populations in Type II GCs.\
In recent papers, we exploited Gaia Data Release 2 [DR2, @gaia2018a] proper motions to investigate the kinematics of stellar populations with different light-element abundances of TypeI GCs [@milone2018; @cordoni2019]. We find that multiple stellar populations of various GCs, NGC0288, NGC6121, NGC6752 and NGC6838, share similar internal kinematics and morphology, in contrast with what is observed in NGC104, NGC5904 and NGC6254. Indeed, when we select the main groups of N-poor and N-rich stars (called first and second population, respectively) we find that both populations of NGC104 share similar rotation patterns in the central region and hints of different rotation in the cluster outskirts [Figure 10 in @cordoni2019]. Moreover, N-rich stars of NGC104 exhibit show stronger radial anisotropies than the first population [@milone2018; @cordoni2019 see their Figure 5 and 10, respectively]. The rotation curves of N-poor and N-rich stars of NGC5904 seem to exhibit different phases with a statistical significance of $\sim$2.5$\sigma$ [@cordoni2019 see their Figure 8] and N-rich stars of NGC5904 and exhibit higher ellipiticy than N-poor ones, in close analogy with what is observed in NGC6254 [@cordoni2019 Figure 5 and 6].

Here, we extend the analysis to the Type II GCs $\omega\,$Centauri, and NGC6656 (M22), 