  We have determined the total numbers and specific frequencies of blue,
metal-poor globular clusters (GCs) in eight spiral and early-type galaxies.
These data, along with five measurements from the literature, show a trend of
increasing blue GC specific frequency with increasing mass of the host galaxy.
The increase is not accounted for in a simple galaxy formation model in which
ellipticals and their GC systems are formed by the merger of typical spiral
galaxies. The data appear broadly consistent with hierarchical formation
scenarios in which metal-poor GCs are formed over a finite period in the early
Universe during the initial stages of galaxy assembly. In this picture, the
observed trend is related to biasing, in the sense that the more massive
galaxies of today began assembling earlier and therefore formed relatively more
GCs during this early epoch of metal-poor GC formation. We discuss how
comparisons of the observed specific frequency of metal-poor GCs with model
calculations can constrain the formation redshift of these objects.
