Abstract
A highly significant correlation has been found for quasars, between the line widths (FWHM) of broad Hβ lines and R, the ratio of radio core flux density to the extended radio lobe flux density. The authors discuss how this might be accounted for by a simple relativistic beaming model in which the motion of the broad-line gas is confined to a disk whose axis is perpendicular to the radio axis. The authors comment on how this relation may explain why Fe II lines are apparently weak in many objects with strong extended radio lobes. They also show how the very asymmetric distribution of FWHM may be accounted for in this model. Finally the dependence of the intensity of the [O III] lines on relative core strength is discussed.
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