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We introduce the SAPP (Stellar Abundances and atmospheric ParametersPipeline), the prototype of the code that will be used to determine parametersof stars observed within the core program of the PLATO space mission. Thepipeline is based on the Bayesian inference and provides effective temperature,surface gravity, metallicity, chemical abundances, and luminosity. The code inits more general version can have a much wider range of applications. It canalso provide masses, ages, and radii of stars and can be used for stars ofstellar types not targeted by the PLATO core program, such as red giants. Wevalidate the code on a set of 27 benchmark stars that includes 19 FGK-typedwarfs, 6 GK-type sub-giants, and 2 red giants. Our results suggest thatcombining various observables is the optimal approach, as it allows to breakdegeneracies between different parameters and yields more accurate values ofstellar parameters and more realistic uncertainties. For the PLATO core sample,we obtain a typical uncertainty of 27 ($\rm{syst.}$) $\pm$ 37 ($\rm{stat.}$) Kfor T$_{\rm{eff}}$, 0.00 $\pm$ 0.01 dex for log$g$, 0.02 $\pm$ 0.02 dex formetallicity [Fe/H], -0.01 $\pm$ 0.03 R$_\odot$ for radii, -0.01 $\pm$ 0.05M$_\odot$ for stellar masses, and -0.14 $\pm$ 0.63 Gyrs for ages. We also showthat the best results are obtained by combining the $\nu_{max}$ scalingrelation and stellar spectra. This resolves the notorious problem ofdegeneracies, which is particularly important for F-type stars.

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