N-poor stars. In $\omega\,$Centauri both stellar groups are radially anisotropic. Interestingly, N-rich, Fe-rich stars exhibit different rotation patterns than N-poor stars with similar metallicities. The stellar populations with different nitrogen of M22 exhibit similar rotation patterns and isotropic motions. We discuss these findings in the context of the formation of multiple populations.'
author:
- 'G.Cordoni'
- 'A. P.Milone'
- 'A. F.Marino'
- 'G. S.Da Costa'
- 'E.Dondoglio'
- 'H.Jerjen'
- 'E. P.Lagioia'
- 'A. Mastrobuono-Battisti'
- 'J. E.Norris'
- 'M.Tailo'
- 'D.Yong'
title: 'Gaia and Hubble unveil the kinematics of stellar populations in the Type II globular clusters $\omega$Centauri and M22.'
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Introduction {#sec:intro}
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An increasing amount of research is providing evidence for the presence of two main classes of GCs [e.g. @marino2009; @marino2019; @milone2017]. While stars in the majority of Type I Galactic GCs exhibit homogeneous abundances of heavy elements [e.g. @carretta2009a], a small but significant number of ‘anomalous’ clusters (Type II GCs) show internal variations in metallicity and in those elements that are associated to $s$ processes [e.g. @yong2008; @dacosta2009; @yong2014; @marino2015; @johnson2015; @marino2019].

Type II GCs exhibit distinctive photometric features, including multimodal sub-giant branches (SGBs) in Color-Magnitude Diagrams (CMDs) made with optical filters [e.g. @milone2008; @marino2009; 