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dc.contributor.authorDuffy, R. T.
dc.contributor.authorWorrall, D. M.
dc.contributor.authorBirkinshaw, M.
dc.contributor.authorNulsen, P. E. J.
dc.contributor.authorWise, M. W.
dc.contributor.authorVries, M. N. de
dc.contributor.authorSnios, B.
dc.contributor.authorMathews, W. G.
dc.contributor.authorPerley, R. A.
dc.contributor.authorHardcastle, M. J.
dc.contributor.authorRafferty, D. A.
dc.contributor.authorMcNamara, B. R.
dc.contributor.authorEdge, A. C.
dc.contributor.authorMcKean, J. P.
dc.contributor.authorCarilli, C. L.
dc.contributor.authorCroston, J. H.
dc.contributor.authorGodfrey, L. E. H.
dc.contributor.authorLaing, R. A.
dc.date.accessioned2018-06-06T17:09:29Z
dc.date.available2018-06-06T17:09:29Z
dc.date.issued2018-06-01
dc.identifier.citationDuffy , R T , Worrall , D M , Birkinshaw , M , Nulsen , P E J , Wise , M W , Vries , M N D , Snios , B , Mathews , W G , Perley , R A , Hardcastle , M J , Rafferty , D A , McNamara , B R , Edge , A C , McKean , J P , Carilli , C L , Croston , J H , Godfrey , L E H & Laing , R A 2018 , ' The X-ray Ribs Within the Cocoon Shock of Cygnus A ' , Monthly Notices of the Royal Astronomical Society , vol. 476 , no. 4 , pp. 4848–4860 . https://doi.org/10.1093/mnras/sty549
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 13524286
dc.identifier.otherPURE UUID: 398b4ab4-5d60-43e3-9f65-a6e5c82e1982
dc.identifier.otherArXiv: http://arxiv.org/abs/1802.09476v1
dc.identifier.otherScopus: 85045456590
dc.identifier.urihttp://hdl.handle.net/2299/20150
dc.descriptionThis article has been accepted for publication in Monthly Notices of the Royal Astronomical Society. ©: 2018 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved
dc.description.abstractWe use new and archival Chandra observations of Cygnus A, totalling ~1.9Ms, to investigate the distribution and temperature structure of gas lying within the projected extent of the cocoon shock and exhibiting a rib-like structure.We confirm that the X-rays are dominated by thermal emission with an average temperature of around 4 keV, and have discovered an asymmetry in the temperature gradient, with the southwestern part of the gas cooler than the rest by up to 2 keV. Pressure estimates suggest that the gas is a coherent structure of single origin located inside the cocoon, with a mass of roughly 2 × 10 10M ⊙. We conclude that the gas is debris resulting from disintegration of the cool core of the Cygnus A cluster after the passage of the jet during the early stages of the current epoch of activity. The 4 keV gas now lies on the central inside surface of the hotter cocoon rim. The temperature gradient could result from an offset between the centre of the cluster core and the Cygnus A host galaxy at the switch-on of current radio activity.en
dc.format.extent13
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.rightsOpen
dc.subjectGalaxies: active
dc.subjectGalaxies: individual: Cygnus A- radio continuum: galaxies
dc.subjectX-rays: galaxies
dc.subjectAstronomy and Astrophysics
dc.subjectSpace and Planetary Science
dc.titleThe X-ray Ribs Within the Cocoon Shock of Cygnus Aen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionCentre for Astrophysics Research
dc.description.statusPeer reviewed
dc.identifier.urlhttp://www.scopus.com/inward/record.url?scp=85045456590&partnerID=8YFLogxK
dc.description.versiontypeFinal Published version
dcterms.dateAccepted2018-06-01
rioxxterms.versionVoR
rioxxterms.versionofrecordhttps://doi.org/10.1093/mnras/sty549
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.rights.accesstypeOpen


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