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The chemical fingerprints of the thin and the thick disk

Published online by Cambridge University Press:  01 June 2008

Sofia Feltzing ,
Sally Oey  and
Thomas Bensby
Sofia Feltzing
Affiliation:
Lund Observatory, Box 43, SE-221 00 Lund, Sweden email: sofia@astro.lu.se
Sally Oey
Affiliation:
University of Michigan830 Dennison Building, Ann Arbor, MI, USA 48109-1042, USA
Thomas Bensby
Affiliation:
European Southern ObservatoryAlonso de Cordova 3107, Vitacura, Casilla 19001, Santiago 19, Chile email: tbensby@eso.org
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Abstract

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The past history and origin of the different Galactic stellar populations are manifested in their different chemical abundance patterns. We obtained new elemental abundances for 553 F and G dwarf stars, to more accurately quantify these patterns for the thin and thick disks. However, the exact definition of disk membership is not straightforward. Stars that have a high likelihood of belonging to the thin disk show different abundance patterns from those for the thick disk. In contrast, we show that stars for the Hercules Stream do not show unique abundance patterns, but rather follow those of the thin and thick disks. This strongly suggests that the Hercules Stream is a feature induced by internal dynamics within the Galaxy rather than the remnant of an accreted satellite.

Keywords

stars: abundancesstars: kinematicsGalaxy: abundancesGalaxy: diskGalaxy: formation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Issue S254: The Galaxy Disk in Cosmological Context , June 2008 , pp. 197 - 202
Copyright
Copyright © International Astronomical Union 2009

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