Stellar envelopes of globular clusters embedded in dark mini-haloes
  We show that hard encounters in the central regions of globular clusters
embedded in dark matter (DM) haloes necessarily lead to the formation of
gravitationally-bound stellar envelopes that extend far beyond the nominal
tidal radius of the system. Using statistical arguments and numerical
techniques we derive the equilibrium distribution function of stars ejected
from the centre of a non-divergent spherical potential. Independently of the
velocity distribution with which stars are ejected, GC envelopes have density
profiles that approach asymptotically $\rho\sim r^{-4}$ at large distances and
become isothermal towards the centre. Adding a DM halo component leaves two
clear-cut observational signatures: (i) a flattening, or slightly increase of
the projected velocity dispersion profile at large distances, and (ii) an outer
surface density profile that is systematically shallower than in models with no
dark matter.
