Comparison of SEDs of very massive radio-loud and radio-quiet AGN
  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 \textit{Swift}/BAT catalogue of AGN having
determined optical spectra types and hosting black holes with masses $\rm >
10^{8.5}\,M_{\odot}$. We confirm our previous results, that radio loudness
distribution of \textit{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 $\mu$m) 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.
