@article{7bd4c1bf6f5546fab888e22d3e3aed90,
title = "Galactic archaeology with asteroseismology and spectroscopy: Red giants observed by CoRoT and APOGEE",
abstract = "With the advent of the space missions CoRoT and Kepler, it has recently become feasible to determine precise asteroseismic masses and relative ages for large samples of red giant stars. We present the CoRoGEE dataset, obtained from CoRoT light curves for 606 red giants in two fields of the Galactic disc that have been co-observed by the Apache Point Observatory Galactic Evolution Experiment (APOGEE). We used the Bayesian parameter estimation code PARAM to calculate distances, extinctions, masses, and ages for these stars in a homogeneous analysis, resulting in relative statistical uncertainties of ≤ 2% in distance, ∼4% in radius, ∼9% in mass and ∼25% in age. We also assessed systematic age uncertainties stemming from different input physics and mass loss. We discuss the correlation between ages and chemical abundance patterns of field stars over a broad radial range of the Milky Way disc (5 kpc <RGal< 14 kpc), focussing on the [α/Fe]-[Fe/H]-age plane in five radial bins of the Galactic disc. We find an overall agreement with the expectations of pure chemical-evolution models computed before the present data were available, especially for the outer regions. However, our data also indicate that a significant fraction of stars now observed near and beyond the solar neighbourhood migrated from inner regions. Mock CoRoGEE observations of a chemodynamical Milky Way disc model indicate that the number of high-metallicity stars in the outer disc is too high to be accounted for even by the strong radial mixing present in the model. The mock observations also show that the age distribution of the [α/Fe]-enhanced sequence in the CoRoGEE inner-disc field is much broader than expected from a combination of radial mixing and observational errors. We suggest that a thick-disc/bulge component that formed stars for more than 3 Gyr may account for these discrepancies. Our results are subject to future improvements due to (a) the still low statistics, because our sample had to be sliced into bins of Galactocentric distances and ages; (b) large uncertainties in proper motions (and therefore guiding radii); and (c) corrections to the asteroseismic mass-scaling relation. The situation will improve not only upon the upcoming Gaia data releases, but also with the foreseen increase in the number of stars with both seismic and spectroscopic information.",
keywords = "Asteroseismology, Galaxy: abundances, Galaxy: disk, Galaxy: evolution, Stars: fundamental parameters",
author = "F. Anders and C. Chiappini and Rodrigues, {T. S.} and A. Miglio and J. Montalb{\'a}n and B. Mosser and L. Girardi and M. Valentini and A. Noels and T. Morel and Johnson, {J. A.} and M. Schultheis and F. Baudin and {De Assis Peralta}, R. and S. Hekker and N. Theme{\ss}l and T. Kallinger and Garc{\'i}a, {R. A.} and S. Mathur and A. Baglin and Santiago, {B. X.} and M. Martig and I. Minchev and M. Steinmetz and {Da Costa}, {L. N.} and Maia, {M. A.G.} and Prieto, {C. Allende} and K. Cunha and Beers, {T. C.} and C. Epstein and P{\'e}rez, {A. E.Garc{\'i}a} and Garc{\'i}a-Hern{\'a}ndez, {D. A.} and P. Harding and J. Holtzman and Majewski, {S. R.} and Sz M{\'e}sz{\'a}ros and D. Nidever and K. Pan and M. Pinsonneault and Schiavon, {R. P.} and Schneider, {D. P.} and Shetrone, {M. D.} and K. Stassun and O. Zamora and G. Zasowski",
note = "Funding Information: TSR acknowledges support from CNPq-Brazil. B.M., F.B., R.P. and R.A.G. acknowledge financial support from the ANR program IDEE Interaction Des {\'E}toiles et des Exoplan{\`e}tes. J.M. acknowledges support from the ERC Consolidator Grant funding scheme (project STARKEY, G.A. No. 615604). L.G. and T.S.R. acknowledge partial support from PRIN INAF 2014 - CRA 1.05.01.94.05. T.M. acknowledges financial support from Belspo for contract PRODEX Gaia-DPAC. A.E.G.P., C.A.P., D.A.G.H., and O.Z. acknowledge support provided by the Spanish Ministry of Economy and Competitiveness (MINECO) under grants AYA2014- 56359-P, RYC-2013-14182, and AYA-2014-58082-P. T.C.B. acknowledges partial support from grant PHY 14-30152 (Physics Frontier Center/JINA-CEE) awarded from the US National Science Foundation. S.a.M. acknowledges support from the NASA grant NNX12AE17G. S.z.M. has been supported by the J{\'a}nos Bolyai Research Scholarship of the Hungarian Academy of Sciences. The research leading to the presented results has received funding from the European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement No. 338251 (StellarAges). Funding for the SDSS-III 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 U.S. Department of Energy Office of Science. Publisher Copyright: {\textcopyright} ESO, 2016.",
year = "2017",
month = jan,
day = "1",
doi = "10.1051/0004-6361/201527204",
language = "English (US)",
volume = "597",
journal = "Astronomy and Astrophysics",
issn = "0004-6361",
publisher = "EDP Sciences",
}