2005A&A...443.1029K

We investigate the debated ``sulphur discrepancy'' found among metal-poor stars of the Galactic halo with [Fe/H]←2. This discrepancy stems in part from the use of two different sets of sulphur lines, the very weak triplet at 8694-95Å and the stronger triplet lines at 9212-9238Å. For three representative cases of metal-poor dwarf, turnoff and subgiant stars, we argue that the abundances from the λλ8694-95 lines have been overestimated which has led to a continually rising trend of [S/Fe] as metallicity decreases. Given that the near-IR region is subject to CCD fringing, these weak lines become excessively difficult to measure accurately in the metallicity regime of [Fe/H]←2. Based on homogeneously determined spectroscopic stellar parameters, we also present updated [S/Fe] ratios from the λλ9212-9238 lines which suggest a plateau-like behaviour similar to that seen for other alpha elements.