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We use the Millennium II cosmological simulation combined with thesemi-analytic galaxy formation model of Guo et al. (2011) to predict thecontribution of galactic nuclei formed by the tidal stripping of nucleateddwarf galaxies to globular cluster (GC) and ultra-compact dwarf galaxy (UCD)populations of galaxies. We follow the merger trees of galaxies in clustersback in time and determine the absolute number and stellar masses of disruptedgalaxies. We assume that at all times nuclei have a distribution innucleus-to-galaxy mass and nucleation fraction of galaxies similar to thatobserved in the present day universe. Our results show stripped nuclei follow amass function $N(M) \sim M^{-1.5}$ in the mass range $10^6 < M/M_\odot < 10^8$,significantly flatter than found for globular clusters. The contribution ofstripped nuclei will therefore be most important among high-mass GCs and UCDs.For the Milky Way we predict between 1 and 3 star clusters more massive than$10^5 M_\odot$ come from tidally disrupted dwarf galaxies, with the mostmassive cluster formed having a typical mass of a few times $10^6 M_\odot$,like omega Centauri. For a galaxy cluster with a mass $7 \times 10^{13}M_\odot$, similar to Fornax, we predict $\sim$19 UCDs more massive than$2\times10^6 M_\odot$ and $\sim$9 UCDs more massive than $10^7 M_\odot$ withina projected distance of 300 kpc come from tidally stripped dwarf galaxies. Theobserved number of UCDs are $\sim$200 and 23, respectively. We conclude thatmost UCDs in galaxy clusters are probably simply the high mass end of the GCmass function.

Contribution of stripped nuclear clusters to globular cluster and ultra-compact dwarf galaxy populations