We report on sulphur abundances in halo stars as derived from near-IR UVES spectra. The importance of removing telluric lines and residual CCD fringing patterns by using early B-type stars as calibrators is emphasized. Comparison of data from the weak λ8694.6 and the stronger λ9212.9,9237.5 pair of S I lines provides important constraints on non-LTE effects. We do not confirm the high sulphur abundances reported by others for some metal-poor stars; our results instead indicate that sulphur behaves like other typical α-capture elements with a plateau at [S/Fe] ∼ + 0.3 dex in the Galactic halo. © 2008 Springer-Verlag Berlin Heidelberg.
CITATION STYLE
Nissen, P. E., Akerman, C., Asplund, M., Fabbian, D., & Pettini, M. (2008). Sulphur abundances in metal-poor stars. In ESO Astrophysics Symposia (Vol. 2008, pp. 51–54). https://doi.org/10.1007/978-3-540-75485-5_12
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