Volume 421, Number 3, July III 2004
|Page(s)||969 - 976|
|Section||Galactic structure, stellar clusters, and populations|
|Published online||29 June 2004|
A possible age-metallicity relation in the Galactic thick disk? *
Lund Observatory, Box 43, 221 00 Lund, Sweden e-mail: [sofia;ingemar]@astro.lu.se
Corresponding author: T. Bensby, firstname.lastname@example.org
Accepted: 21 March 2004
A sample of 229 nearby thick disk stars has been used to investigate the existence of an age-metallicity relation (AMR) in the Galactic thick disk. The results indicate that that there is indeed an age-metallicity relation present in the thick disk. By dividing the stellar sample into sub-groups, separated by 0.1 dex in metallicity, we show that the median age decreases by about 5–7 Gyr when going from [Fe/H] to [Fe/H] . Combining our results with our newly published α-element trends for a local sample of thick disk stars that show signatures from supernovae type Ia (SN Ia), we draw the conclusion that the time-scale for the peak of the SN Ia rate is of the order of 3–4 Gyr in the thick disk. The tentative evidence for a thick disk AMR that we present here also has implications for the thick disk formation scenario; star-formation must have been an ongoing process for several billion years. This appears to strengthen the hypothesis that the thick disk originated from a merger event with a companion galaxy that puffed up a pre-existing thin disk.
Key words: stars: Hertzsprung-Russell (HR) and C-M diagrams / stars: kinematics / Galaxy: disk / Galaxy: kinematics and dynamics / Galaxy: solar neighbourhood / Galaxy: formation
© ESO, 2004
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