Long RXTE Observations of A2163

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dc.creatorRephaeli, Yoel
dc.creatorGruber, Duane
dc.creatorArieli, Yinon
dc.date2006-06-05
dc.date.accessioned2026-07-07T10:39:12Z
dc.date.available2026-07-07T10:39:12Z
dc.descriptionA2163 was observed by the RXTE satellite for 530 ks during a 6 month period starting in August 2004. The cluster primary emission is from very hot intracluster gas with kT~15 keV, but this component does not by itself provide the best fitting model. A secondary emission component is quite clearly needed, and while this could also be thermal at a temperature significantly lower than kT~15 keV, the best fit (to the combined PCA and HEXTE datasets) is obtained with a power law secondary spectral component. The deduced parameters of the non-thermal (NT) emission imply a significant fractional flux amounting to ~25% of the integrated 3-50 keV emission. NT emission is expected given the intense level of radio emission, most prominently from a large extended (`halo') central region of the cluster. Interpreting the deduced NT emission as Compton scattering of the radio-emitting relativistic electrons by the CMB, we estimate the volume-averaged value of the magnetic field in the extended radio region to be B=0.4+/-0.2 microG.
dc.description10 pages, 1 figure; accepted for publication in ApJ
dc.identifierhttps://arxiv.org/abs/astro-ph/0606097
dc.identifierhttp://arxiv.org/abs/astro-ph/0606097
dc.identifierAstrophys.J.649:673-677,2006
dc.identifierdoi:10.1086/506310
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/180943
dc.subjectAstrophysics
dc.titleLong RXTE Observations of A2163
dc.typetext

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