The Sombrero galaxy , NGC 4594 , contains the most numerous globular cluster system of any nearby spiral .
It is an ideal candidate in which to study the globular clusters and contrast them with those in Local Group spirals .
Here we present B and I imaging from the CTIO Schmidt telescope which gives a field-of-view of 31 ^ { { } ^ { \prime } } \times 31 ^ { { } ^ { \prime } } .
Using DAOPHOT we have detected over 400 globular clusters and derived their magnitudes , B–I colors and photometric metallicities .
We have attempted to separate our sample into disk and bulge/halo globular cluster populations , based on location in the galaxy .
There is some evidence that the disk population is more metal–rich than the bulge/halo globular clusters , however contamination , dust reddening and small number statistics makes this result very tentative .
We find that the median metallicity of the bulge/halo globular clusters is [ Fe/H ] = –0.8 .
This metallicity is consistent with previous estimates based on smaller samples .
It is also similar to the metallicity predicted by the globular cluster metallicity – galaxy luminosity relation .
As with our Galaxy , there is no radial metallicity gradient in the halo globular clusters .
This suggests that the spheriodal component of NGC 4594 did not form by a dissipational process .