dc.contributor.author | An, T. | |
dc.contributor.author | Hong, X.Y. | |
dc.contributor.author | Hardcastle, M.J. | |
dc.contributor.author | Worrall, D.M. | |
dc.contributor.author | Venturi, T. | |
dc.contributor.author | Pearson, T.J. | |
dc.contributor.author | Shen, Z.Q. | |
dc.contributor.author | Zhao, W. | |
dc.contributor.author | Feng, W.X. | |
dc.date.accessioned | 2010-07-28T08:15:24Z | |
dc.date.available | 2010-07-28T08:15:24Z | |
dc.date.issued | 2010 | |
dc.identifier.citation | An , 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.issn | 0035-8711 | |
dc.identifier.other | dspace: 2299/4699 | |
dc.identifier.uri | http://hdl.handle.net/2299/4699 | |
dc.description | ‘The definitive version is available at www3.interscience.wiley.com '. Copyright Royal Astronomical Society | |
dc.description.abstract | We 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 knots | en |
dc.format.extent | 1538711 | |
dc.language.iso | eng | |
dc.relation.ispartof | Monthly Notices of the Royal Astronomical Society | |
dc.title | Kinematics of the parsec-scale radio jet in 3C 48 | en |
dc.contributor.institution | School of Physics, Astronomy and Mathematics | |
dc.contributor.institution | SPECS Deans Group | |
dc.contributor.institution | School of Physics, Engineering & Computer Science | |
dc.contributor.institution | Department of Physics, Astronomy and Mathematics | |
dc.contributor.institution | Centre for Astrophysics Research (CAR) | |
dc.description.status | Peer reviewed | |
rioxxterms.versionofrecord | 10.1111/j.1365-2966.2009.15899.x | |
rioxxterms.type | Journal Article/Review | |
herts.preservation.rarelyaccessed | true | |