  We present new metallicity estimates for globular cluster (GC) candidates in
the Sd spiral NGC 300, one of the nearest spiral galaxies outside the Local
Group. We have obtained optical spectroscopy for 44 Sculptor Group GC
candidates with the Boller and Chivens (B&C) spectrograph on the Baade
Telescope at Las Campanas Observatory. There are 2 GCs in NGC 253 and 12
objects in NGC 300 with globular-cluster-like spectral features, 9 of which
have radial velocities above 0 km/s. The remaining three, due to their radial
velocities being below the expected 95% confidence limit for velocities of NGC
300 halo objects, are flagged as possible foreground stars. The non-clusterlike
candidates included 13 stars, 15 galaxies, and an HII region. One GC, four
galaxies, two stars, and the HII region from our sample were identified in
archival Hubble Space Telescope images. For the GCs, we measure spectral
indices and estimate metallicities using an empirical calibration based on
Milky Way GCs. The GCs of NGC 300 appear similar to those of the Milky Way.
Excluding possible stars and including clusters from the literature, the GC
system (GCS) has a velocity dispersion of 68 km/s, and has no clear evidence of
rotation. The mean metallicity for our full cluster sample plus one literature
object is [Fe/H] = -0.94, lying above the relationship between mean GC
metallicity and overall galaxy luminosity. Excluding the three low-velocity
candidates, we obtain a mean [Fe/H] = -0.98, still higher than expected,
raising the possibility of significant foreground star contamination even in
this sample. Visual confirmation of genuine GCs using high-resolution
space-based imagery could greatly reduce the potential problem of interlopers
in small samples of GCSs in low-radial-velocity galaxies.
