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dc.contributor.authorKapinska, A. D.
dc.contributor.authorStaveley-Smith, L.
dc.contributor.authorCrocker, R.
dc.contributor.authorMeurer, G. R.
dc.contributor.authorBhandari, S.
dc.contributor.authorHurley-Walker, N.
dc.contributor.authorOffringa, A. R.
dc.contributor.authorHanish, D. J.
dc.contributor.authorSeymour, N.
dc.contributor.authorEkers, R. D.
dc.contributor.authorBell, M. E.
dc.contributor.authorCallingham, J. R.
dc.contributor.authorDwarakanath, K. S.
dc.contributor.authorFor, B. -Q.
dc.contributor.authorGaensler, B. M.
dc.contributor.authorHancock, P. J.
dc.contributor.authorHindson, Luke
dc.contributor.authorJohnston-Hollitt, M.
dc.contributor.authorLenc, E.
dc.contributor.authorMcKinley, B.
dc.contributor.authorMorgan, J.
dc.contributor.authorProcopio, P.
dc.contributor.authorWayth, R. B.
dc.contributor.authorWu, C.
dc.contributor.authorZheng, Q.
dc.contributor.authorBarry, N.
dc.contributor.authorBeardsley, A. P.
dc.contributor.authorBowman, J. D.
dc.contributor.authorBriggs, F.
dc.contributor.authorCarroll, P.
dc.contributor.authorDillon, J. S.
dc.contributor.authorEwall-Wice, A.
dc.contributor.authorFeng, L.
dc.contributor.authorGreenhill, L. J.
dc.contributor.authorHazelton, B. J.
dc.contributor.authorHewitt, J. N.
dc.contributor.authorJacobs, D. J.
dc.contributor.authorKim, H. -S.
dc.contributor.authorKittiwisit, P.
dc.contributor.authorLine, J.
dc.contributor.authorLoeb, A.
dc.contributor.authorMitchell, D. A.
dc.contributor.authorMorales, M. F.
dc.contributor.authorNeben, A. R.
dc.contributor.authorPaul, S.
dc.contributor.authorPindor, B.
dc.contributor.authorPober, J. C.
dc.contributor.authorRiding, J.
dc.contributor.authorSethi, S. K.
dc.contributor.authorShankar, N. Udaya
dc.contributor.authorSubrahmanyan, R.
dc.contributor.authorSullivan, I. S.
dc.contributor.authorTegmark, M.
dc.contributor.authorThyagarajan, N.
dc.contributor.authorTingay, S. J.
dc.contributor.authorTrott, C. M.
dc.contributor.authorWebster, R. L.
dc.contributor.authorWyithe, S. B.
dc.date.accessioned2017-06-01T15:46:24Z
dc.date.available2017-06-01T15:46:24Z
dc.date.issued2017-03-27
dc.identifier.citationKapinska , A D , Staveley-Smith , L , Crocker , R , Meurer , G R , Bhandari , S , Hurley-Walker , N , Offringa , A R , Hanish , D J , Seymour , N , Ekers , R D , Bell , M E , Callingham , J R , Dwarakanath , K S , For , B -Q , Gaensler , B M , Hancock , P J , Hindson , L , Johnston-Hollitt , M , Lenc , E , McKinley , B , Morgan , J , Procopio , P , Wayth , R B , Wu , C , Zheng , Q , Barry , N , Beardsley , A P , Bowman , J D , Briggs , F , Carroll , P , Dillon , J S , Ewall-Wice , A , Feng , L , Greenhill , L J , Hazelton , B J , Hewitt , J N , Jacobs , D J , Kim , H -S , Kittiwisit , P , Line , J , Loeb , A , Mitchell , D A , Morales , M F , Neben , A R , Paul , S , Pindor , B , Pober , J C , Riding , J , Sethi , S K , Shankar , N U , Subrahmanyan , R , Sullivan , I S , Tegmark , M , Thyagarajan , N , Tingay , S J , Trott , C M , Webster , R L & Wyithe , S B 2017 , ' Spectral energy distribution and radio halo of NGC253 at low radio frequencies ' , The Astrophysical Journal , vol. 838 , no. 1 , 68 . https://doi.org/10.3847/1538-4357/aa5f5d
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 11154796
dc.identifier.otherPURE UUID: 3ff7d3b1-0046-4d06-9b2c-7c1d9b0847ca
dc.identifier.otherArXiv: http://arxiv.org/abs/1702.02434v1
dc.identifier.otherScopus: 85016763865
dc.identifier.urihttp://hdl.handle.net/2299/18269
dc.descriptionA. D. Kapinska, 'Spectral Energy Distribution and Radio Halo of NGC 253 at Low Radio Frequencies', The Astrophysical Journal, Vol. 838(68), 15 pp, March 2017. The version of record is available online at doi: https://doi.org/10.3847/1538-4357/aa5f5d. © 2017. The American Astronomical Society. All rights reserved.
dc.description.abstractWe present new radio continuum observations of NGC253 from the Murchison Widefield Array at frequencies between 76 and 227 MHz. We model the broadband radio spectral energy distribution for the total flux density of NGC253 between 76 MHz and 11 GHz. The spectrum is best described as a sum of central starburst and extended emission. The central component, corresponding to the inner 500pc of the starburst region of the galaxy, is best modelled as an internally free-free absorbed synchrotron plasma, with a turnover frequency around 230 MHz. The extended emission component of the NGC253 spectrum is best described as a synchrotron emission flattening at low radio frequencies. We find that 34% of the extended emission (outside the central starburst region) at 1 GHz becomes partially absorbed at low radio frequencies. Most of this flattening occurs in the western region of the SE halo, and may be indicative of synchrotron self-absorption of shock re-accelerated electrons or an intrinsic low-energy cut off of the electron distribution. Furthermore, we detect the large-scale synchrotron radio halo of NGC253 in our radio images. At 154 - 231 MHz the halo displays the well known X-shaped/horn-like structure, and extends out to ~8kpc in z-direction (from major axis).en
dc.format.extent15
dc.language.isoeng
dc.relation.ispartofThe Astrophysical Journal
dc.rightsOpen
dc.subjectgalaxies: halos
dc.subjectgalaxies: individual (NGC 253)
dc.subjectgalaxies: starburst
dc.subjectradiation mechanism: non-thermal
dc.subjectradiation mechanisms: thermal
dc.subjectradio continuum; galaxies
dc.titleSpectral energy distribution and radio halo of NGC253 at low radio frequenciesen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
dc.identifier.urlhttps://arxiv.org/abs/1702.02434
dc.description.versiontypeFinal Published version
dcterms.dateAccepted2017-03-27
rioxxterms.versionVoR
rioxxterms.versionofrecordhttps://doi.org/10.3847/1538-4357/aa5f5d
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.rights.accesstypeOpen


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