In this paper , we are exploring the properties of old , metal-poor globular clusters in galaxies .
We investigate whether their properties are related to the properties of their host galaxies , and whether we can constrain their formation .
The main result is that the mean metallicities of old GC systems are found to lie in a narrow range -1.7 < [ Fe/H ] < -1.1 ( 80 % of the population ) .
Moreover , no correlations are found between the mean metallicities and other galaxy properties which implies a GC formation independent of the host galaxies .
Further , we try to identify the sites of old , metal-poor GC formation , with any currently known high redshift objects .
We find that the metalicities of damped Ly \alpha systems in the redshift range 1.6 < z < 4 are consistent with our GC metalicities , which suggests that these high-density neutral gas objects may be the progenitors of the old , metal-poor globular clusters .