It fits even complex brightness and temperature profiles. T (r)/n(r)2/3, where T (r) and n(r) are the ICP temperatureĪnd density profiles, respectively) and shows how accurately The main dichotomy “CC versus NCC” clusters in terms of aįew ICP parameters governing the radial entropy run (k(r) = This analysis highlights how simply the SM represents These two componentsĪre related not only by their common potential well but alsoīy parallel accretion of surrounding DM and baryons into theĪn analysis of the X-ray brightness and temperature profilesįor both cool core (CC) and non cool core (NCC) clusters hasīeen performed in terms of the SM (Cavaliere et al. The intracluster plasma (ICP) within the potential wells providedīy the dominant dark matter (DM). Profiles when we consider the entropy-modulated equilibrium of The Supermodel (SM) describes the density and temperature Mechanisms: non-thermal – X-rays: galaxies: clusters Key words: galaxies: clusters: general – galaxies: clusters: individual (Coma) – intergalactic medium – radiation PDS FOV being considerably greater than the HXD-PIN FOV. above 4σ also for the higher average temperature of 8.45 keV thanks to the Spectra reaffirms the presence of an NT component in the HXR spectrum of the Coma cluster. Here we present a further evidence of the compatibility between the Suzaku and BeppoSAX spectra, obtained by our SM analysis of the PDS data, when the smaller size of the HXD-PIN FOV and the two different average temperatures derived by XMM-Newton and by the joint XMM-Newton/Suzaku analysis are taken into account. above 4σ, without including systematic effects, for an average XMM-Newton temperature of 8.2 keV in the Suzaku/HXD-PIN FOV, in agreement with our earlier PDS analysis. The energy range 20–80 keV for the NT flux with an average gas temperature of 8.45± 0.06 keV and an excess of NT A recent joint XMM-Newton/Suzaku analysis reports an upper limit of∼6×10−12erg cm−2s−1in The confidence level (c.l.) of ∼4.8σ and a nonthermal (NT) flux of (1.30 ± 0.40) × 10−11erg cm−2s−1in the energy Phoswich Detector System (PDS) hard X-ray (HXR) spectrum confirms our previous results, namely, an excess at The XMM-Newton temperature profile and the ROSAT brightness distribution. Starting from the intracluster gas temperature and density profiles obtained by the SM analysis of X-ray observables: In this paper, the thermal emissivity in the Coma cluster is derived Which is crucial for the analysis of the hard excess. The Supermodel (SM) provides an accurate description of the thermal contribution by the hot intracluster plasma Received 2010 November 30 accepted 2011 March 4 published 2011 April 20 Lapi 5,6ġ INAF/IASF-Roma, Via del Fosso del Cavaliere, I-00133 Roma, ItalyĢ INAF/IASF-BO, Via Gobetti 101, I-40129 Bologna, Italyģ Department of Physics, University of Alabama, Huntsville, AL 35899, USAĤ National Space Science and Technology Center, NASA Marshall Space Flight Center, Huntsville, AL 35812, USAĥ Dipartimento di Fisica, Universit`a “Tor Vergata,” Via Ricerca Scientifica 1, I-00133 Roma, ItalyĦ SISSA/ISAS, Via Bonomea 265, I-34136 Trieste, Italy SUPERMODEL ANALYSIS OF THE HARD X-RAY EXCESS IN THE COMA CLUSTER
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