  We have obtained intermediate-resolution VLT spectroscopy of 75 globular
cluster candidates around the Sa galaxy M104 (NGC4594). Fifty-seven candidates
out to ~ 40 kpc in the halo of the galaxy were confirmed to be bona-fide
globular clusters, 27 of which are new. A first analysis of the velocities
provides only marginal evidence for rotation of the cluster system. From Hbeta
line strengths, almost all of the clusters in our sample have ages that are
consistent, within the errors, with Milky Way globular clusters. Only a few
clusters may be 1-2 Gyr old, and bulge and halo clusters appear coeval. The
absorption line indices follow the correlations established for the Milky Way
clusters. Metallicities are derived based upon new empirical calibrations with
Galactic globular clusters taking into account the non-linear behavior of some
indices (e.g., Mg2). Our sample of globular clusters in NGC4594 spans a
metallicity range of -2.13 < [Fe/H] < +0.26 dex, and the median metallicity of
the system is [Fe/H] = -0.85. Thus, our data provide evidence that some of the
clusters have super-solar metallicity. Overall, the abundance distribution of
the cluster system is consistent with a bimodal distribution with peaks at
[Fe/H] ~- 1.7 and -0.7. However, the radial change in the metallicity
distribution of clusters may not be straightforwardly explained by a varying
mixture of two sub-populations of red and blue clusters.
