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We study the assembly of globular clusters (GCs) in 9 galaxy clusters usingthe cosmological simulation Illustris. GCs are tagged to individual galaxies attheir infall time. The tidal removal of GCs from their galaxies and thedistribution of the GCs within the cluster is later followed self-consistentlyby the simulation. The method relies on the simple assumption of a singlepower-law relation between halo mass (M_vir) and mass in GCs (M_GC) as found inobservations. We find that the GCs specific frequency $S_N$ as a function ofV-band magnitude naturally reproduces the observed "U"-shape, due to thecombination of a power law M_GC-M_vir relation and the non-linear M_*-M_virrelation from the simulation. Additional scatter in the $S_N$ values are tracedback to galaxies with early infall times due to the evolution in the M_*-M_virrelation with redshift. GCs that have been tidally removed from their galaxiesform today the intra-cluster component from which about ~60% were brought in bygalaxies that orbit today within the cluster potential. The remaining "orphan"GCs are contributed by satellite galaxies with a wide range of stellar massesthat are fully tidally disrupted at z=0. This intra-cluster component is a gooddynamical tracer of the dark matter potential. As a consequence of the accretednature of most intra-cluster GCs, their orbits are fairly radial with apredicted orbital anisotropy \beta >= 0.5. However, local tangential motionsmay appear as a consequence of localized substructure, providing a possibleinterpretation to the \beta<0 values suggested in observations of M87.

Simulating the Spatial Distribution and Kinematics of Globular Clusters within Galaxy Clusters in Illustris