We investigate structural properties of old , metal-poor globular clusters ( GCs ) formed at high redshifts ( z > 6 ) and located inside and outside virialized galaxy-scale halos in clusters of galaxies with the total masses of M _ { CL } based on high-resolution cosmological simulations with models of GC formation .
We mainly derive the parameter dependences of physical properties of intracluster GCs ( ICGCs ) based on the results of 14 cluster models .
Our principle results are summarized as follows .

( 1 ) ICGCs are formed as a result of tidal stripping of GCs initially within galaxy-scale halos during hierarchical growth of clusters via halo merging .
These ICGCs comprise 20-40 % of all GCs in clusters with 1.0 \times 10 ^ { 14 } { M } _ { \odot } \leq M _ { CL } \leq 6.5 \times 10 ^ { 14 } { M } _ { \odot } and the number fraction of ICGCs does not depend on M _ { CL } for the above cluster mass range .

( 2 ) The projected radial density profiles ( { \Sigma } _ { GC } ) of ICGCs in clusters with different M _ { CL } can be diverse , though ICGCs have inhomogeneous , asymmetric , and somewhat elongated distributions in most models .
If { \Sigma } _ { GC } ( R ) \propto R ^ { \alpha } , \alpha ranges from \approx - 1.5 to \approx - 2.5 for GCs in clusters with the above mass range .

( 3 ) Although total number of GCs within the central 0.05 Mpc ( N _ { GC, 0.05 } ) and 0.2 Mpc ( N _ { GC, 0.2 } ) are diverse in different clusters , they can depend weakly on M _ { CL } in such a way that both N _ { GC, 0.05 } and N _ { GC, 0.2 } are likely to be larger for clusters with larger M _ { CL } .

( 4 ) Total number of GCs per cluster masses ( specific frequency of GCs for clusters of galaxies ) are more likely to be larger in more massive clusters , mainly because a larger number of earlier virialized objects can be located in more massive clusters .

( 5 ) Radial density distributions of all GCs including ICGCs and galactic GCs have steeper profiles than those of the background dark matter halos in the central regions of clusters ( R < 200 kpc ) with different M _ { CL } .

( 6 ) Spatial distributions of old GCs in clusters can depend on the truncation epoch of GC formation ( z _ { trun } ) such that they can be steeper and more compact in the models with higher z _ { trun } .

( 7 ) The mean metallicity of ICGCs in a cluster can be smaller than that of GCs within the cluster member galaxy-scale halos by \sim 0.3 in [ Fe/H ] .
Metallicity distribution functions ( MDFs ) of ICGCs show peak values around [ Fe/H ] \sim - 1.6 and do not have remarkable bimodality .