tangential profiles, we find positive values of $\Delta V_{\rm TAN}$ over the entire analyzed radial interval, thus favouring rotation among all the studied populations of $\omega\,$Centauri and M22. The tangential profiles of Fe-poor and Fe-rich stars in $\omega\,$Centauri exhibit their maximum amplitudes of about 6 km s$^{-1}$ at radial distances of about one half-light radii and steadily decrease towards larger distances from the cluster center. In the case of M22 both populations are consistent with a flat tangential profile in the analyzed radial interval. Our data do not allow to determine whether the rotation pattern of M22 strongly differs from that of $\omega$Centauri, or if the apparent flat rotation of M22 is due to the lack of observations in the external regions.

To compare the average velocity profiles of stellar populations we used the same procedure described in @cordoni2019 [see their Section 5]. We first used the Anderson-Darling (A-D) test to estimate the probability, $p$, that the tangential and radial motions of Fe-poor and Fe-rich stars are drawn from the same parent population. Furthermore, we compared the observed velocity profiles of Fe-poor and Fe-rich stars with $N_{\rm sim}=1000$ velocity profiles of simulated Fe-poor and Fe-rich stars. We assumed that the 