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dc.contributor.authorAn, T.
dc.contributor.authorHong, X.Y.
dc.contributor.authorHardcastle, M.J.
dc.contributor.authorWorrall, D.M.
dc.contributor.authorVenturi, T.
dc.contributor.authorPearson, T.J.
dc.contributor.authorShen, Z.Q.
dc.contributor.authorZhao, W.
dc.contributor.authorFeng, W.X.
dc.date.accessioned2010-07-28T08:15:24Z
dc.date.available2010-07-28T08:15:24Z
dc.date.issued2010
dc.identifier.citationAn , T , Hong , X Y , Hardcastle , M J , Worrall , D M , Venturi , T , Pearson , T J , Shen , Z Q , Zhao , W & Feng , W X 2010 , ' Kinematics of the parsec-scale radio jet in 3C 48 ' , Monthly Notices of the Royal Astronomical Society , vol. 402 , no. 1 , pp. 87-104 . https://doi.org/10.1111/j.1365-2966.2009.15899.x
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 178909
dc.identifier.otherPURE UUID: 179f185a-f880-44ae-ab71-eebb17f633d7
dc.identifier.otherdspace: 2299/4699
dc.identifier.otherScopus: 77949336663
dc.identifier.urihttp://hdl.handle.net/2299/4699
dc.description‘The definitive version is available at www3.interscience.wiley.com '. Copyright Royal Astronomical Society
dc.description.abstractWe present results on the compact steep-spectrum quasar 3C 48 from observations with the Very Long Baseline Array (VLBA), the Multi-Element Radio Linked Interferometer Network (MERLIN) and the European Very long baseline interferometry (VLBI) Network (EVN) at multiple radio frequencies. In the 1.5-GHz VLBI images, the radio jet is characterized by a series of bright knots. The active nucleus is embedded in the southernmost VLBI component A, which is further resolved into two sub-components A1 and A2 at 4.8 and 8.3 GHz, respectively. A1 shows a flat spectrum and A2 shows a steep spectrum. The most strongly polarized VLBI components are located at component C ∼ 0.25 arcsec north of the core, where the jet starts to bend to the north-east. The polarization angles at C show gradual changes across the jet width at all observed frequencies, indicative of a gradient in the emission-weighted intrinsic polarization angle across the jet and possibly a systematic gradient in the rotation measure; moreover, the percentage of polarization increases near the curvature at C, likely consistent with the presence of a local jet–interstellar-medium interaction and/or changing magnetic-field directions. The hot spot B shows a higher rotation measure, and has no detected proper motion. These facts provide some evidence for a stationary shock in the vicinity of B. Comparison of the present VLBI observations with those made 8.43 yr ago suggests a significant northward motion for A2 with an apparent transverse velocity βapp= 3.7 ± 0.4c . The apparent superluminal motion suggests that the relativistic jet plasma moves at a velocity of ≳0.96c if the jet is viewed at an inclination angle less than 20° . A simple precessing jet model and a hydrodynamical isothermal jet model with helical-mode Kelvin–Helmholtz instabilities are used to fit the oscillatory jet trajectory of 3C 48 defined by the bright knotsen
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.rights/dk/atira/pure/core/openaccesspermission/open
dc.titleKinematics of the parsec-scale radio jet in 3C 48en
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
dc.relation.schoolSchool of Physics, Astronomy and Mathematics
rioxxterms.versionofrecordhttps://doi.org/10.1111/j.1365-2966.2009.15899.x
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.rights.accesstyperestrictedAccess


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