AGN feedback and entropy injection in galaxy cluster cores

Abstract

The non-gravitational energy feedback is of crucial importance in modeling/simulating clusters to be used as cosmological probes. AGNs are, arguably, of primary importance in injecting energy in the cluster cores. We make the first estimate of non-gravitational energy {\it profiles} in galaxy cluster cores (and beyond) from observational data. Comparing the observed entropy profiles within $r_{500}$, from the Representative {\it XMM-Newton} Cluster Structure Survey (REXCESS), to simulated entropy profiles from both AMR and SPH non-radiative simulations, we estimate the amount of non-gravitational energy, $E_{\mathrm{ICM}}$, contained in the ICM. Adding the radiative losses we estimate the total energy feedback, $E_{\mathrm{Feedback}}$, into the clusters. The profiles for the energy deposition, $\Delta E_{\mathrm{ICM}}(x)$, in the inner regions differ for Cool-Core (CC) and Non Cool-Core (NCC) clusters, decreasing after accounting for the radiative cooling. The total feedback energy scales with the mean spectroscopic temperature as $E_{\mathrm{Feedback}}\propto T_{\mathrm{sp}}^{2.52\pm 0.08}$ and $E_{\mathrm{Feedback}}\propto T_{\mathrm{sp}}^{2.17\pm 0.11}$, when compared with the baseline SPH and AMR profiles respectively. The scatter in the two cases is 15% and 23%, respectively. The mean non-gravitational energy per particle within $r_{500}$, is ${\epsilon }_{\mathrm{ICM}}=2.8\pm 0.8$ keV for the SPH theoretical relation and ${\epsilon }_{\mathrm{ICM}}=1.7\pm 0.9$ keV for the AMR theoretical relation. We use the {\it NRAO/VLA Sky Survey} (NVSS) source catalog to determine the radio luminosity, $L_R$, at 1.4 GHz of the central source(s) of our sample. For $T_{\mathrm{sp}}>3$ keV, the $E_{\mathrm{Feedback}}$ correlates with $L_R$. We show that AGNs could provide a significant component of the feedback. (Abridged)

Accepted for publication in ApJ

References in corpus (13)

• On the prevalence of radio-loud AGN in brightest cluster galaxies: implications for AGN heating of cooling flows
• AGN-controlled cooling in elliptical galaxies
• The Representative XMM-Newton Cluster Structure Survey (REXCESS) of an X-ray Luminosity Selected Galaxy Cluster Sample
• Why Do Only Some Galaxy Clusters Have Cool Cores?
• AGN Jet Kinetic Power and the Energy Budget of Radio Galaxy Lobes
• Cosmological Constraints from the Red-Sequence Cluster Survey
• On the Origin of Cores in Simulated Galaxy Clusters
• Stellar mass estimates in early-type galaxies: procedures, uncertainties and models dependence
• Simulations of cosmic ray feedback by AGN in galaxy clusters
• The luminosity -- halo-mass relation for brightest cluster galaxies
• The Weak Shock in the Core of the Perseus Cluster
• The Lifetime of FRIIs in Groups and Clusters: Implications for Radio-Mode Feedback
• Limits on the AGN activities in X-ray underluminous galaxy groups

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• Cosmological Simulation of Galaxy Groups and Clusters-I: Global Effect of Feedback from Active Galactic Nuclei
• JWST/NIRCam Narrowband Survey of Pa$\beta$ Emitters in the Spiderweb Protocluster at z=2.16
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• Constraining the X-ray AGN halo occupation distribution: implications for eROSITA
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