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The properties of globular cluster systems (GCSs) in the core of the nearbygalaxy clusters Fornax and Hydra I are presented. In the Fornax cluster we havegathered the largest radial velocity sample of a GCS system so far, whichenables us to identify photometric and kinematic sub-populations around thecentral galaxy NGC 1399. Moreover, ages, metallicities and [alpha/Fe]abundances of a sub-sample of 60 bright globular clusters (GCs) with high S/Nspectroscopy show a multi-modal distribution in the correlation space of thesethree parameters, confirming heterogeneous stellar populations in the halo ofNGC 1399. In the Hydra I cluster very blue GCs were identified. They are notuniformly distributed around the central galaxies. 3-color photometry includingthe U-band reveals that some of them are of intermediate age. Their locationcoincides with a group of dwarf galaxies under disruption. This is evidence ofa structurally young stellar halo 'still in formation', which is also supportedby kinematic measurements of the halo light that point to a kinematicallydisturbed system. The most massive GCs divide into generally more extendedultra-compact dwarf galaxies (UCDs) and genuine compact GCs. In both clusters,the spatial distribution and kinematics of UCDs are different from those ofgenuine GCs. Assuming that some UCDs represent nuclei of stripped galaxies, theproperties of those UCDs can be used to trace the assembly of nucleated dwarfgalaxies into the halos of central cluster galaxies. We show viasemi-analytical approaches within a cosmological simulation that only the mostmassive UCDs in Fornax-like clusters can be explained by stripped nuclei,whereas the majority of lower mass UCDs belong to the star cluster family.

Globular clusters as tracers of the halo assembly of nearby central cluster galaxies