of their orbits, at least half of the known Type II GCs (seven out thirteen clusters) are associated with the Enceladus Galaxy thus demonstrating their extragalactic origin [@milone2020].

Remarkably, the evidence that both metal-rich and metal-poor stars of most Type II GCs host stellar populations with different light-element abundances [e.g. @marino2009; @marino2011], indicates that independent processes are responsible for the heavy-element enrichment and for the variation of light elements. Insights on the formation processes can be gained via the study of the kinematics of stellar populations with different chemical compositions.

Indeed, the various scenarios on the formation of multiple populations in GCs, suggest that second-generation stars are born in the cluster center, in a high density subsystem embedded in a more-extended first generation [@dercole2008; @calura2019 and references therein]. $N$-body simulations [e.g. @mastrobuono2013; @mastrobuono2016; @vesperini2013; @henault2015; @tiongco2019] demonstrate that the dynamical evolution of second-generation stars should be significantly different from that of the first generation and the signature of the different initial conditions could be detected in present-day GC kinematics of GCs where the stars are not fully mixed. Hence, the present-day dynamics of stellar populations with different metallicities and light-element abundances provide a unique window into the origin of multiple 