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The determination of characteristic amplitudes and anisotropy of hot gasmotions in galaxy clusters from observations of the brightest resonance linesis discussed. Gas motions affect (i) the spectral line shape through theDoppler effect and (ii) the radial surface brightness profiles in lines duringresonant scattering. Radiative transfer calculations have been performed by theMonte Carlo method in the FeXXV resonance line at 6.7 eV for the Perseuscluster (Abell426). It was shown that (a) radial motions reduce the scatteringefficiency much more dramatically than purely tangential motions; (b)large-scale gas motions weakly affect the scattering efficiency. Theuncertainty in measuring the characteristics of gas motions using resonantscattering has been estimated for existing and future observations of clusters.

Resonant scattering in galaxy clusters for anisotropic gas motions on various spatial scales