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We present a study on the coherent rotation of the intracluster medium anddark matter components of simulated galaxy clusters extracted from avolume-limited sample of the MUSIC project. The set is re-simulated with threedifferent recipes for the gas physics: $(i)$ non-radiative, $(ii)$ radiativewithout AGN feedback, and $(iii)$ radiative with AGN feedback. Our analysis isbased on the 146 most massive clusters identified as relaxed, 57 per cent ofthe total sample. We classify these objects as rotating and non-rotatingaccording to the gas spin parameter, a quantity that can be related to clusterobservations. We find that 4 per cent of the relaxed sample is rotatingaccording to our criterion. By looking at the radial profiles of their specificangular momentum vector, we find that the solid body model is not a suitabledescription of rotational motions. The radial profiles of the velocity of thedark matter show a prevalence of the random velocity dispersion. Instead, theintracluster medium profiles are characterized by a comparable contributionfrom the tangential velocity and the dispersion. In general, the dark mattercomponent dominates the dynamics of the clusters, as suggested by thecorrelation between its angular momentum and the gas one, and by the lack ofrelevant differences among the three sets of simulations.

On the coherent rotation of diffuse matter in numerical simulations of galaxy clusters