Evidence for AGN Feedback in Galaxy Clusters and Groups
Figure 5
(a) Bolometric X-ray luminosities corrected for the effect of cooling flow in the central ~70 kpc versus emission-weighted temperatures derived excluding cooling flow components, from Markevitch [25]. The dashed line is the best-fit power law to the sample: . The red triangle and the blue square represent the measurements from the XMM-Newton and Chandra data of the giant cavity clusters MS [209] and Hydra A, respectively, corrected consistently with the method adopted by Markevitch [25]. (b) Temperature profiles measured for a sample of relaxed clusters presented by Vikhlinin et al. [79]. The temperatures are scaled to the cluster emission-weighted temperature excluding the central 70 kpc regions. The profiles for all clusters are projected and scaled in radial units of the virial radius , estimated from the relation [210]. Overlaid are the cooling flow corrected, scaled temperature profiles of the giant cavity clusters MS (red triangles, Gitti et al. [136]) and Hydra A (blue squares, Gitti et al. [120]).
