Milky Way globular cluster dynamics: are they preferentially
  co-rotating?
  The motion of the baryonic components of the Milky Way is governed by both
luminous and dark matter content of the Galaxy. Thus, the dynamics of the Milky
Way globular clusters can be used as tracers to infer the mass model of the
Galaxy up to a large radius. In this work, we use the directly observable
line-of-sight velocities to test if the dynamics of the globular cluster
population is consistent with an assumed axisymmetric gravitational potential
of the Milky Way. For this, we numerically compute the phase space distribution
of the globular cluster population where the orbits are either oriented
randomly or co-/counter- rotating with respect to the stellar disk. Then we
compare the observed position and line-of-sight velocity distribution of $\sim$
150 globular clusters with that of the models. We found that, for the adopted
mass model, the co-rotating scenario is the favored model based on various
statistical tests. We do the analysis with and without the GCs associated to
the progenitors of early merger events. This analysis can be extended in the
near future to include precise and copious data to better constrain the
Galactic potential up to a large radius.
