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Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/5956
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dc.contributor.authorChaudhuri, Anya-
dc.contributor.authorMajumdar, Subhabrata-
dc.contributor.authorNath, Biman B.-
dc.date.accessioned2014-08-26T07:47:08Z-
dc.date.available2014-08-26T07:47:08Z-
dc.date.issued2013-10-20-
dc.identifier.citationAstrophysical Journal, 2013, Vol. 776, p84en
dc.identifier.issn0004-637X-
dc.identifier.issn1538-4357-(Online)-
dc.identifier.urihttp://hdl.handle.net/2289/5956-
dc.descriptionRestricted Access. An open-access version is available at arXiv.org (one of the alternative locations)en
dc.description.abstractWe 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 r 500, 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 $E_{\rm Feedback} \propto T_{\rm sp}^{2.52 \pm 0.08}$ and $E_{\rm Feedback} \propto T_{\rm sp}^{2.17 \pm 0.11}$ for the SPH and AMR baseline profiles. The mean non-gravitational energy per particle within r 500 remaining in the ICM after energy lost during cooling is epsilonICM = 2.8 ± 0.8 keV for the SPH theoretical relation and epsilonICM = 1.7 ± 0.9 keV for the AMR theoretical relation. We use the NRAO/VLA Sky Survey source catalog to determine the radio luminosity, LR , at 1.4 GHz of the central source(s) of our sample. For T sp > 3 keV, the E Feedback correlates with LR , although with different normalization for cool-core and non-cool-core clusters. We show that AGNs could provide a significant portion of the feedback.en
dc.language.isoenen
dc.publisherIOP Publishing for the American Astronomical Societyen
dc.relation.urihttp://adsabs.harvard.edu/abs/2013ApJ...776...84Cen
dc.relation.urihttp://arxiv.org/abs/1211.3817en
dc.relation.urihttp://dx.doi.org/10.1088/0004-637X/776/2/84en
dc.rights2013 The American Astronomical Societyen
dc.subjectGalaxiesen
dc.subjectX-raysen
dc.titleActive galactic nucleus feedback and entropy injection in galaxy cluster coresen
dc.typeArticleen
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