Ti abundance.

Key words: stars: fundamental parameters -- stars: abundances -- Galaxy: disk -- Galaxy: formation -- Galaxy: abundances -- Galaxy: kinematics and dynamics

Offprint request: T. Bensby, thomas@astro.lu.se

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