Left panel: reconstructed full face-on SED of the adopted CAT3D models, adding to the dusty torus SED (red solid line for model B and green solid line for model C) a dust-free view of the Hönig & Kishimoto (2010) intrinsic SED of the accretion disk. The dotted line is the SED of the accretion disk scaled to the observed optical/UV datapoints. Central panel: SEDs for models A (blue) and B (red) using the central source only and adopting two different inclination angles of the polar axis of the torus with respect to that of the host: i = 0 (dashed lines) and 20° (dotted lines). Right panel: SEDs for model A but with dust mass reduced by a factor of 10 (dashed line), and by using the original dust mass but increasing the resolution and adopting a full grain size distribution plus stochastic heating (dotted line). The solid line is the reference model from the left panel of Fig. 4.