Comparison of the alignment of the hot dusty disc models. The models themselves are not shown, only the implied interpretation of the observed continuum features. Left: Model 3 is the favoured interpretation, in which the ring-like structure in the K-band continuum arises from (partially) optically thin clouds (same as in Fig.4). In this case, it traces a disc that has a similar position angle and aspect ratio to the inner geometry of NGC 1068, is co-planar with the maser emission and traces the dust sublimation ring. Right: Model 4 comprises optically thick clouds, and the alignment of the mid-plane (indicated by the large dashed ring) to the NIR continuum observed with GRAVITY is given by radiative transfer simulations using the CAT3D-WIND model (Hönig & Kishimoto 2017). In Model 4, the near side of the mid-plane as traced by the masers, but is completely obscured in the K-band. The K-band emission originates from the τ = 1 surface of the hot disc, that is still geometrically thin. But all the structure in the image is assigned to chance effects of patchy obscuration along the line of sight.