On the Galactic chemical evolution of sulfur

¹ Uppsala Astronomical Observatory, Box 515, 751 20 Uppsala, Sweden
² Department of Astronomy, University of Texas, Austin, TX 78712-1083, USA

Corresponding author: N. Ryde, ryde@astro.uu.se

Received: 21 May 2003
Accepted: 12 November 2003

Abstract

Sulfur abundances have been determined for ten stars to resolve a debate in the literature on the Galactic chemical evolution of sulfur in the halo phase of the Milky Way. Our analysis is based on observations of the S i lines at 9212.9, 9228.1, and 9237.5 Å for stars for which the S abundance was obtained previously from much weaker S i lines at 8694.0 and 8694.6 Å. In contrast to the previous results showing [S/Fe] to rise steadily with decreasing [Fe/H], our results show that [S/Fe] is approximately constant for metal-poor stars () at . Thus, sulfur behaves in a similar way to the other α elements, with an approximately constant [S/Fe] for metallicities lower than . We suggest that the reason for the earlier claims of a rise of [S/Fe] is partly due to the use of the weak S i 8694.0 and 8694.6 Å lines and partly uncertainties in the determination of the metallicity when using Fe i lines. The S i 9212.9, 9228.1, and 9237.5 Å lines are preferred for an abundance analysis of sulfur for metal-poor stars.