Orbiting globular clusters formed in dark matter mini-halos
  We seek to differentiate dynamical and morphological attributes between
globular clusters that were formed inside their own dark matter mini-halo, and
those who were not. For that, we employ high resolution $N$-body simulations of
globular clusters with (and without) an enveloping dark matter mini-halo,
orbiting a host galaxy. We set the same prescriptions of the Fornax dwarf
spheroidal galaxy and its main five globular clusters, and use $N$-body
particles for all components (i.e., stars and dark matter, for both Fornax and
its clusters). For clusters embedded in dark matter, we observe that the
increment of mass from the extra dark component triggers a tidal radius growth
that allows the mini-halo to work as a protective shield against tidal
stripping, being itself stripped beforehand the stars. Consequently, tidal
effects such as inflation of the stellar velocity dispersion, development of
prominent tidal tails, ellipticity increase and diffusion of the stellar
distribution profile are generally much milder in clusters originally embedded
in dark matter. However, this shielding effect becomes negligible after an
important amount of dark matter has been stripped, which happens faster for
clusters having simultaneously short orbital periods, low typical orbital radii
and relatively high eccentricities. Finally, we notice that even for clusters
that retain a large amount of dark matter at redshift zero, their inner regions
are still predominantly composed of stars, with the typical density ratio of
dark matter to cluster stars being of the order of $1\%$ up to roughly $10~$pc
away from the clusters' centre.
