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Most ultra-compact dwarf galaxies (UCDs) and very massive globular clustersreside in nearby galaxy clusters or around nearby giant galaxies. Due to theirdistance (>Mpc) and compactness (r_eff<100pc) they are barely resolved, andthus it is difficult to obtain their internal properties. Here I present ourmost recent attempts to constrain the mass function, stellar content anddynamical state of UCDs in the Fornax cluster. Thanks to radial velocitymembership assignment of ~950 globular clusters (GCs) and UCDs in the core ofFornax, the shape of their mass function is well constrained. It is consistentwith the 'standard' Gaussian mass function of GCs. Our recent simulations onthe disruption process of nucleated dwarf galaxies in cluster environmentsshowed that ~40% of the most massive UCDs should originate from nuclear starclusters. Some Fornax UCDs actually show evidence for this scenario, asrevealed by extended low surface brightness disks around them and onsets oftidal tails. Multi-band UV to optical imaging as well as low to mediumresolution spectroscopy revealed that there exist UCDs with youngish ages,(sub-)solar [alpha/Fe] abundances, and probably He-enriched populations.

Stellar population properties of the most massive globular clusters and ultra-compact dwarf galaxies of the Fornax cluster