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 ( [ Fe/H ] <

\sim

-1 ) at [ S/Fe ] \simeq +0.3 .
Thus , sulfur behaves in a similar way to the other \alpha elements , with an approximately constant [ S/Fe ] for metallicities lower than \mathrm { [ Fe / H ] } \simeq - 1 .
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 .