  The photometric study of the Sagittarius dwarf galaxy by Marconi et al (1998)
has suggested the presence of a spread in metallicity (-0.7< [Fe/H] < -1.6),
which may result from different bursts of star formation. We present the
results from a Multi Object Slit spectroscopy program carried out at the NTT
with the aim to determine spectroscopic abundances of Sagittarius giants
selected from the CCD photometry. From our intermediate resolution (R about
1500) spectra radial velocities are determined to confirm the membership and
metallicities are derived by using spectral synthesis codes for stars down to V
about18, i.e. below the RGB clump. Out of 57 observed stars 23 have a radial
velocity consistent with Sagittarius membership, here we present results for 8
of these. No star with [Fe/H]<-1.0 is found, three stars are found to be
metal-rich.
