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dc.contributor.authorYoung, S.
dc.contributor.authorAxon, D.J.
dc.contributor.authorHough, J.
dc.contributor.authorFabian, A.C.
dc.contributor.authorWard, M.J.
dc.date.accessioned2009-04-16T12:50:42Z
dc.date.available2009-04-16T12:50:42Z
dc.date.issued1998
dc.identifier.citationYoung , S , Axon , D J , Hough , J , Fabian , A C & Ward , M J 1998 , ' The obscured BLR in the radio galaxy 3C 234 ' Monthly Notices of the Royal Astronomical Society , vol. 294 , no. 3 , pp. 478-484 . https://doi.org/10.1046/j.1365-8711.1998.01243.x
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 164709
dc.identifier.otherPURE UUID: ed8bfe68-f2b3-4497-98f1-9931c91c58c1
dc.identifier.otherdspace: 2299/3190
dc.identifier.otherScopus: 0039290652
dc.identifier.urihttp://hdl.handle.net/2299/3190
dc.descriptionOriginal article can be found at: www3.interscience.wiley.com Copyright Blackwell Publishing / Royal Astronomical Society. DOI: 10.1046/j.1365-8711.1998.01243.x [Full text of this article is not available in the UHRA]
dc.description.abstractWe present spectropolarimetric observations of the radio galaxy 3C 234 at optical and, for the first time, near-IR wavelengths. In agreement with previous observations we detect broad Hα in total and polarized flux, consistent with the scenario in which the central active nucleus is hidden from view and observed via scattered radiation. We model the flux and polarization properties at optical and near-IR wavelengths, which result in a point-source, cone-based scattering geometry in the optical, and an extended source scattering in the near-IR, with a dichroic view to the emission regions, which becomes important only at the longer wavelengths. From this model we calculate an intrinsic Hα luminosity of 4.9×1044 erg s−1, and an extinction to the near-IR emission region of 60 mag for AV. The scattered radiation also undergoes extinction, this time by 1 mag for AV, assuming a source function of a typical stellar-subtracted Seyfert 1 galaxy. Our modelling does not require the presence of a second featureless continuum (FC2). Additionally, we require that the scatterers are in bulk radial outflow at approximately 600 km s−1 to explain an observed increase in the intrinsic polarization of the scattered broad Hα line in the red wing, and blueshifted narrow-line components in polarized flux.en
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.titleThe obscured BLR in the radio galaxy 3C 234en
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
dc.relation.schoolSchool of Physics, Astronomy and Mathematics
rioxxterms.versionofrecordhttps://doi.org/10.1046/j.1365-8711.1998.01243.x
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.rights.accesstyperestrictedAccess


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