Formation and Evolution of
Galaxy Clusters Across Cosmic Time

The increasing amount and quality of observational data on Globular Clusters (GCs) nowadays allows placing further constraints on the formation pathways of GCs. An interesting feature found in many GC populations is a bimodality in color and metallicity: metal-poor, blue GCs, and metal-rich, red GCs. Their typically different spatial distributions throughout galaxies indicate distinct formation histories of the GC subpopulations. In this research, we developed an empirical model for the numbers and ages of GCs in galaxies that is consistent with recent data from massive elliptical galaxies down to the dwarf galaxy regime. It demonstrates how the need of models with two separate GC formation mechanisms arises from various single formation pathway models. This poster presents some properties of single formation models, as well as how a set of dual formation models improves on them and leads to better agreement with observations with respect to GC abundances and ages.