Nearby star cluster formation: Probes of cosmological galaxy evolution

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(abridged) The old Star Cluster (SC) systems surrounding any sofar investigated galaxy represent a powerful tool for the understanding of the cosmological evolution of their host galaxies. Phases of enhanced cluster formation can be identified by reliably age dating the clusters. These are symptoms of violent star formation, results of intense starbursts as commonly seen in merging nearby galaxies and high-z forming galaxies. However, the young SC systems of nearby merging galaxies and the old SC systems of nearby passive galaxies (most likely resulting from high-z starburst events of these galaxies) appear to be significantly different in terms of their mass functions. Whether this difference originates in differences in the formation physics/environment or is only due to dynamical evolution of the cluster systems is currently a hot issue. A main diagnostic for the survival probability of a newly formed cluster is most likely its compactness, since less compact, fluffy clusters are more vulnerable to destructive interactions with the galactic environment of the cluster. For these reasons, we developed 1) a tool to significantly improve photometry of nearby SCs (which appear resolved on high-resolution images, provided e.g. by HST), by accurately measuring and taking the cluster size into account, and 2) a tool to effectively determine ages and masses (plus metallicities and extinctions) of SCs from multi-wavelength photometry, ranging from the UV to the NIR.