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dc.contributor.authorHindson, L.
dc.contributor.authorJohnston-Hollitt, M.
dc.contributor.authorHurley-Walker, N.
dc.contributor.authorBuckley, K.
dc.contributor.authorMorgan, J.
dc.contributor.authorCarretti, E.
dc.contributor.authorDwarakanath, K. S.
dc.contributor.authorBell, M.
dc.contributor.authorBernardi, G.
dc.contributor.authorBhat, N. D. R.
dc.contributor.authorBowman, J. D.
dc.contributor.authorBriggs, F.
dc.contributor.authorCappallo, R. J.
dc.contributor.authorCorey, B. E.
dc.contributor.authorDeshpande, A. A.
dc.contributor.authorEmrich, D.
dc.contributor.authorEwall-Wice, A.
dc.contributor.authorFeng, L.
dc.contributor.authorGaensler, B. M.
dc.contributor.authorGoeke, R.
dc.contributor.authorGreenhill, L. J.
dc.contributor.authorHazelton, B. J.
dc.contributor.authorJacobs, D.
dc.contributor.authorKaplan, D. L.
dc.contributor.authorKasper, J. C.
dc.contributor.authorKratzenberg, E.
dc.contributor.authorKudryavtseva, N.
dc.contributor.authorLenc, E.
dc.contributor.authorLonsdale, C. J.
dc.contributor.authorLynch, M. J.
dc.contributor.authorMcWhirter, S. R.
dc.contributor.authorMcKinley, B.
dc.contributor.authorMitchell, D. A.
dc.contributor.authorMorales, M. F.
dc.contributor.authorMorgan, E.
dc.contributor.authorOberoi, D.
dc.contributor.authorOrd, S. M.
dc.contributor.authorPindor, B.
dc.contributor.authorPrabu, T.
dc.contributor.authorProcopio, P.
dc.contributor.authorOffringa, A. R.
dc.contributor.authorRiding, J.
dc.contributor.authorRogers, A. E. E.
dc.contributor.authorRoshi, A.
dc.contributor.authorShankar, N. Udaya
dc.contributor.authorSrivani, K. S.
dc.contributor.authorSubrahmanyan, R.
dc.contributor.authorTingay, S. J.
dc.contributor.authorWaterson, M.
dc.contributor.authorWayth, R. B.
dc.contributor.authorWebster, R. L.
dc.contributor.authorWhitney, A. R.
dc.contributor.authorWilliams, A.
dc.contributor.authorWilliams, C. L.
dc.date.accessioned2017-07-20T16:03:52Z
dc.date.available2017-07-20T16:03:52Z
dc.date.issued2014-11-21
dc.identifier.citationHindson , L , Johnston-Hollitt , M , Hurley-Walker , N , Buckley , K , Morgan , J , Carretti , E , Dwarakanath , K S , Bell , M , Bernardi , G , Bhat , N D R , Bowman , J D , Briggs , F , Cappallo , R J , Corey , B E , Deshpande , A A , Emrich , D , Ewall-Wice , A , Feng , L , Gaensler , B M , Goeke , R , Greenhill , L J , Hazelton , B J , Jacobs , D , Kaplan , D L , Kasper , J C , Kratzenberg , E , Kudryavtseva , N , Lenc , E , Lonsdale , C J , Lynch , M J , McWhirter , S R , McKinley , B , Mitchell , D A , Morales , M F , Morgan , E , Oberoi , D , Ord , S M , Pindor , B , Prabu , T , Procopio , P , Offringa , A R , Riding , J , Rogers , A E E , Roshi , A , Shankar , N U , Srivani , K S , Subrahmanyan , R , Tingay , S J , Waterson , M , Wayth , R B , Webster , R L , Whitney , A R , Williams , A & Williams , C L 2014 , ' The first Murchison Widefield Array low frequency radio observations of cluster scale non-thermal emission : the case of Abell 3667 ' , Monthly Notices of the Royal Astronomical Society , vol. 445 , no. 1 , pp. 330-346 . https://doi.org/10.1093/mnras/stu1669
dc.identifier.issn1365-2966
dc.identifier.otherPURE: 10291444
dc.identifier.otherPURE UUID: 81eb6237-ad7e-4784-bea4-a3944f781ad5
dc.identifier.otherArXiv: http://arxiv.org/abs/1408.3167v1
dc.identifier.otherScopus: 84913605413
dc.identifier.urihttp://hdl.handle.net/2299/19019
dc.descriptionThis article has been accepted for publication in Monthly Notices of the Royal Astronomical Society. © 2014 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.
dc.description.abstractWe present the first Murchison Widefield Array observations of the well-known cluster of galaxies Abell 3667 (A3667) between 105 and 241 MHz. A3667 is one of the best known examples of a galaxy cluster hosting a double radio relic and has been reported to contain a faint radio halo and bridge. The origins of radio halos, relics and bridges is still unclear, however galaxy cluster mergers seems to be an important factor. We clearly detect the North-West (NW) and South-East (SE) radio relics in A3667 and find an integrated flux density at 149 MHz of 28.1 +/- 1.7 and 2.4 +/- 0.1 Jy, respectively, with an average spectral index, between 120 and 1400 MHz, of -0.9 +/- 0.1 for both relics. We find evidence of a spatial variation in the spectral index across the NW relic steepening towards the centre of the cluster, which indicates an ageing electron population. These properties are consistent with higher frequency observations. We detect emission that could be associated with a radio halo and bridge. How- ever, due to the presence of poorly sampled large-scale Galactic emission and blended point sources we are unable to verify the exact nature of these features.en
dc.format.extent17
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.rights/dk/atira/pure/core/openaccesspermission/open
dc.subjectastro-ph.GA
dc.titleThe first Murchison Widefield Array low frequency radio observations of cluster scale non-thermal emission : the case of Abell 3667en
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
dc.relation.schoolSchool of Physics, Astronomy and Mathematics
dc.description.versiontypeFinal Published version
dcterms.dateAccepted2014-08-12
rioxxterms.versionVoR
rioxxterms.versionofrecordhttps://doi.org/10.1093/mnras/stu1669
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.rights.accesstypeopenAccess


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