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dc.contributor.authorAnders, Friedrichpt_BR
dc.contributor.authorChiappini, C.C.M.pt_BR
dc.contributor.authorSantiago, Basilio Xavierpt_BR
dc.contributor.authorRocha-Pinto, H.J.pt_BR
dc.contributor.authorGirardi, Leo Albertopt_BR
dc.contributor.authorCosta, Luiz N. dapt_BR
dc.contributor.authorMaia, Marcio Antonio Geimbapt_BR
dc.contributor.authorSteinmetz, M.pt_BR
dc.contributor.authorMinchev, Ivanpt_BR
dc.contributor.authorSchultheis, Mathiaspt_BR
dc.contributor.authorBoeche, Corradopt_BR
dc.contributor.authorMiglio, Andreapt_BR
dc.contributor.authorMontalbán, Josefinapt_BR
dc.contributor.authorSchneider, D.P.pt_BR
dc.contributor.authorBeers, T.C.pt_BR
dc.contributor.authorCunha, Katiapt_BR
dc.contributor.authorAllende Prieto, Carlospt_BR
dc.contributor.authorBalbinot, Eduardopt_BR
dc.contributor.authorBizyaev, D.pt_BR
dc.contributor.authorBrauer, Dorothéept_BR
dc.contributor.authorBrinkmann, Jonpt_BR
dc.contributor.authorFrinchaboy, P.M.pt_BR
dc.contributor.authorGarcía Pérez, Ana Eliapt_BR
dc.contributor.authorHayden, Michaelpt_BR
dc.contributor.authorHearty, Frederick R.pt_BR
dc.contributor.authorHoltzman, J.A.pt_BR
dc.contributor.authorJohnson, J.A.pt_BR
dc.contributor.authorKinemuchi, Karenpt_BR
dc.contributor.authorMajewski, Steven Raymondpt_BR
dc.contributor.authorMalanushenko, E.pt_BR
dc.contributor.authorMalanushenko, V.pt_BR
dc.contributor.authorNidever, D.L.pt_BR
dc.contributor.authorO'Connell, Robert Westpt_BR
dc.contributor.authorPan, K.pt_BR
dc.contributor.authorRobin, A.C.pt_BR
dc.contributor.authorSchiavon, Ricardo P.pt_BR
dc.contributor.authorShetrone, M.pt_BR
dc.contributor.authorSkrutskie, M.F.pt_BR
dc.contributor.authorSmith, Verne V.pt_BR
dc.contributor.authorStassun, Keivan G.pt_BR
dc.contributor.authorZasowski, G.pt_BR
dc.date.accessioned2015-06-02T02:00:09Zpt_BR
dc.date.issued2014pt_BR
dc.identifier.issn0004-6361pt_BR
dc.identifier.urihttp://hdl.handle.net/10183/117404pt_BR
dc.description.abstractContext. The Apache Point Observatory Galactic Evolution Experiment (APOGEE) features the first multi-object high-resolution fiber spectrograph in the near-infrared ever built, thus making the survey unique in its capabilities: APOGEE is able to peer through the dust that obscures stars in the Galactic disc and bulge in the optical wavelength range. Here we explore the APOGEE data included as part of the Sloan Digital Sky Survey’s 10th data release (SDSS DR10). Aims. The goal of this paper is to a) investigate the chemo-kinematic properties of the Milky Way disc by exploring the first year of APOGEE data; and b) to compare our results to smaller optical high-resolution samples in the literature, as well as results from lower resolution surveys such as the Geneva-Copenhagen Survey (GCS) and the RAdial Velocity Experiment (RAVE). Methods. We select a high-quality (HQ) sample in terms of chemistry (amounting to around 20 000 stars) and, after computing distances and orbital parameters for this sample, we employ a number of useful subsets to formulate constraints on Galactic chemical and chemodynamical evolution processes in the solar neighbourhood and beyond (e.g., metallicity distributions – MDFs, [α/Fe] vs. [Fe/H] diagrams, and abundance gradients). Results. Our red giant sample spans distances as large as 10 kpc from the Sun. Given our chemical quality requirements, most of the stars are located between 1 and 6 kpc from the Sun, increasing by at least a factor of eight the studied volume with respect to the most recent chemodynamical studies based on the two largest samples obtained from RAVE and the Sloan Extension for Galactic Understanding and Exploration (SEGUE). We find remarkable agreement between the MDF of the recently published local (d < 100 pc) high-resolution high-S/N HARPS sample and our local HQ sample (d < 1 kpc). The local MDF peaks slightly below solar metallicity, and exhibits an extended tail towards [Fe/H] = 􀀀1, whereas a sharper cuto is seen at larger metallicities (the APOGEE sample shows a slight overabundance of stars with metallicities larger than ≃+0.3 with respect to the HARPS sample). Both samples also compare extremely well in an [α/Fe] vs. [Fe/H] diagram. The APOGEE data also confirm the existence of a gap in the abundance diagram. When expanding our sample to cover three di erent Galactocentric distance bins (inner disc, solar vicinity and outer disc), we find the high-[α/Fe] stars to be rare towards the outer zones (implying a shorter scale-length of the thick disc with respect to the thin disc), as previously suggested in the literature. Finally, we measure the gradients in [Fe/H] and [α/Fe], and their respective MDFs, over a range of 6 < R < 11 kpc in Galactocentric distance, and a 0 < z < 3 kpc range of distance from the Galactic plane. We find a good agreement with the gradients traced by the GCS and RAVE dwarf samples. For stars with 1:5 < z < 3 kpc (not present in the previous samples), we find a positive metallicity gradient and a negative gradient in [α/Fe].en
dc.format.mimetypeapplication/pdfpt_BR
dc.language.isoengpt_BR
dc.relation.ispartofAstronomy and astrophysics. Les Ulis. Vol. 564 (Apr. 2014), A115, 24 p.pt_BR
dc.rightsOpen Accessen
dc.subjectStars: abundancesen
dc.subjectGalaxiapt_BR
dc.subjectGalaxy: generalen
dc.subjectCinemáticapt_BR
dc.subjectGalaxy: disken
dc.subjectGalaxy: abundancesen
dc.subjectGalaxy: evolutionen
dc.subjectStars: kinematics and dynamicsen
dc.titleChemodynamics of the Milky Way I. The first year of APOGEE datapt_BR
dc.typeArtigo de periódicopt_BR
dc.identifier.nrb000966519pt_BR
dc.type.originEstrangeiropt_BR


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