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dc.contributor.authorRead, Shaun
dc.contributor.authorSmith, Daniel
dc.contributor.authorGurkan, Gulay
dc.contributor.authorHardcastle, Martin
dc.contributor.authorWilliams, Wendy Louise
dc.contributor.authorBest, P.N.
dc.contributor.authorBrinks, Elias
dc.contributor.authorCalistro-Rivera, Gabriela
dc.contributor.authorChyzy, K.T.
dc.contributor.authorDuncan, Kenneth J.
dc.contributor.authorDunne, Loretta
dc.contributor.authorJarvis, M. J.
dc.contributor.authorMorabito, Leah K.
dc.contributor.authorPrandoni, I.
dc.contributor.authorRottgering, H. J. A.
dc.contributor.authorSabater, Jose
dc.contributor.authorViaene, Sébastien
dc.date.accessioned2018-08-16T00:18:28Z
dc.date.available2018-08-16T00:18:28Z
dc.date.issued2018-11-11
dc.identifier.citationRead , S , Smith , D , Gurkan , G , Hardcastle , M , Williams , W L , Best , P N , Brinks , E , Calistro-Rivera , G , Chyzy , K T , Duncan , K J , Dunne , L , Jarvis , M J , Morabito , L K , Prandoni , I , Rottgering , H J A , Sabater , J & Viaene , S 2018 , ' The Far-Infrared Radio Correlation at low radio frequency with LOFAR/H-ATLAS ' , Monthly Notices of the Royal Astronomical Society , vol. 480 , no. 4 , pp. 5625-5644 . https://doi.org/10.1093/mnras/sty2198
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 15169645
dc.identifier.otherPURE UUID: f908bc7e-bc45-4d5f-8bde-2534d2b5c7ad
dc.identifier.otherScopus: 85054748490
dc.identifier.otherORCID: /0000-0002-7758-9699/work/54143419
dc.identifier.otherORCID: /0000-0001-7315-1596/work/62750968
dc.identifier.urihttp://hdl.handle.net/2299/20465
dc.descriptionThis article has been accepted for publication in Monthly Notices of the Royal Astronomical Society © 2018 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
dc.description.abstractThe radio and far-infrared luminosities of star-forming galaxies are tightly correlated over several orders of magnitude; this is known as the far-infrared radio correlation (FIRC). Previous studies have shown that a host of factors conspire to maintain a tight and linear FIRC, despite many models predicting deviation. This discrepancy between expectations and observations is concerning since a linear FIRC underpins the use of radio luminosity as a star-formation rate indicator. Using LOFAR 150MHz, FIRST 1.4GHz, and Herschel infrared luminosities derived from the new LOFAR/H-ATLAS catalogue, we investigate possible variation in the monochromatic (250μm) FIRC at low and high radio frequencies. We use statistical techniques to probe the FIRC for an optically-selected sample of 4,082 emission-line classified star-forming galaxies as a function of redshift, effective dust temperature, stellar mass, specific star formation rate, and mid-infrared colour (an empirical proxy for specific star formation rate). Although the average FIRC at high radio frequency is consistent with expectations based on a standard power-law radio spectrum, the average correlation at 150MHz is not. We see evidence for redshift evolution of the FIRC at 150MHz, and find that the FIRC varies with stellar mass, dust temperature and specific star formation rate, whether the latter is probed using MAGPHYS fitting, or using mid-infrared colour as a proxy. We can explain the variation, to within 1σ , seen in the FIRC over mid-infrared colour by a combination of dust temperature, redshift, and stellar mass using a Bayesian partial correlation technique.en
dc.format.extent20
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.rightsOpen
dc.subjectGalaxies: star formation
dc.subjectInfrared: galaxies
dc.subjectRadio continuum: galaxies
dc.subjectAstronomy and Astrophysics
dc.subjectSpace and Planetary Science
dc.titleThe Far-Infrared Radio Correlation at low radio frequency with LOFAR/H-ATLASen
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=85054748490&partnerID=8YFLogxK
dc.relation.schoolSchool of Physics, Astronomy and Mathematics
dc.description.versiontypeFinal Accepted Version
dcterms.dateAccepted2018-11-11
rioxxterms.versionAM
rioxxterms.versionofrecordhttps://doi.org/10.1093/mnras/sty2198
rioxxterms.licenseref.uriOther
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.rights.accesstypeOpen


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