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Abstract
The radial distribution of globular clusters in our Galaxy, M 31 and M 87 is studied and compared with that of halo stars. The globular cluster distributions seem significantly flatter than those of the parent-galaxy stellar bulge. Assuming this is a consequence of an evolution of the globular cluster distribution in these galaxies, a comparison with the (unevolved) stellar distribution allows us to obtain estimates of the number and total mass of clusters lost. It results that the cluster systems in our Galaxy and in M 31 have been initially about one third richer than now, and twice as abundant in M 87. The estimated mass in form of globular clusters lost is compatible with the nucleus masses of these galaxies
