The SAPP pipeline for the determination of stellar abundances and atmospheric parameters of stars in the core program of the PLATO mission - Archive ouverte HAL
Article Dans Une Revue Astronomy & Astrophysics - A&A Année : 2022

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

Maria Bergemann
  • Fonction : Auteur
Aldo Serenelli
  • Fonction : Auteur
Luca Casagrande
  • Fonction : Auteur
Jeffrey M. Gerber
  • Fonction : Auteur
Ulrike Heiter
  • Fonction : Auteur
Mikhail Kovalev
  • Fonction : Auteur
Thierry Morel
Nicolas Nardetto
Vardan Adibekyan
Víctor Silva Aguirre
  • Fonction : Auteur
Martin Asplund
  • Fonction : Auteur
Carlos del Burgo
  • Fonction : Auteur
Lionel Bigot
  • Fonction : Auteur
  • PersonId : 830491
Andrea Chiavassa
  • Fonction : Auteur
Jonay I. González Hernández
  • Fonction : Auteur
Denis Mourard
Thibault Merle
  • Fonction : Auteur
Szabolcs Mészáros
  • Fonction : Auteur
Douglas J. Marshall
  • Fonction : Auteur
Regner Trampedach
  • Fonction : Auteur
Maria Tsantaki
  • Fonction : Auteur

Résumé

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 temperature, surface gravity, metallicity, chemical abundances, and luminosity. The code in its more general version can have a much wider range of applications. It can also provide masses, ages, and radii of stars and can be used for stars of stellar types not targeted by the PLATO core program, such as red giants. We validate the code on a set of 27 benchmark stars that includes 19 FGK-type dwarfs, 6 GK-type sub-giants, and 2 red giants. Our results suggest that combining various observables is the optimal approach, as it allows to break degeneracies between different parameters and yields more accurate values of stellar parameters and more realistic uncertainties. For the PLATO core sample, we obtain a typical uncertainty of 27(syst.) ± 37 (stat.) K for T eff , 0.00 ± 0.01 dex for log g, 0.02 ± 0.02 dex for metallicity [Fe/H], −0.01 ± 0.03 R for radii, −0.01 ± 0.05 M for stellar masses, and −0.14 ± 0.63 Gyrs for ages. We also show that the best results are obtained by combining the ν max scaling relation and stellar spectra. This resolves the notorious problem of degeneracies, which is particularly important for F-type stars.
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Dates et versions

hal-03440305 , version 1 (22-11-2021)

Identifiants

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Matthew Raymond Gent, Maria Bergemann, Aldo Serenelli, Luca Casagrande, Jeffrey M. Gerber, et al.. The SAPP pipeline for the determination of stellar abundances and atmospheric parameters of stars in the core program of the PLATO mission. Astronomy & Astrophysics - A&A, 2022, 658, pp.A147. ⟨10.1051/0004-6361/202140863⟩. ⟨hal-03440305⟩
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