Gas rotation in galaxy clusters: signatures and detectability in X-rays
  We study simple models of massive galaxy clusters in which the intracluster
medium (ICM) rotates differentially in equilibrium in the cluster gravitational
potential. We obtain the X-ray surface brightness maps, evaluating the isophote
flattening due to the gas rotation. Using a set of different rotation laws, we
put constraint on the amplitude of the rotation velocity, finding that rotation
curves with peak velocity up to \sim 600 km s^-1 are consistent with the
ellipticity profiles of observed clusters. We convolve each of our models with
the instrument response of the X-ray Calorimeter Spectrometer on board the
ASTRO-H to calculate the simulated X-ray spectra at different distance from the
X-ray centre. We demonstrate that such an instrument will allow us to measure
rotation of the ICM in massive clusters, even with rotation velocities as low
as \sim 100 km s^-1
