3D core kinematics of NGC$~$6362: central rotation in a dynamically
  evolved globular cluster
  We present a detailed 3D kinematic analysis of the central regions ($R<30''$)
of the low-mass and dynamically evolved galactic globular cluster NGC 6362. The
study is based on data obtained with ESO-VLT/MUSE used in combination with the
adaptive optics module and providing $\sim3000$ line-of-sight radial
velocities, which have been complemented with Hubble Space Telescope proper
motions. The quality of the data and the number of available radial velocities
allowed us to detect for the first time a significant rotation signal along the
line of sight in the cluster core with amplitude of $\sim 1$ km/s and with a
peak located at only $\sim20''$ from the cluster center, corresponding to only
$\sim10\%$ of the cluster half-light radius. This result is further supported
by the detection of a central and significant tangential anisotropy in the
cluster innermost regions. This is one of the most central rotation signals
ever observed in a globular cluster to date. We also explore the rotational
properties of the multiple populations hosted by this cluster and find that
Na-rich stars rotate about two times more rapidly than the Na-poor
sub-population thus suggesting that the interpretation of the present-day
globular cluster properties require a multi-component chemo-dynamical approach.
Both the rotation amplitude and peak position would fit qualitatively the
theoretical expectations for a system that lost a significant fraction of its
original mass because of the long-term dynamical evolution and interaction with
the Galaxy. However, to match the observations more quantitatively further
theoretical studies to explore the initial dynamical properties of the cluster
are needed.
