Prompted by a new catalogue of M31 globular clusters , we have collected together individual metallicity values for globular clusters in the Local Group .
Although we briefly describe the globular cluster systems of the individual Local Group galaxies , the main thrust of our paper is to examine the collective properties .
In this way we are simulating the dissipationless merger of the Local Group , into presumably an elliptical galaxy .
Such a merger is dominated by the Milky Way and M31 , which appear to be fairly typical examples of globular cluster systems of spiral galaxies .

The Local Group ‘ Elliptical ’ has about 700 \pm 125 globular clusters , with a luminosity function resembling the ‘ universal ’ one .
The metallicity distribution has peaks at [ Fe/H ] \sim –1.55 and –0.64 with a metal–poor to metal–rich ratio of 2.5:1 .
The specific frequency of the Local Group Elliptical is initially about 1 but rises to about 3 , when the young stellar populations fade and the galaxy resembles an old elliptical .
The metallicity distribution and stellar population corrected specific frequency are similar to that of some known early type galaxies .
Based on our results , we briefly speculate on the origin of globular cluster systems in galaxies .