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We use the hydrodynamical EAGLE simulation to predict the numbers, masses andradial distributions of tidally stripped galaxy nuclei in massive galaxyclusters, and compare these results to observations of ultra-compact dwarfgalaxies (UCDs) in the Virgo cluster. We trace the merger trees of galaxies inmassive galaxy clusters back in time and determine the numbers and masses ofstripped nuclei from galaxies disrupted in mergers. The spatial distribution ofstripped nuclei in the simulations is consistent with those of UCDs surroundingmassive galaxies in the Virgo cluster. Additionally, the numbers of strippednuclei are consistent with the numbers of M > $10^{7}~M_{\odot}$ UCDs aroundindividual galaxies and in the Virgo cluster as a whole. The mass distributionsin this mass range are also consistent. We find that the numbers of strippednuclei surrounding individual galaxies correlates better with the stellar orhalo mass of individual galaxies than the total cluster mass. We conclude thatmost high mass (M > $10^{7}~M_{\odot}$ UCDs are likely stripped nuclei. It isdifficult to draw reliable conclusions about low mass (M < $10^{7}~M_{\odot}$UCDs because of observational selection effects. We additionally predict that afew hundred stripped nuclei below a mass of $2~\times~10^{6}~M_{\odot}$ shouldexist in massive galaxies that will overlap in mass with the globular clusterpopulation. Approximately 1-3 stripped nuclei in the process of forming alsoexist per massive galaxy.

Contribution of stripped nuclei to the ultracompact dwarf galaxy population in the Virgo Cluster