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