Formation imprints in the kinematics of the Milky Way globular cluster
  system
  We report results on the kinematics of Milky Way (MW) globular clusters (GCs)
based on updated space velocities for nearly the entire GC population. We found
that a 3D space with the semi-major axis, the eccentricity and the inclination
of the orbit with respect to the MW plane as its axes is helpful in order to
dig into the formation of the GC system. We find that GCs formed in-situ show a
clear correlation between their eccentricities and their orbital inclination in
the sense that clusters with large eccentricities also have large inclinations.
These GCs also show a correlation between their distance to the MW center and
their eccentricity. Accreted GCs do not exhibit a relationship between
eccentricity and inclination, but span a wide variety of inclinations at
eccentricities larger than ~ 0.5. Finally, we computed the velocity anisotropy
"beta" of the GC system and found for GCs formed in-situ that "beta" decreases
from ~ 0.8 down to 0.3 from the outermost regions towards the MW center, but
remains fairly constant (0.7-0.9) for accreted ones. These findings can be
explained if GCs formed from gas that collapsed radially in the outskirts, with
preference for relative high infall angles. As the material reached the
rotating forming disk, it became more circular and moved with lower inclination
relative to the disk. A half of the GC population was accreted and deposited in
orbits covering the entire range of energies from the outer halo to the bulge.
