The kinematics of Small Magellanic Cloud star clusters

We report results of proper motions 25 known Small Magellanic Cloud (SMC) clusters (ages ~ 1 - 10 Gyr old) derived from Gaia EDR3 data sets. When these mean are gathered with existent radial velocity measurements to compose the clusters' vectors, we found parameter values a rotation disk that best resemble their observed motions, namely: central coordinates and distance, inclination position angle line-of-node, motion in right ascension declination systemic velocity, dispersion. The SMC cluster seems be at some level kinematically synchronized field red giants recently modeled using DR2 Such is seen sky as tilted edge-on disk, dispersion perpendicular it twice big plane disk. Because direction nearly aligned Bridge, interpret larger consequence stretching caused by tidal interaction Large Cloud. Rotation alone would not seem sufficient explain kinematic behaviors SMC.