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We model the spectropolarimetric signature resulting from the radiativecoupling between the innermost parts of active galactic nuclei (AGNs). We use anew public version of STOKES, a Monte Carlo radiative transfer code presentedin the first paper of this series. The code has been significantly improved forcomputational speed and polarization imaging has been implemented. We couplecontinuum sources with equatorial scattering regions, polar outflows, andtoroidal obscuring dust and we study the resulting polarization. We compute agrid of thermal AGN models for different half-opening angles of the torus andpolar winds. We also consider a range of optical depths for equatorial andpolar electron scattering and investigate how the model geometry influences thetype-1/type-2 polarization dichotomy for thermal AGNs. We put new constrains onthe inflowing medium within the inner walls of the torus. The inflow should beconfined to the common equatorial plane of the torus and the accretion disc andhave a radial optical depth of 1 < tau < 3. Our modeling of type-1 AGNs alsoindicates that the torus is more likely to have a large (~ 60{\deg})half-opening angle. Polarization perpendicular to the axis of the torus mayarise 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 modelingsuggests that most Seyfert-2 AGN must have a half-opening angle > 60{\deg} tomatch the level of perpendicular polarization expected. If outflows arecollimated 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 isfound not to play a critical role for the degree of polarization of type-2thermal AGNs but it has a significant impact on the type-1/type-2 polarizationdichotomy when the optical depth exceeds tau = 0.3.

Modeling optical and UV polarization of AGNs II. Polarization imaging and complex reprocessing