We present K , L and M diffraction-limited images of NGC~1068 , obtained with NAOS+CONICA at VLT/YEPUN over a 3.5″ \times 3.5″region around the central engine . Hot dust ( T _ { col } = 550-650 K ) is found to be distributed in three main structurally different regions : ( a ) in the true nucleus , seen as a quasi-spherical , however slightly NS elongated , core of extremely hot dust , resolved in K and L with respective diameters of \approx 5 pc and 8.5 pc ; ( b ) along the North-South direction , according to a spiral arm like structure and a southern tongue ; ( c ) as a set of parallel elongated nodules ( wave-like ) on each side , albeit mainly at north , of the jet , at a distance of 50 to 70 pc from the central engine . The IR images reveal several structures also clearly observed on either radio maps , mid-IR or HST UV-visible maps , so that a very precise registration of the respective emissions can be done for the first time from UV to 6 cm . These results do support the current interpretion that source ( a ) corresponds to emission from dust near sublimation temperature delimiting the walls of the cavity in the central obscuring torus . Structure ( b ) is thought to be a mixture of hot dust and active star forming regions along a micro spiral structure that could trace the tidal mechanism bringing matter to the central engine . Structure c ) which was not known , exhibits too high a temperature for “ classical ” grains ; it is most probably the signature of transiently heated very small dust grains ( VSG ) : nano-diamonds , which are resistant and can form in strong UV field or in shocks , are very attractive candidates . The “ waves ” can be condensations triggered by jet induced shocks , as predicted by recent models . First estimates , based on a simple VSG model and on a detailed radiative transfer model , do agree with those interpretations , both qualitatively and quantitatively .