@article{2b2070b1ddee4d25b63e76953e3ea710,
title = "Chemodynamics of the Milky Way I. The first year of APOGEE data",
abstract = "Context. 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 cutoff 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 different 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].",
author = "F. Anders and C. Chiappini and Santiago, {B. X.} and Rocha-Pinto, {H. J.} and L. Girardi and {Da Costa}, {L. N.} and Maia, {M. A.G.} and M. Steinmetz and I. Minchev and M. Schultheis and C. Boeche and A. Miglio and J. Montalb{\'a}n and Schneider, {D. P.} and Beers, {T. C.} and K. Cunha and {Allende Prieto}, C. and E. Balbinot and D. Bizyaev and Brauer, {D. E.} and J. Brinkmann and Frinchaboy, {P. M.} and {Garc{\'i}a P{\'e}rez}, {A. E.} and Hayden, {M. R.} and Hearty, {F. R.} and J. Holtzman and Johnson, {J. A.} and K. Kinemuchi and Majewski, {S. R.} and E. Malanushenko and V. Malanushenko and Nidever, {D. L.} and O'Connell, {R. W.} and K. Pan and Robin, {A. C.} and Schiavon, {R. P.} and M. Shetrone and Skrutskie, {M. F.} and Smith, {V. V.} and K. Stassun and G. Zasowski",
note = "Funding Information: It is a pleasure to thank R.-D. Scholz for helpful discussions on astrometry, and J. Bovy & K. Schlesinger for their valuable input on the discussion. Furthermore, we thank J. Bovy for making his code publicly available. T.C.B. acknowledges partial support from grant PHY 08-22648; Physics Frontier Center/JINA, awarded by the US National Science Foundation. K.C. acknowledges support from the National Science Foundation (AST-0907873). P.M.F. is supported by an NSF grant AST-1311835. Funding for the Brazilian Participation Group has been provided by the Minist{\'e}rio de Ci{\^e}ncia e Tecnologia (MCT), Funda{\c c}{\~a}o Carlos Chagas Filho de Amparo {\`a} Pesquisa do Estado do Rio de Janeiro (FAPERJ), Conselho Nacional de Desenvolvimento Cient{\'i}fico e Tecnol{\'o}gico (CNPq), and Financiadora de Estudos e Projetos (FINEP). Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the US Department of Energy Office of Science. The SDSS-III web site is http://www.sdss3.org/. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrof{\'i}sica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. Funding Information: Acknowledgements. It is a pleasure to thank R.-D. Scholz for helpful discussions on astrometry, and J. Bovy & K. Schlesinger for their valuable input on the discussion. Furthermore, we thank J. Bovy for making his code publicly available. T.C.B. acknowledges partial support from grant PHY 08-22648; Physics Frontier Center/JINA, awarded by the US National Science Foundation. K.C. acknowledges support from the National Science Foundation (AST-0907873). P.M.F. is supported by an NSF grant AST-1311835. Funding for the Brazilian Participation Group has been provided by the Minist{\'e}rio de Ci{\^e}ncia e Tecnologia (MCT), Funda{\c c}{\~a}o Carlos Chagas Filho de Amparo {\`a} Pesquisa do Estado do Rio de Janeiro (FAPERJ), Conselho Nacional de Desenvolvimento Cient{\'i}fico e Tecnol{\'o}gico (CNPq), and Financiadora de Estudos e Projetos (FINEP). Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the US Department of Energy Office of Science. The SDSS-III web site is http://www. sdss3.org/. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrof{\'i}sica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. Publisher Copyright: {\textcopyright} ESO 2014.",
year = "2014",
doi = "10.1051/0004-6361/201323038",
language = "English (US)",
volume = "564",
journal = "Astronomy and Astrophysics",
issn = "0004-6361",
publisher = "EDP Sciences",
}