Abstract
We perform an analysis of the properties of radio-loud (RL) and radio-quiet (RQ) quasars with MgII broad emission line (i-band magnitude ≤19.1 and z ≤1.9), selected from the parent sample of SDSS DR7 catalogue. For sources with full-width half maxima (FWHM) greater than 15,000 km s−1 (very broad line sample; VBL) we find the radio loud fraction (RLF) to be about 40%. To further investigate this result we compare the bolometric luminosity, optical continuum luminosity, black hole (BH) mass and Eddington ratios of our VBL sample of RL and RQ quasars. Our analysis shows that in our VBL sample space, RL quasars have higher luminosities and BH mass than RQ quasars. The similarity in the distribution of their covering fraction (CF) shows that there is no difference in dust distribution between VBL RL and RQ quasars and hence dust is not affecting our results. We also find that there is no correlation of RL quasar properties with optical continuum luminosity and BH mass.
Highlights
It has been widely reported in the literature that only a small fraction of the quasar population exhibits powerful radio emission in the form of radio jets e.g., [1,2,3,4,5,6,7,8], despite its very first detection in the radio band [9]
In [44], we studied the distributions of bolometric luminosity, optical continuum luminosity at 3000 Å and virial black hole (BH) masses of RL and RQ quasars in our VBL sample and found them to be slightly different from the parent sample of [43]
That our VBL RL quasars have marginally higher luminosities and BH masses compared to RQ quasars while in the parent sample there is no difference of the said properties between
Summary
It has been widely reported in the literature that only a small fraction of the quasar population exhibits powerful radio emission in the form of radio jets e.g., [1,2,3,4,5,6,7,8], despite its very first detection in the radio band [9]. The search for bimodality has spanned different parameter spaces of quasar properties, namely, black hole (BH) mass [13], origin of radio emission [14], accretion rates [15,16], host galaxy properties [15,17,18], and BH spins [19,20,21]. Znajek (BZ) mechanism [19] remains as the most plausible theoretical explanation. It has been observed in many studies, that a correlation exists between emission line luminosities originated from the disk, and radio luminosities of jets in RL quasars [28,29,30,31,32,33,34,35]. It has been further reported that there exists some correlation between the radio luminosity and BH mass in RL quasars [13,36,37,38] but the claim has been debated by other groups [39,40,41,42]
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