We investigate the kinematics of a combined sample of 74 globular clusters
around NGC 1399. Their high velocity dispersion, increasing with radius,
supports their association with the gravitational potential of the galaxy
cluster rather than with that of NGC 1399 itself. We find no evidence for
rotation in the full sample, although some indication for rotation in the outer
regions. The data do not allow us to detect differences between the kinematics
of the blue and red sub-populations of globular clusters.
A comparison between 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 only property which distinguishes the NGC 1399 globular cluster
system from these others is that it is ten times more abundant. We summarize
the evidence for associating these excess globulars with the galaxy cluster
rather than with NGC 1399 itself, and suggest that the over-abundance can be
explained by tidal stripping, at an early epoch, of neighboring galaxies and
subsequent accumulation of globulars in the gravitational potential of the
galaxy cluster.Comment: AJ accepted (March issue), 27 pages (6 figures included), AAS style,
two columns. Also available at http://www.eso.org/~mkissle