  We studied the metal-poor globular cluster (GC) populations of a large
variety of galaxies (47 galaxies spanning about 10mag in absolute brightness)
and compared their mean [Fe/H] with the properties of the host galaxies. The
mean [Fe/H] of the systems lie in the -1.65<[Fe/H]<-1.20 range (74% of the
population). Using only GC systems with more than 6 objects detected, 85% of
the population lie within -1.65<[Fe/H]<-1.20. The relation between the mean
[Fe/H] of the metal-poor GC systems and the Mv of their host galaxies presents
a very low slope which includes zero. An analysis of the correlation of the
mean [Fe/H] with other galaxy properties also leads to the conclusion that no
strong correlation exists. The lack of correlation suggests a formation of all
metal-poor GC in similar gas fragments. A weak correlation might exist between
mean [Fe/H] of the metal-poor GC and host galaxy metallicity. This would imply
that some fragments in which metal-poor GC formed were already embedded in the
larger dark matter halo of the final galaxy (as oppose to being independent
satellites that were accreted later). Our result suggests a homogeneous
formation of metal-poor GC in all galaxies, in typical fragments of masses
around 10^9-10^10 solar masses with very similar metallicities, compatible with
hierarchical formation scenarios for galaxies. We compared the mean [Fe/H] of
the metal-poor GC populations with the typical metallicities of high-z objects.
If we add the constraint that GC need a high column density of gas to form,
DLAs are the most likely sites for the formation of metal-poor GC populations.
