SIMBAD references

We make the first estimate of non-gravitational energy profiles in galaxy cluster cores (and beyond) based on observational data. Comparing the observed entropy profiles within r₅₀₀, from the Representative XMM-Newton Cluster Structure Survey to simulated base entropy profiles without feedback from both adaptive mesh refinement (AMR) and smoothed particle hydrodynamic (SPH) non-radiative simulations, we estimate the amount of additional non-gravitational energy, E_ICM, contained in the intracluster medium (ICM), as well as the total energy feedback, E_Feedback, from active galactic nuclei (AGNs; the central AGNs in most cases) into the clusters. The total feedback energy scales with the mean spectroscopic temperature as E_Feedback ∝ T_sp^2.52±0.008 and E_Feedback ∝ T_sp^2.17±0.11 for the SPH and AMR baseline profiles. The mean non-gravitational energy per particle within r₅₀₀ remaining in the ICM after energy lost during cooling is ε_ICM = 2.8±0.8 keV for the SPH theoretical relation and ε_ICM= 1.7 ±0.9 keV for the AMR theoretical relation. We use the NRAO/VLA Sky Survey source catalog to determine the radio luminosity, L_R, at 1.4 GHz of the central source(s) of our sample. For T_sp> 3 keV, the E_Feedbackcorrelates with L_R, although with different normalization for cool-core and non-cool-core clusters. We show that AGNs could provide a significant portion of the feedback.