matter. This could be a geometrical effect, if the disc and the torus subtend a small solid angle from the corona. Alternatively, the X-ray coronal emission could be anisotropic [@beckmann2004; @kamraj2017]. For example, if the X-ray corona is outflowing at relativistic velocities, its emission would be beamed away from the disc, possibly producing a weaker reflection component [@malzac2001].

The 2–10 keV luminosity extrapolated from the IBIS time-averaged spectrum is [($1.3 \pm 0.1) \times 10^{43}$]{} [ergs s$^{-1}$]{} for [NGC 4388]{} and [($1.33 \pm 0.03) \times 10^{43}$]{} [ergs s$^{-1}$]{}for [NGC 2110]{}, respectively. Using the bolometric correction of [@marconi2004], we estimate a bolometric luminosity of $ \sim {2.5 \times 10^{44}}$ [ergs s$^{-1}$]{} for both sources. Given the different black hole mass, this yields a different accretion rate in Eddington units, of $\sim 0.23$ for [NGC 4388]{} and $\sim 0.01$ for [NGC 2110]{}. The latter is in agreement with the estimate reported by [@marinucci2015], with the caveat that the estimate of black hole mass in [NGC 2110]{} has a large uncertainty.

The X-ray corona of AGNs can produce radio synchrotron emission , as recently observed in the two bright Seyferts IC 4329A and NGC 985 . This could explain the radio emission seen in 