  We investigate whether the globular clusters (GCs) in the recently published
sample of GCs in the Fornax cluster by Bergond and coworkers are indeed
intra-cluster objects. We combine the catalogue of radial velocity measurements
by Bergond et al. with our CTIO MOSAIC photometry in the Washington system and
analyse the relation of metal-poor and metal-rich GCs with their host galaxies.
The metal-rich GCs appear to be kinematically associated with their respective
host galaxies. The vast majority of the metal-poor GCs found in between the
galaxies of the Fornax cluster have velocities which are consistent with them
being members of the very extended NGC 1399 GC system. We find that when the
sample is restricted to the most accurate velocity measurements, the GC
velocity dispersion profile can be described with a mass model derived for the
NGC 1399 GC system within 80 kpc. We identify one ``vagrant'' GC whose radial
velocity suggests that it is not bound to any galaxy unless its orbit has a
very large apogalactic distance.
