Simulating Globular Clusters in Dark Matter Sub-Halos
  A cosmological zoom-in simulation which develops into a Milky Way-like halo
is started at redshift 7. The initial dark matter distribution is seeded with
dense star clusters, median mass $5\times 10^5 M_\sun$, placed in the largest
sub-halos present, which have a median peak circular velocity of 25 \kms. Three
simulations are initialized using the same dark matter distribution, with the
star clusters started on approximately circular orbits having initial median
radii 6.8 kpc, 0.14 kpc, and, at the exact center of the sub-halos. The
simulations are evolved to the current epoch at which time the median galactic
orbital radii of the three sets of clusters are 30, 5 and 16 kpc, with the
clusters losing about 2, 50 and 15\% of their mass, respectively. Clusters
started at small orbital radii have so much tidal forcing that they are often
not in equilibrium. Clusters started at larger sub-halo radii have a velocity
dispersion that declines smoothly to $\simeq$20\% of the central value at
$\simeq$20 half mass radii. The clusters started at the sub-halo centers can
show a rise in velocity dispersion beyond 3-5 half mass radii. That is, the
clusters formed without local dark matter always have stellar mass dominated
kinematics at all radii, whereas about 25\% of the clusters started at sub-halo
centers have remnant local dark matter.
