  We present our work on the halo evolution of sulfur, based on observations of
the S I lines around 9220 A for ten stars for which the S abundance was
obtained previously from much weaker S I lines at 8694 A. We cannot confirm the
rise and the high [S/Fe] abundances for low [Fe/H], as claimed in the
literature from analysis of the 8694 A lines. The reasons for claims of an
increase in [S/Fe] with decreasing [Fe/H] are probably twofold: uncertainties
in the measurements of the weak 8694 A lines, and systematic errors in
metallicity determinations from Fe I lines. The near-infrared sulfur triplet at
9212.9, 9228.1, and 9237.5 A are preferred for an abundance analysis of sulfur
for metal-poor stars. Our work was presented in full by Ryde & Lambert (2004).
