Abstract
QSOs’ emission lines arise from highest velocity (∼104 km s−1), dense gas within <0.1 parsec of the central engine, out to low-velocity, low-density gas at great distances from the host galaxy. In radio-loud QSOs there are clear indications that the distribution and kinematics of emission-line gas are related to the symmetry axis of the central engine, as defined by the radio jet. These jets originate at nuclear distances <0.1 pc—similar to the highest-velocity emission line gas. There are two ways we can investigate the different environments of radio-loud and radio-quiet QSOs, i.e., those with and without powerful radio jets. One is to look for optical-UV spectroscopic differences between radio-loud and radio-quiet QSOs. The other is to investigate dependences of spectroscopic properties on properties of the powerful jets in radio-loud QSOs. Here we summarize the spectroscopic differences between the two classes, and present known dependences of spectra on radio coredominance, which we interpret as dependences on the angle of the central engine to the line-of-sight. We speculate on what some of the differences may mean.
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Wills, B.J., Brotherton, M.S. (1996). Jets and QSO spectra. In: Kundt, W. (eds) Jets from Stars and Galactic Nuclei. Lecture Notes in Physics, vol 471. Springer, Berlin, Heidelberg. https://doi.org/10.1007/BFb0102609
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DOI: https://doi.org/10.1007/BFb0102609
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