Abundances of light elements in metal-poor stars. I. Atmospheric parameters and a new T_eff scale

TL;DR

This paper establishes a new effective temperature scale for metal-poor stars using a homogeneous iterative method, IRFM calibrations, and Kurucz models, improving atmospheric parameter accuracy for stellar abundance studies.

Contribution

It introduces a new eff\ scale based on IRFM and interferometric data, with improved consistency over previous models, especially for stars hotter than 4400 K.

Findings

New eff\ scale aligns well with IRFM and Hα estimates.

Kurucz models better predict solar limb darkening than OSMARCS.

Cooler metal-poor stars show low gravities, indicating possible model limitations.

Abstract

We present atmospheric parameters for about 300 stars of different chemical composition, whose spectra will be used to study the galactic enrichment of Fe and light elements. These parameters were derived using an homogenous iterative procedure, which considers new calibrations of colour-\teff\ relations for F, G and K-type stars based on Infrared Flux Method (IRFM) and interferometric diameters for population~I stars, and the Kurucz (1992) model atmospheres. We found that these calibrations yield a self-consistent set of atmospheric parameters for \teff$>4400$~K, representing a clear improvement over results obtained with older model atmospheres. Using this \teff-scale and Fe equilibrium of ionization, we obtained very low gravities (implying luminosities incompatible with that expected for RGB stars) for metal-poor stars cooler than 4400~K; this might be due either to a moderate Fe overionization (expected from statistical equilibrium calculations) or to inadequacy of Kurucz models to describe the atmospheres of very cool giants. Our \teff\ scale is compared with other scales recently used for metal-poor stars; it agrees well with those obtained using Kurucz (1992) models, but it gives much larger \teff's than those obtained using OSMARCS models (Edvardsson et al. 1993). This difference is attributed to the different treatment of convection in the two sets of models. For the Sun, the Kurucz (1992) model appears to be preferable to the OSMARCS ones because it better predicts the solar limb darkening; furthermore, we find that our photometric \teff's for metal-poor stars agree well with both direct estimates based on the IRFM, and with \teff's derived from H$\alpha$\ wings when using Kurucz models.