Comparison of SEDs of very massive radio-loud and radio-quiet AGN

Abstract

The main objective of this work is to establish and interpret the dominant spectral components and their differences in radio-loud (RL) and radio-quiet (RQ) AGN with very massive black holes, and accreting at moderate rates. Such a sample is selected from the Swift/BAT catalogue of AGN having determined optical spectra types and hosting black holes with masses > 10 8.5 M . We confirm our previous results, that radio loudness distribution of Swift/BAT AGN is bimodal and that radio galaxies are about two times X-ray louder than their radio-quiet counterparts. We show that the average X-ray loudness (defined as a ratio of luminosity in the 14 − 195 keV band to that at 12 µm) of Type 1 and Type 2 AGN is very similar. This similarity holds for both RL and RQ subsamples and indicates negligible dependence of the observed X-ray luminosities on the inclination angle in both populations.In both the radiative output is dominated by mid-IR and hard X-ray components, and relatively weak UV luminosities indicate large amounts of dust in polar regions.

The origin of X-ray emission in 3CRR sources: hints from mid-infrared Spitzer observations

“…We constructed a high-excitation RLAGN sample to further investigate this question. The moderately strong relationship between α IX and λ IR (figure 2) in this work supports the conclusion of Gupta et al (2018Gupta et al ( , 2020, though no significant relationships between α OX and λ O have been reported in the quasar sample. The similar L X -L UV relationships between RQ and RL quasars also indicate a disk origin of X-ray emission.…”

“…The average X-ray flux in RLAGNs is found to be higher than that in RQAGNs, while its origin is still unclear (e.g., Gupta et al 2018;Zhou & Gu 2020). The additional X-ray emission may be attributed to the contribution of either the jet (Wilkes & Elvis 1987;Li 2019;Zhou & Gu 2020) or the fast rotating black holes (Gupta et al 2018(Gupta et al , 2020. The spinning black hole can improve the radiative efficiency of the accretion disk Upper and lower panels: Histograms for X-ray luminosity at 2 kev and redshift, respectively, where the red slash and green regions represent the narrow-line radio galaxies and quasar samples, respectively.…”

“…However, Gupta et al (2018) recently compiled an excellent sample to investigate the differences of Xray properties between luminous radio galaxies and their radioquiet counterparts, where the black hole mass and Eddington ratio were well selected and the bolometric luminosity were calculated from mid-infrared emission observed by the Wide-field Infrared Survey Explorer (WISE) mission. They argue that the X-ray emission in radio-loud radio galaxies should also come from a disk-corona system because their distribution of the Xray slope is very similar with those of radio-quiet counterparts (see Gupta et al 2018 for details, see also Gupta et al 2020).…”

The Jet-Disk Coupling of Seyfert Galaxies from a Complete Hard X-ray Sample

“…There are slightly larger median values of P j and 20L X in the Seyfert 1s than in Seyfert 2s (see column 3 in Table 1), implying probably a potential contribution of L X from the jet base in Seyfert 1s. This effect would be not significant as noted in [32].…”

“…The hard X-ray selected sample is almost unbiased with respect to absorption compared with the optical estimate for bolometric disk luminosity, and the Seyferts are mostly located in the nearby Universe, reducing as much as possible the selection (e.g., distance) effects [9]. The Seyfert 1s, 2s, and R, S, U sources are equally distributed in redshift [8], and K-corrections are ignored in our analysis since the redshifts for our Seyferts are relatively small (≤ 0.36), and the correlation results in Table 1 should be not caused by the redshift or distance effects [32].…”