Properties of Globular Clusters in Galaxy Clusters: Sensitivity from the Formation and Evolution of Globular Clusters

We investigate the properties of globular clusters (GCs) in a galaxy cluster, using the particle tagging method with a semianalytical approach in a cosmological context. We assume GCs form from dark matter halo mergers and their metallicity is assigned based on the stellar mass of the host dark matter halos and the formation redshift of GCs. Dynamical evolution and disruption of GCs are considered using semianalytical approaches, controlled by several free parameters. In this paper, we investigate how our results are changed by the choice of free parameters. We compare our fiducial results with representative observations, including the mass ratio between the GC system and its host galaxy, the GC occupancy, the number fraction of blue GCs, and the metallicity gradient with the GC mass. Because we can know the positions of GCs with time, comparison with additional observations is possible, e.g., the median radii of the GC system in individual galaxies, the mean projected density profiles of intracluster GCs, and the metallicity and age gradients of GCs with a clustercentric radius. We also find that the specific mass of the GC system in each galaxy is different with a clustercentric radius.