Astrophysical tests of atomic data important for stellar Mg abundance determinations

Abstract: Magnesium abundances of cool stars with different metallicities are important for understanding the galactic chemical evolution. This study tests atomic data used in stellar magnesium abundance analyses. We evaluate non-local thermodynamical equilibrium (NLTE) line formation for Mg I using the most up-to-date theoretical and experimental atomic data available so far and check the Mg abundances from individual lines in the Sun, four well studied A-type stars, and three reference metal-poor stars. With the adopted gf-values, NLTE abundances derived from the Mg I 4703 A, 5528 A, and Mg Ib lines are consistent within 0.05 dex for each A-type star. The same four Mg I lines in the solar spectrum give consistent NLTE abundances at $\log N_{\rm Mg}/N_{\rm H} = -4.45$, when correcting the van der Waals damping constants inferred from the perturbation theory. Inelastic Mg+H collisions as treated by Barklem, Belyaev, Spielfiedel, Guitou, and Feautrier serve as efficient thermalizing process for the statistical equilibrium of Mg I in the atmospheres of metal-poor stars. The use of the Mg+H collision data improves Mg abundance determinations for HD 84937 and HD 122563, though does not remove completely the differences between different lines.