par Jofré, Paula;Worley, Clare C.C.;Bergemann, Maria;Lind, Karin;Masseron, Thomas ;Soubiran, Caroline;Blanco, Stéphane S.;Heiter, Ulrike;Nordlander, Thomas;Hill, Vanessa;De Laverny, Patrick;Recio-Blanco, Alejandra;Pancino, Elena;Lardo, C.;Cantat-Gaudin, Tristan;Sordo, Rosanna;Vallenari, Antonella;Magrini, Laura;González Hernández, Jonay J.I.;Van Eck, Sophie ;Montes, Davíd R P D.;Tabernero, Hugo;Mucciarelli, Alessio;Sobeck, Jennifer;Sousa, Sérgio S.G.
Référence Astronomy & astrophysics, 564, A133
Publication Publié, 2014
Référence Astronomy & astrophysics, 564, A133
Publication Publié, 2014
Article révisé par les pairs
Résumé : | Context. To calibrate automatic pipelines that determine atmospheric parameters of stars, one needs a sample of stars, or "benchmark stars", with well-defined parameters to be used as a reference. Aims. We provide detailed documentation of the iron abundance determination of the 34 FGK-type benchmark stars that are selected to be the pillars for calibration of the one billion Gaia stars. They cover a wide range of temperatures, surface gravities, and metallicities. Methods. Up to seven different methods were used to analyze an observed spectral library of high resolutions and high signal-to-noise ratios. The metallicity was determined by assuming a value of effective temperature and surface gravity obtained from fundamental relations; that is, these parameters were known a priori and independently from the spectra. Results. We present a set of metallicity values obtained in a homogeneous way for our sample of benchmark stars. In addition to this value, we provide detailed documentation of the associated uncertainties. Finally, we report a value of the metallicity of the cool giant ψ Phe for the first time. © ESO, 2014. |