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dc.contributor.authorMullin, L.M.
dc.contributor.authorHardcastle, M.J.
dc.contributor.authorRiley, J.M.
dc.date.accessioned2009-04-01T08:18:55Z
dc.date.available2009-04-01T08:18:55Z
dc.date.issued2006
dc.identifier.citationMullin , L M , Hardcastle , M J & Riley , J M 2006 , ' High-resolution observations of radio sources with 0.6 < z≤ 1.0 ' , Monthly Notices of the Royal Astronomical Society , vol. 372 , no. 1 , pp. 113-135 . https://doi.org/10.1111/j.1365-2966.2006.10763.x
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 169124
dc.identifier.otherPURE UUID: e6926b9b-bad4-4164-9e81-d8cd422ff1a2
dc.identifier.otherdspace: 2299/3094
dc.identifier.otherScopus: 33749255649
dc.identifier.urihttp://hdl.handle.net/2299/3094
dc.description‘The definitive version is available at www.blackwell-synergy.com.’ Copyright Blackwell Publishing / RAS. DOI: 10.1111/j.1365-2966.2006.10763.x [Full text of this article is not available in the UHRA]
dc.description.abstractHigh-resolution, high-sensitivity 8.4- and 5-GHz VLA observations and 5-GHz MERLIN observations are presented for 32 FRII radio sources with 0.6 < z≤ 1.0 from the 3CRR sample. These data conclude a long-term project in which high-sensitivity, high-resolution observations of a complete sample of 97 FRII quasars and radio galaxies with z≤ 1.0 have been collected; data for sources with z≤ 0.6 from this sample have been presented previously in a series of papers. Jet features are detected in 16 of the 32 new sources, giving a jet detection rate of 50 per cent in this high-redshift subsample. Jet and hotspot detectability in the subsample are discussed.en
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.titleHigh-resolution observations of radio sources with 0.6 < z≤ 1.0en
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
rioxxterms.versionofrecordhttps://doi.org/10.1111/j.1365-2966.2006.10763.x
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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