What fraction of the density fluctuations in the Perseus cluster core is due to gas sloshing rather than AGN feedback?

Citations Over TimeTop 20% of 2018 papers

Abstract

Deep Chandra observations of the core of the Perseus cluster show a plethora of complex structures. It has been found that when the observed density fluctuations in the intracluster medium are converted into constraints on AGN-induced turbulence, the resulting turbulent heating rates are sufficient to balance cooling locally throughout the central 220 kpc. However, while the signatures of AGN feedback (inflated bubbles) dominate the central 60 kpc in X-ray images, beyond this radius the intracluster medium is increasingly shaped by the effects of gas sloshing, which can also produce subtle variations in X-ray surface brightness. We use mock Chandra observations of gas sloshing simulations to investigate what fraction of the observed density fluctuations in the core of the Perseus galaxy cluster may originate from sloshing rather than AGN-induced feedback. Outside 60 kpc, we find that the observed level of the density fluctuations is broadly consistent with being produced by sloshing alone. If this is the case, AGN-generated turbulence is likely to be insufficient in combating cooling outside 60 kpc.

Related Papers

• → Bubbles, feedback and the intracluster medium: three-dimensional hydrodynamic simulations(2001)158 cited
• → Cooling of X-ray emitting gas by heat conduction in the center of cooling flow clusters(2004)20 cited
• → Precessing AGN Jets, Bubbles and Cooling Flows(2011)1 cited
• → Precessing AGN jets, bubbles and cooling flows(2010)
• → Cooling of X-ray Emitting Gas by Heat Conduction in the Center of Cooling Flow Clusters(2003)