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We present a photometric analysis of the rich star cluster population in thetidal tails of NGC 6872. We find star clusters with ages between 1 - 100 Myrdistributed in the tidal tails, while the tails themselves have an age of lessthan 150 Myr. Most of the young massive ($10^{4} \le M/M_{\odot} \le 10^{7}$)clusters are found in the outer regions of the galactic disk or the tidaltails. The mass distribution of the cluster population can be well described bypower-law of the form $N(m) \propto m^{-\alpha}$, where $\alpha = 1.85 \pm0.11$, in very good agreement with other young cluster populations found in avariety of different environments. We estimate the star formation rate forthree separate regions of the galaxy, and find that the eastern tail is formingstars at $\sim 2$ times the rate of the western tail and $\sim 5$ times therate of the main body of the galaxy. By comparing our observations withpublished N-body models of the fate of material in tidal tails in a galaxycluster potential, we see that many of these young clusters will be lost intothe intergalactic medium. We speculate that this mechanism may also be at workin larger galaxy clusters such as Fornax, and suggest that the so-calledultra-compact dwarf galaxies could be the most massive star clusters that haveformed in the tidal tails of an ancient galactic merger.Comment: 12 pages, 10 figures, accepted A&

The star cluster population in the tidal tails of NGC 6872