A possible age-metallicity relation in the Galactic thick disk?

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Fältnamn	Indikatorer	Metadata
000		03959naa a2200421 4500
001		oai:lup.lub.lu.se:2c0409d9-99b5-4765-8541-1abcdfc0cee9
003		SwePub
008		160401s2004 \| \|\|\|\|\|\|\|\|\|\|\|000 \|\|eng\|
024	7	a https://lup.lub.lu.se/record/1341192 URI
024	7	a https://doi.org/10.1051/0004-6361:200359572 DOI
040		a (SwePub)lu
041		a engb eng
042		9 SwePub
072	7	a art2 swepub-publicationtype
072	7	a ref2 swepub-contenttype
100	1	a Bensby, Thomasu Lund University,Lunds universitet,Astronomi - Genomgår omorganisation,Institutionen för astronomi och teoretisk fysik - Genomgår omorganisation,Naturvetenskapliga fakulteten,Lund Observatory - Undergoing reorganization,Department of Astronomy and Theoretical Physics - Undergoing reorganization,Faculty of Science4 aut0 (Swepub:lu)astr-tbe
245	1 0	a A possible age-metallicity relation in the Galactic thick disk?
264		c 2004-06-29
264	1	b EDP Sciences,c 2004
338		a electronic2 rdacarrier
520		a A sample of 229 nearby thick disk stars has been used to investigate theexistence of an age-metallicity relation (AMR) in the Galactic thickdisk. The results indicate that that there is indeed an age-metallicityrelation present in the thick disk. By dividing the stellar sample intosub-groups, separated by 0.1 dex in metallicity, we show that the medianage decreases by about 5-7 Gyr when going from [Fe/H] ≈ -0.8 to[Fe/H] ≈ -0.1. Combining our results with our newly publishedα-element trends for a local sample of thick disk stars that showsignatures from supernovae type Ia (SN Ia), we draw the conclusion thatthe time-scale for the peak of the SN Ia rate is of the order of 3-4 Gyrin the thick disk. The tentative evidence for a thick disk AMR that wepresent here also has implications for the thick disk formationscenario; star-formation must have been an ongoing process for severalbillion years. This appears to strengthen the hypothesis that the thickdisk originated from a merger event with a companion galaxy that puffedup a pre-existing thin disk.Based on data obtained with the Hipparcos satellite.
650	7	a NATURVETENSKAPx Fysikx Astronomi, astrofysik och kosmologi0 (SwePub)103052 hsv//swe
650	7	a NATURAL SCIENCESx Physical Sciencesx Astronomy, Astrophysics and Cosmology0 (SwePub)103052 hsv//eng
653		a stars: Hertzsprung-Russell (HR) and C-M diagrams
653		a stars: kinematics
653		a Galaxy: disk
653		a Galaxy: formation
653		a Galaxy: solar neighbourhood
653		a Galaxy: kinematics and dynamics
700	1	a Feltzing, Sofiau Lund University,Lunds universitet,Astronomi - Genomgår omorganisation,Institutionen för astronomi och teoretisk fysik - Genomgår omorganisation,Naturvetenskapliga fakulteten,Lund Observatory - Undergoing reorganization,Department of Astronomy and Theoretical Physics - Undergoing reorganization,Faculty of Science4 aut0 (Swepub:lu)astr-sfe
700	1	a Lundström, Ingemaru Lund University,Lunds universitet,Astronomi - Genomgår omorganisation,Institutionen för astronomi och teoretisk fysik - Genomgår omorganisation,Naturvetenskapliga fakulteten,Lund Observatory - Undergoing reorganization,Department of Astronomy and Theoretical Physics - Undergoing reorganization,Faculty of Science4 aut0 (Swepub:lu)astr-ilu
710	2	a Astronomi - Genomgår omorganisationb Institutionen för astronomi och teoretisk fysik - Genomgår omorganisation4 org
773	0	t Astronomy and Astrophysicsd : EDP Sciencesg 421, s. 969-976q 421<969-976x 1432-0746x 0004-6361
856	4	u https://portal.research.lu.se/files/4704775/624411.pdfx primaryx freey FULLTEXT
856	4	u http://dx.doi.org/10.1051/0004-6361:20035957y FULLTEXT
856	4	u https://www.aanda.org/articles/aa/pdf/2004/27/aa0957.pdf
856	4 8	u https://lup.lub.lu.se/record/134119
856	4 8	u https://doi.org/10.1051/0004-6361:20035957

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Av författaren/redakt...: Bensby, Thomas; Feltzing, Sofia; Lundström, Ingem ...

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