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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.rightsOpen
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
dcterms.dateAccepted2010
rioxxterms.versionofrecordhttps://doi.org/10.1111/j.1365-2966.2009.15899.x
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.rights.accesstypeOpen


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