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Aims: In this paper, we aim to constrain the properties of dust structures inthe central first parsecs of Active Galactic Nuclei (AGN). Our goal is to studythe required optical depth and composition of different dusty and ionisedstructures.  Methods: We developed a radiative transfer code, MontAGN, optimised forpolarimetric observations in the infrared. With both this code and STOKES,designed to be relevant from the hard X-ray band to near-infrared wavelengths,we investigate the polarisation emerging from a characteristic model of the AGNenvironment. For that purpose, we compare predictions of our models withprevious infrared observations of NGC 1068, and try to reproduce several keypolarisation patterns revealed by polarisation mapping.  Results: We constrain the required dust structures as well as theirdensities. More precisely, we find out that the electron density inside theionisation cone is about $2.0 \times 10^9$ m$^{-3}$ . With structuresconstituted of spherical grains of constant density, we also highlight that thetorus should be thicker than 20 in term of K band optical depth to block directlight from the centre. It should also have a stratification in density, with alesser dense outer rim with an optical depth at 2.2 {\mu}m typically between0.8 and 4 for observing the double scattering effect previously proposed.  Conclusions: We bring constraints on the dust structures in the inner parsecsof an AGN model supposed to describe NGC 1068. When compared to observations,this leads to optical depth of at least 20 in Ks band for the torus of NGC1068, corresponding to $\tau_V \approx 170$, which is within the range ofcurrent estimation based on observations. In the future, we will improve ourstudy by including non uniform dust structures and aligned elongated grains toconstrain other possible interpretations of the observations.

Exploring the inner parsecs of Active Galactic Nuclei using near-infrared high resolution polarimetric simulations with MontAGN