Dynamical Simulations of the First Globular Clusters
  Tidally limited star clusters are started on nearly circular orbits in the
dark matter sub-halos present at high redshift and evolved with an n-body code
augmented with gravitational interactions in the clusters. The tidally removed
stars and the remaining high redshift clusters from a redshift 8 start are more
concentrated than the dark matter, as expected. However, the subset of stars
from the clusters that began in the lower mass sub-halos have a distribution
somewhat more extended than the dark matter halo, with a mean galactic radius
of about 60 kpc inside 150 kpc. The clusters from low mass sub-halos, those
with a peak circular velocity of $ 12-18$ \kms, also produce most of the
population's thin stellar streams. The dependence of the stellar population
distribution on sub-halo mass is not seen in simulations that start clusters at
lower redshift. The half mass radii of the clusters are set by the tidal fields
of the initial cluster orbits, which leads to the average half mass radius
decreasing with increased redshift of formation. Starting clusters at greater
than redshift 4 leads to cluster half mass radii approximately as seen in the
Milky Way, with lower redshifts leading to clusters that are too large. If
extremely metal poor globular clusters were preferentially formed in high
redshift, low mass, dwarf galaxies, then the clusters should be spread nearly
uniformly over the dark halo, along with their tidally removed stars.
