We numerically investigate the kinematic properties of globular cluster systems ( GCSs ) in E/S0 galaxies formed from dissipationless merging of spiral galaxies .
The metal-poor globular clusters ( MPCs ) and metal-rich clusters ( MRCs ) in the merger progenitors are initially assumed to have spatial distributions consistent with the Milky Way GC system .
Our principal results , which can be tested against observations , are as follows .
Both MPCs and MRCs in elliptical galaxies formed from major mergers can exhibit significant rotation at large radii ( \sim 20 kpc ) due to the conversion of initial orbital angular momentum into intrinsic angular momentum of the remnant .
MPCs show higher central velocity dispersions than MRCs for most major merger models . V _ { m } / { \sigma } _ { 0 } ( where V _ { m } and { \sigma } _ { 0 } , are the GCS maximum rotational velocity and central velocity dispersion of respectively ) ranges from 0.2– 1.0 and 0.1–0.9 for the MPCs and MRCs respectively , within 6 R _ { e } for the remnant elliptical .
For most merger remnant ellipticals , V _ { m } / { \sigma } _ { 0 } of GCSs within 6 R _ { e } is greater than that of the field stars within 2 R _ { e } .
The radial profiles of rotational velocities and velocity dispersions of the GCSs depend upon the orbital configuration of the merger progenitors , their mass-ratios , and the viewing angle .
For example , more flattened early-type galaxies , formed through mergers with small mass ratios ( \sim 0.1 ) , show little rotation in the outer MRCs .
Two-dimensional ( 2D ) velocity dispersion distributions of the GCSs of merger remnant ellipticals are generally flattened for both MPCs and MRCs , reflecting the fact that the GCSs have anisotropic velocity dispersions .
The 2D distributions of line-of-sight-velocity of the GCSs in some remnant ellipticals show minor-axis rotation , particularly for MRCs .
The kinematic properties of MPCs in merger remnant ellipticals strongly resemble those of the surrounding dark matter .
This implies that the kinematics of MPCs in such galaxies can be used to probe the kinematic properties of their dark matter halos .
We discuss these results in the context of GC and galaxy formation .
We note a possible difference in the GC kinematics between field and cluster Es and explain how GC kinematics may help us understand the origin of S0 galaxies .