  The dynamics of globular cluster systems (GCSs) around galaxies are often
used to assess the total enclosed mass, and even to constrain the dark matter
distribution. The globular cluster system of a galaxy is typically assumed to
be in dynamical equilibrium within the potential of the host galaxy. However
cluster galaxies are subjected to a rapidly evolving and, at times, violently
destructive tidal field. We investigate the impact of the harassment on the
dynamics of GCs surrounding early type cluster dwarfs, using numerical
simulations. We find that the dynamical behaviour of the GCS is strongly
influenced by the fraction of bound dark matter f_{DM} remaining in the galaxy.
Only when f_{DM} falls to ~15%, do stars and GCs begin to be stripped. Still
the observed GC velocity dispersion can be used to measure the true enclosed
mass to within a factor of 2, even when f_{DM} falls as low as ~3%. This is
possible partly because unbound GCs quickly separate from the galaxy body.
However even the distribution of {\it{bound}} GCs may spatially expand by a
factor of 2-3. Once f_{DM} falls into the <3% regime, the galaxy is close to
complete disruption, and GCS dynamics can no longer be used to reliably
estimate the enclosed mass. In this regime, the remaining bound GCS may
spatially expand by a factor of 4 to 8. It may be possible to test if a galaxy
is in this regime by measuring the dynamics of the stellar disk. We demonstrate
that if a stellar disk is rotationally supported, it is likely that a galaxy
has sufficient dark matter, that the dynamics of the GCS can be used to
reliably estimate the enclosed mass.
