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dc.contributor.authorHerbert, Peter
dc.contributor.authorJarvis, M.J.
dc.contributor.authorWillcott, C.J.
dc.contributor.authorMcLure, R.J.
dc.contributor.authorMitchell, E.
dc.contributor.authorRawlings, S.
dc.contributor.authorHill, G.J.
dc.contributor.authorDunlop, J.S.
dc.date.accessioned2011-08-15T11:01:31Z
dc.date.available2011-08-15T11:01:31Z
dc.date.issued2011
dc.identifier.citationHerbert , P , Jarvis , M J , Willcott , C J , McLure , R J , Mitchell , E , Rawlings , S , Hill , G J & Dunlop , J S 2011 , ' The evolution of the fundamental plane of radio galaxies from z∼ 0.5 to the present day ' Monthly Notices of the Royal Astronomical Society , vol. 410 , no. 2 , pp. 1360-1376 . https://doi.org/10.1111/j.1365-2966.2010.17524.x
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 305755
dc.identifier.otherPURE UUID: 139f56b6-6f7c-4689-b022-123b74d9de31
dc.identifier.otherScopus: 78650712965
dc.identifier.urihttp://hdl.handle.net/2299/6196
dc.descriptionThe definitive version is available at www3.interscience.wiley.com Copyright Wiley-Blackwell and Royal Astronomical Society
dc.description.abstractWe present deep spectroscopic data for a 24-object subsample of our full 41-object z∼ 0.5 radio galaxy sample in order to investigate the evolution of the Fundamental Plane of radio galaxies. We find that the low-luminosity, Fanaroff–Riley type I (FRI), radio galaxies in our sample are consistent with the local Fundamental Plane of radio galaxies defined by Bettoni et al. when corrected for simple passive evolution of their stellar populations. However, we find that the higher luminosity, Fanaroff–Riley type II (FRII), radio galaxies are inconsistent with the local Fundamental Plane if only passive evolution is considered, and find evidence for a rotation in the Fundamental Plane at z∼ 0.5 when compared with the local relation. We show that neither passive evolution, nor a mass-dependent evolution in the mass-to-light ratio, nor an evolution in the size of the host galaxies can, by themselves, plausibly explain the observed tilt. However, we suggest that some combination of all three effects, with size evolution as the dominant factor, may be sufficient to explain the difference between the planes. We also find evidence for a correlation between host galaxy velocity dispersion and radio luminosity at the 97 per cent significance level within our subsample, although further observations are required in order to determine whether this is different for the FRI and FRII radio sources. Assuming that the MBH–σ relation still holds at z∼ 0.5, this implies that radio luminosity scales with black hole mass, in agreement with previous studies.en
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.rights/dk/atira/pure/core/openaccesspermission/open
dc.subjectgalaxies
dc.subjectactive galaxies
dc.subjectfundamental parameters
dc.subjectgalaxies : nuclei
dc.titleThe evolution of the fundamental plane of radio galaxies from z∼ 0.5 to the present dayen
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
dc.description.versiontypeFinal Accepted Version
rioxxterms.versionAM
rioxxterms.versionofrecordhttps://doi.org/10.1111/j.1365-2966.2010.17524.x
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.rights.accesstypeopenAccess


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