Abstract
AbstractWe analyze the optical properties of Radio-Loud quasars along the Main Sequence (MS) of quasars. A sample of 355 quasars selected on the basis of radio detection was obtained by cross-matching the FIRST survey at 20cm and the SDSS DR12 spectroscopic survey. We consider the nature of powerful emission at the high-Fe ii end of the MS. At variance with the classical radio-loud sources which are located in the Population B domain of the MS optical plane, we found evidence indicating a thermal origin of the radio emission of the highly accreting quasars of Population A.
Highlights
The 4D Eigenvector 1 (E1) is a powerful tool to contextualize the diversity of observational properties in type-1 AGN(see e.g., Marziani et al 2018 for a recent review)
The shape of the Main Sequence (MS) (Figure 1, left plot) allow us for the subdivision of quasars in two Populations (A and B) and in bins of FWHM(Hβ) and Feii which define a sequence of spectral types (STs): 1) Pop
− Radio morphology as Core Dominated (CD) and FRII sources, selected using the statistical procedure defined by de Vries et al (2006)
Summary
The 4D Eigenvector 1 (E1) is a powerful tool to contextualize the diversity of observational properties in type-1 AGN(see e.g., Marziani et al 2018 for a recent review). Radio-Loud (RL) quasars, defined as relativistic jetted sources, are not distributed uniformly along the MS (Zamfir et al 2008).
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