Toward an understanding of the globular cluster overabundance around the central giant elliptical galaxy NGC 1399

We investigate the kinematics of a combined sample of 74 globular clusters around NGC 1399. Their high velocity dispersion, increasing with radius, in dicates their association with the gravitational potential of the galaxy cl uster rather than with that of NGC 1399 itself. We find no evidence for rot ation in the full sample, although there is some indication of rotation in the outer regions. The data do not allow us to detect differences between t he kinematics of the blue and red subpopulations of globular clusters. A co mparison of the globular cluster systems of NGC 1399 and those of NGC 1404 and NGC 1380 indicates that the globular clusters in all three galaxies are likely to have formed via similar mechanisms and at similar epochs. The on ly property that distinguishes the NGC 1399 globular cluster system from th ese others is that it is 10 times more abundant. We summarize the evidence for associating these excess globular clusters with the galaxy cluster rath er than with NGC 1399 itself and suggest that the overabundance can be expl ained by tidal stripping, at an early epoch, of neighboring galaxies and su bsequent accumulation of globular clusters in the gravitational potential o f the galaxy cluster.