  From equivalent widths of the SI lines at 8694 A, Israelian & Rebolo (2001)
and Takada-Hidai et al. (2002) have derived a surprisingly high sulphur-to-iron
ratio ([S/Fe] = 0.5 to 0.7) in six halo stars with [Fe/H] ~ -2.0 suggesting
perhaps that hypernovae made a significant contribution to the formation of
elements in the early Galaxy. To investigate this problem we have used
high-resolution spectra obtained with the ESO VLT/UVES spectrograph to
determine the S/Fe ratio in 19 main-sequence and subgiant stars ranging in
[Fe/H] from -3.2 to -0.7. The sulphur abundances are determined from SI lines
at 8694 A and 9212 - 9237 A, and the iron abundances from about 20 FeII lines.
S/Fe ratios as derived from 1D model atmospheres are presented and possible 3D
effects are discussed. The initial results from our survey do not confirm the
high values of [S/Fe] quoted above; instead we find that the ratio [S/Fe]
remains constant at about 0.35 dex for metallicities -3 < [Fe/H] -1.
