  We model the spectropolarimetric signature resulting from the radiative
coupling between the innermost parts of active galactic nuclei (AGNs). We use a
new public version of STOKES, a Monte Carlo radiative transfer code presented
in the first paper of this series. The code has been significantly improved for
computational speed and polarization imaging has been implemented. We couple
continuum sources with equatorial scattering regions, polar outflows, and
toroidal obscuring dust and we study the resulting polarization. We compute a
grid of thermal AGN models for different half-opening angles of the torus and
polar winds. We also consider a range of optical depths for equatorial and
polar electron scattering and investigate how the model geometry influences the
type-1/type-2 polarization dichotomy for thermal AGNs. We put new constrains on
the inflowing medium within the inner walls of the torus. The inflow should be
confined to the common equatorial plane of the torus and the accretion disc and
have a radial optical depth of 1 < tau < 3. Our modeling of type-1 AGNs also
indicates that the torus is more likely to have a large (~ 60{\deg})
half-opening angle. Polarization perpendicular to the axis of the torus may
arise at a type-1 viewing angle for a torus half-opening angle of 30{\deg}-
45{\deg} or polar outflows with an optical depth near unity. Our modeling
suggests that most Seyfert-2 AGN must have a half-opening angle > 60{\deg} to
match the level of perpendicular polarization expected. If outflows are
collimated by the torus inner walls, they must not be optically thick (tau < 1)
in order to preserve the polarization dichotomy. The wind's optical depth is
found not to play a critical role for the degree of polarization of type-2
thermal AGNs but it has a significant impact on the type-1/type-2 polarization
dichotomy when the optical depth exceeds tau = 0.3.
