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dc.contributor.authorJarvis, M.J.
dc.contributor.authorSmith, Daniel
dc.contributor.authorBonfield, David G.
dc.contributor.authorHardcastle, M.J.
dc.contributor.authorFalder, J. T.
dc.contributor.authorStevens, Jason
dc.contributor.authorIvison, R.J.
dc.contributor.authorAuld, R.
dc.contributor.authorBaes, M.
dc.contributor.authorBaldry, I.K.
dc.contributor.authorBamford, S. P.
dc.contributor.authorBourne, N.
dc.contributor.authorButtiglione, S.
dc.contributor.authorCava, A.
dc.contributor.authorCooray, A.
dc.contributor.authorDariush, A.
dc.contributor.authorde Zotti, G.
dc.contributor.authorDunlop, J. S.
dc.contributor.authorDunne, L.
dc.contributor.authorDye, S.
dc.contributor.authorEales, S.
dc.contributor.authorFritz, J.
dc.contributor.authorHill, D. T.
dc.contributor.authorHopwood, R.
dc.contributor.authorHughes, D.H.
dc.contributor.authorIbar, E.
dc.contributor.authorJones, D. H.
dc.contributor.authorKelvin, L.
dc.contributor.authorLawrence, A.
dc.contributor.authorLeeuw, L.
dc.contributor.authorLoveday, J.
dc.contributor.authorMaddox, S. J.
dc.contributor.authorMichalowski, M. J.
dc.contributor.authorNegrello, M.
dc.contributor.authorNorberg, P.
dc.contributor.authorPohlen, M.
dc.contributor.authorPrescott, M.
dc.contributor.authorRigby, E. E.
dc.contributor.authorRobotham, A.
dc.contributor.authorRodighiero, G.
dc.contributor.authorScott, D.
dc.contributor.authorSharp, R.
dc.contributor.authorTemi, P.
dc.contributor.authorThompson, Mark
dc.contributor.authorvan der Werf, P.
dc.contributor.authorvan Kampen, E.
dc.contributor.authorVlahakis, C.
dc.contributor.authorWhite, G.
dc.date.accessioned2011-12-19T16:01:23Z
dc.date.available2011-12-19T16:01:23Z
dc.date.issued2010
dc.identifier.citationJarvis , M J , Smith , D , Bonfield , D G , Hardcastle , M J , Falder , J T , Stevens , J , Ivison , R J , Auld , R , Baes , M , Baldry , I K , Bamford , S P , Bourne , N , Buttiglione , S , Cava , A , Cooray , A , Dariush , A , de Zotti , G , Dunlop , J S , Dunne , L , Dye , S , Eales , S , Fritz , J , Hill , D T , Hopwood , R , Hughes , D H , Ibar , E , Jones , D H , Kelvin , L , Lawrence , A , Leeuw , L , Loveday , J , Maddox , S J , Michalowski , M J , Negrello , M , Norberg , P , Pohlen , M , Prescott , M , Rigby , E E , Robotham , A , Rodighiero , G , Scott , D , Sharp , R , Temi , P , Thompson , M , van der Werf , P , van Kampen , E , Vlahakis , C & White , G 2010 , ' Herschel-ATLAS: the far-infrared-radio correlation at z <0.5 ' , Monthly Notices of the Royal Astronomical Society , vol. 409 , no. 1 , pp. 92-101 . https://doi.org/10.1111/j.1365-2966.2010.17772.x
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 162317
dc.identifier.otherPURE UUID: 16a684a4-f305-46da-ab9f-62de711250d7
dc.identifier.otherdspace: 2299/5753
dc.identifier.otherWOS: 000284285500010
dc.identifier.otherScopus: 78149363292
dc.identifier.urihttp://hdl.handle.net/2299/7357
dc.descriptionOriginal article can be found at : http://onlinelibrary.wiley.com/ Copyright Royal Astronomical Society
dc.description.abstractWe use data from the Herschel-ATLAS to investigate the evolution of the far-infrared–radio correlation over the redshift range 0 < z < 0.5. Using the total far-infrared luminosity of all >5σ sources in the Herschel-ATLAS Science Demonstration Field and cross-matching these data with radio data from the Faint Images of the Radio Sky at Twenty-Centimetres (FIRST) survey and the NRAO Very Large Array (VLA) Northern Sky Survey (NVSS), we obtain 104 radio counterparts to the Herschel sources. With these data we find no evidence for evolution in the far-infrared–radio correlation over the redshift range 0 < z < 0.5, where the median value for the ratio between far-infrared and radio luminosity, qIR, over this range is qIR= 2.40 ± 0.12 (and a mean of qIR= 2.52 ± 0.03 accounting for the lower limits), consistent with both the local value determined from IRAS and values derived from surveys targeting the high-redshift Universe. By comparing the radio fluxes of our sample measured from both FIRST and NVSS we show that previous results suggesting an increase in the value of qIR from high to low redshift may be the result of resolving out extended emission of the low-redshift sources with relatively high-resolution interferometric data, although contamination from active galactic nuclei could still play a significant role. We also find tentative evidence that the longer wavelength cooler dust is heated by an evolved stellar population which does not trace the star formation rate as closely as the shorter wavelength ≲ 250 μm emission or the radio emission, supporting suggestions based on detailed models of individual galaxies.en
dc.format.extent10
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.rightsOpen
dc.subjectgalaxies: evolution
dc.subjectinfrared: galaxies
dc.subjectradio continuum: galaxies
dc.subjectHIGH-REDSHIFT GALAXIES
dc.subjectACTIVE GALACTIC NUCLEI
dc.subjectSTAR-FORMING GALAXIES
dc.subjectMASS ASSEMBLY GAMA
dc.subjectLUMINOUS GALAXIES
dc.subjectSPIRAL GALAXIES
dc.subjectLOCAL UNIVERSE
dc.subjectCOSMOS FIELD
dc.subjectSKY SURVEY
dc.subject1ST SURVEY
dc.titleHerschel-ATLAS: the far-infrared-radio correlation at z <0.5en
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionScience & Technology Research Institute
dc.contributor.institutionCentre for Astrophysics Research
dc.description.statusPeer reviewed
dc.relation.schoolSchool of Physics, Astronomy and Mathematics
dcterms.dateAccepted2010
rioxxterms.versionofrecordhttps://doi.org/10.1111/j.1365-2966.2010.17772.x
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.rights.accesstypeOpen


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