Kinematic differences between multiple populations in Galactic globular clusters

The formation process of multiple populations in globular clusters is still up for debate. Kinematic differences between the are particularly interesting this respect, because they allow us to distinguish single-epoch scenarios and multi-epoch scenarios. We analyze kinematics 25 aim find kinematic constrain their process. split red-giant branch (RGB) stars each cluster into three (P1, P2, P3) type-II two (P1 P2) otherwise using Hubble photometry. derive rotation dispersion profiles its by all with radial velocity measurements obtained from MUSE spectroscopy. Based on these profiles, we calculate strength terms ordered-over-random motion $\left(v/\sigma\right)_\mathrm{HL}$ evaluated at half-light radius cluster. detect but four clusters. For NGC~104, NGC~1851, NGC~2808, NGC~5286, NGC~5904, NGC~6093, NGC~6388, NGC~6541, NGC~7078 NGC~7089 also P1 and/or P2 stars. NGC~6093 that larger than $1\sigma$. Whereas rotates faster NGC~7078, opposite true NGC~2808. However, even clusters, low significance. a generally scales median relaxation time. corresponding relation very weak best. observe no correlation difference stellar velocities analysis based made publicly available.