Extended inverse-Compton emission from distant, powerful radio galaxies

We present Chandra observations of two relatively high redshift FRII radio galaxies, 3C 432 and 3C 191 (z=1.785 and z=1.956 respectively), both of which show extended X-ray emission along the axis of the radio jet or lobe. This X-ray emission is most likely to be due to inverse-Compton scattering of...

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Main Authors: Erlund, M, Fabian, A, Blundell, K, Celotti, A, Crawford, C
Formato: Journal article
Idioma:English
Publicado em: 2006
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author Erlund, M
Fabian, A
Blundell, K
Celotti, A
Crawford, C
author_facet Erlund, M
Fabian, A
Blundell, K
Celotti, A
Crawford, C
author_sort Erlund, M
collection OXFORD
description We present Chandra observations of two relatively high redshift FRII radio galaxies, 3C 432 and 3C 191 (z=1.785 and z=1.956 respectively), both of which show extended X-ray emission along the axis of the radio jet or lobe. This X-ray emission is most likely to be due to inverse-Compton scattering of Cosmic Microwave Background (CMB) photons. Under this assumption we estimate the minimum energy contained in the particles responsible. This can be extrapolated to determine a rough estimate of the total energy. We also present new, deep radio observations of 3C 294, which confirm some association between radio and X-ray emission along the NE-SW radio axis and also that radio emission is not detected over the rest of the extent of the diffuse X-ray emission. This, together with the offset between the peaks of the X-ray and radio emissions may indicate that the jet axis in this source is precessing.
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spelling oxford-uuid:878d745c-16f5-4ee6-8fca-8fe29389ed402022-03-26T22:11:28ZExtended inverse-Compton emission from distant, powerful radio galaxiesJournal articlehttp://purl.org/coar/resource_type/c_dcae04bcuuid:878d745c-16f5-4ee6-8fca-8fe29389ed40EnglishSymplectic Elements at Oxford2006Erlund, MFabian, ABlundell, KCelotti, ACrawford, CWe present Chandra observations of two relatively high redshift FRII radio galaxies, 3C 432 and 3C 191 (z=1.785 and z=1.956 respectively), both of which show extended X-ray emission along the axis of the radio jet or lobe. This X-ray emission is most likely to be due to inverse-Compton scattering of Cosmic Microwave Background (CMB) photons. Under this assumption we estimate the minimum energy contained in the particles responsible. This can be extrapolated to determine a rough estimate of the total energy. We also present new, deep radio observations of 3C 294, which confirm some association between radio and X-ray emission along the NE-SW radio axis and also that radio emission is not detected over the rest of the extent of the diffuse X-ray emission. This, together with the offset between the peaks of the X-ray and radio emissions may indicate that the jet axis in this source is precessing.
spellingShingle Erlund, M
Fabian, A
Blundell, K
Celotti, A
Crawford, C
Extended inverse-Compton emission from distant, powerful radio galaxies
title Extended inverse-Compton emission from distant, powerful radio galaxies
title_full Extended inverse-Compton emission from distant, powerful radio galaxies
title_fullStr Extended inverse-Compton emission from distant, powerful radio galaxies
title_full_unstemmed Extended inverse-Compton emission from distant, powerful radio galaxies
title_short Extended inverse-Compton emission from distant, powerful radio galaxies
title_sort extended inverse compton emission from distant powerful radio galaxies
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AT blundellk extendedinversecomptonemissionfromdistantpowerfulradiogalaxies
AT celottia extendedinversecomptonemissionfromdistantpowerfulradiogalaxies
AT crawfordc extendedinversecomptonemissionfromdistantpowerfulradiogalaxies