Probability to observe microlensing (de)magnification |Δm| > 0.1 mag as a function of the fraction of the flux f_AD originating from the accretion disc. The solid line is for a compact model for the torus and the dashed line for an extended model. The blue, red and green curves correspond to different source bolometric luminosities. Panels from left to right correspond to κ_∗ = 0.07, κ_∗ = 0.3, κ_∗ = 1.0. Probabilities are calculated for λ_rest = 2.2 μm.