  We studied and compared the radial profiles of globular clusters and of the
stellar bulge component in three galaxies of the Fornax cluster observed with
the WFPC2 of the HST. A careful comparative analysis of these distributions
confirms that stars are more concentrated toward the galactic centres than
globular clusters, in agreement with what was observed in many other galaxies.
If the observed difference is the result of evolution of the globular cluster
system sstarting from initial profiles similar to those of the halo--bulge
stellar components, a relevant fraction of their mass (74%, 47%, 52% for NGC
1379, NGC 1399 and NGC 1404, respectively) is disappeared in the inner regions,
likely contributing to the nuclear field population, local dynamics and high
energy phenomena in the primeval life of the galaxy. An indication in favour of
the evolutionary interpretation of the difference between the globular cluster
system and stellar bulge radial profiles is given by the positive correlation
we found between the value of the mass lost from the GCS and the central
galactic black hole mass in the set of seven galaxies for which these data are
available.
