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We implemented non-solar-scaled opacities in a simultaneous derivation offundamental parameters and abundances. We carried out a high-precision stellarparameters and abundance determination by applying non-solar-scaled opacitiesand model atmospheres. Our sample is composed by 20 stars includingmain-sequence and evolved objects. Opacities for an arbitrary composition andvmicro were calculated through the Opacity Sampling method. We obtained a smalldifference in stellar parameters derived with non-solar-scaled opacitiescompared to classical solar-scaled models. The differences in Teff, log g and[Fe/H] amount up to 26 K, 0.05 dex and 0.020 dex for the stars in our sample.These differences could be considered as the first estimation of the error dueto the use of classical solar-scaled opacities to derive stellar parameterswith solar-type and evolved stars. Some chemical species could also show anindividual variation higher than those of the [Fe/H] (up to 0.03 dex) andvarying from one specie to another, obtaining a chemical pattern differencebetween both methods. This means that condensation temperature Tc trends couldalso present a variation. We include an example showing that usingnon-solar-scaled opacities, the classical solution cannot always verify theexcitation and ionization balance conditions required for a model atmosphere.We consider that the use of the non-solar-scaled opacities is not mandatory inevery statistical study with large samples of stars. However, for thosehigh-precision works whose results depend on the mutual comparison of differentchemical species (such as Tc trends), we consider that it is worthwhile itsapplication. To date, this is probably one of the more precise spectroscopicmethods of stellar parameters derivation [abridged].

Using non-solar-scaled opacities to derive stellar parameters. Toward high-precision parameters and abundances