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Vertical distribution of Galactic disk stars IV - AMR and AVR from clump giants

hal.structure.identifierObservatoire aquitain des sciences de l'univers [OASU]
hal.structure.identifierLaboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux [L3AB]
hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
dc.contributor.authorSOUBIRAN, C.
hal.structure.identifierObservatoire astronomique de Strasbourg [OAS]
dc.contributor.authorBIENAYME, O.
hal.structure.identifierAstronomical observatory of Odessa National University [Odessa]
hal.structure.identifierOdessa Astronomical Observatory
dc.contributor.authorMISHENINA, T. V.
hal.structure.identifierAstronomical observatory of Odessa National University [Odessa]
hal.structure.identifierOdessa Astronomical Observatory
dc.contributor.authorKOVTYUKH, V. V.
dc.date.issued2008
dc.identifier.issn0004-6361
dc.description.abstractEnWe present the parameters of 891 stars, mostly clump giants, including atmospheric parameters, distances, absolute magnitudes, spatial velocities, galactic orbits and ages. One part of this sample consists of local giants, within 100 pc, with atmospheric parameters either estimated from our spectroscopic observations at high resolution and high signal-to-noise ratio, or retrieved from the literature. The other part of the sample includes 523 distant stars, which we have estimated atmospheric parameters from high resolution but low signal-to-noise Echelle spectra. This new sample is kinematically unbiased, with well-defined boundaries in magnitude and colours. We revisit the basic properties of the Galactic thin disk as traced by clump giants. We find the metallicity distribution to be different from that of dwarfs, with less metal-rich stars. We find evidence for a vertical metallicity gradient of -0.31 dex/kpc and for a transition at 4-5 Gyr in both the metallicity and velocities. The age - metallicity relation (AMR), which exhibits a very low dispersion, increases smoothly from 10 to 4 Gyr, with a steeper increase for younger stars. The age-velocity relation (AVR) is characterized by the saturation of the V and W dispersions at 5 Gyr, and continuous heating in U.
dc.language.isoen
dc.publisherEDP Sciences
dc.subject.enStars: kinematics
dc.subject.enStars: fundamental parameters
dc.subject.enGalaxy: disk
dc.subject.enGalaxy: structure
dc.subject.enSolar neighbourhood
dc.title.enVertical distribution of Galactic disk stars IV - AMR and AVR from clump giants
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361:20078788
dc.subject.halPhysique [physics]/Astrophysique [astro-ph]/Cosmologie et astrophysique extra-galactique [astro-ph.CO]
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.page91-101
bordeaux.volume480
bordeaux.peerReviewedoui
hal.identifierhal-00256881
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-00256881v1
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