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The SAPP pipeline for the determination of stellar abundances and atmospheric parameters of stars in the core program of the PLATO mission

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  • Matthew Raymond Gent, Max Planck Institute for Astronomy
  • ,
  • Maria Bergemann, Max Planck Institute for Astronomy, University of Copenhagen
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  • Aldo Serenelli, Max Planck Institute for Astronomy, Institute of Space Studies of Catalonia, Institut d'Estudis Espacials de Catalunya (IEEC)
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  • Luca Casagrande, Australian National University
  • ,
  • Jeffrey M. Gerber, Max Planck Institute for Astronomy
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  • Ulrike Heiter, Uppsala University
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  • Mikhail Kovalev, Max Planck Institute for Astronomy, CAS - National Astronomical Observatories
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  • Thierry Morel, University of Liege
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  • Nicolas Nardetto, Observatoire de la Cote d'Azur
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  • Vardan Adibekyan, Eotvos Lorand University, University of Porto
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  • Víctor Silva Aguirre
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  • Martin Asplund, Max Planck Institute for Astrophysics
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  • Kevin Belkacem, LESIA, Observatoire de Paris
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  • Carlos Del Burgo, Instituto Nacional de Astrofisica Optica y Electronica, Instituto Astrofisico de Canarias
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  • Lionel Bigot, Observatoire de la Cote d'Azur
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  • Andrea Chiavassa, Observatoire de la Cote d'Azur
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  • Luisa Fernanda Rodríguez Díaz
  • Marie Jo Goupil, LESIA, Observatoire de Paris
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  • Jonay I.González Hernández, Instituto Astrofisico de Canarias, University of La Laguna
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  • Denis Mourard, Observatoire de la Cote d'Azur
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  • Thibault Merle, Université Libre de Bruxelles
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  • Szabolcs Mészáros, Eotvos Lorand University, MTA-ELTE Lendület Milky Way Research Group
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  • Douglas J. Marshall, Universite Toulouse III - Paul Sabatier, IRAP
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  • Rhita Maria Ouazzani, LESIA, Observatoire de Paris
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  • Bertrand Plez, Universite de Montpellier
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  • Daniel Reese, LESIA, Observatoire de Paris
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  • Regner Trampedach, Space Science Institute
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  • Maria Tsantaki, Osservatorio Astrofisico Di Arcetri, Florence

We introduce the SAPP (Stellar Abundances and atmospheric Parameters Pipeline)the prototype of the code that will be used to determine parameters of stars observed within the core program of the PLATO space mission. The pipeline is based on the Bayesian inference and provides effective temperaturesurface gravitymetallicitychemical abundancesand luminosity. The code in its more general version has a much wider range of potential applications. It can also provide massesagesand radii of stars and can be used with stellar types not targeted by the PLATO core programsuch as red giants. We validate the code on a set of 27 benchmark stars that includes 19 FGK-type dwarfs6 GK-type subgiantsand 2 red giants. Our results suggest that combining various observables is the optimal approachas this allows the degeneracies between different parameters to be broken and yields more accurate values of stellar parameters and more realistic uncertainties. For the PLATO core samplewe obtain a typical uncertainty of 27 (syst.) ± 37 (stat.) K for Teff0.00 ± 0.01 dex for log g0.02 ± 0.02 dex for metallicity [Fe/H]-0.01 ± 0.03 Rfor radii-0.01 ± 0.05 Mfor stellar massesand -0.14 ± 0.63 Gyr for ages. We also show that the best results are obtained by combining the νmaxscaling relation with stellar spectra. This resolves the notorious problem of degeneracieswhich is particularly important for F-type stars.

Original languageEnglish
Article numberA147
JournalAstronomy and Astrophysics
Volume658
ISSN0004-6361
DOIs
Publication statusPublished - Feb 2022

Bibliographical note

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    Research areas

  • stars: abundances, stars: atmospheres, stars: fundamental parameters, stars: solar-type, surveys

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