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Cores of relaxed galaxy clusters are often disturbed by AGN. Their Chandraobservations revealed a wealth of structures induced by shocks, subsonic gasmotions, bubbles of relativistic plasma, etc. In this paper, we determine thenature and energy content of gas fluctuations in the Perseus core by probingstatistical properties of emissivity fluctuations imprinted in the soft- andhard-band X-ray images. About 80 per cent of the total variance ofperturbations on ~ 8-70 kpc scales in the inner region have an isobaric nature,i.e., are consistent with slow displacements of the gas in pressure equilibriumwith ambient medium. Observed variance translates to the ratio of non-thermalto thermal energy of ~13 per cent. In the region dominated by weak "ripples",about half of the total variance is also associated with isobaric perturbationson scales ~ a few tens of kpc. If these isobaric perturbations are induced bybuoyantly rising bubbles, then these results suggest that most of theAGN-injected energy should first go into bubbles rather than into shocks. Usingsimulations of a shock propagating through the Perseus atmosphere, we foundthat models reproducing the observed features of a central shock have more than50 per cent of the AGN-injected energy associated with the bubble enthalpy andonly about 20 per cent is carried away with the shock. Such energy partition isconsistent with the AGN-feedback model, mediated by bubbles of relativisticplasma, and supports the importance of turbulence in the balance between gasheating and radiative cooling.

The nature and energetics of AGN-driven perturbations in the hot gas in the Perseus Cluster