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Detection of the copious amount of X-ray emission from the dilute hot plasmain galaxy clusters suggests that a substantial fraction of the centralintracluster medium (ICM) is cooling radiatively on a time scale much fasterthan the Hubble time. Theoretical models predict the cooling rate as high asabout few hundred to few thousand solar mass per year, which would be then madeavailable for the formation of new stars in the core of these clusters.However, systematic studies of the cores of such clusters failed to detect theexpected reservoirs of cooled gas. Thus, the gas in the cores of galaxyclusters is losing substantial amount of energy in the form of X-rays but isnot cooling. This in turn point towards the famous cooling flow paradox andhence demands some intermittent heating to balance the cooling over such a longperiod. Several sources have been suggested to counteract on the cooling of theICM, however, the AGN feedback appeared to be the most promising and enoughenergetic source to resist cooling of the ICM in the cores of such clusters. Inthis presentation I will provide a brief overview on the feedback processesthat are involved in the cores of the galaxy clusters with an emphasis on theAGN feedback and its observable signatures.

Accretion powered AGN feedback in the cores of galaxy clusters