The emission and distribution of dust of the torus of NGC 1068

We present observations of NGC 1068 covering the \(19.7-53.0\) \(\mu\)m wavelength range using FORCAST and HAWC+ onboard SOFIA. Using these observations, high-angular resolution infrared (IR) and sub-mm observations, we find an observational turn-over of the torus emission in the \(30-40\) \(\mu\)m wavelength range with a characteristic temperature of \(70-100\) K. This component is clearly different from the diffuse extended emission in the narrow line and star formation regions at 10-100 \(\mu\)m within the central 700 pc. We compute \(2.2-432\) \(\mu\)m 2D images using the best inferred \textsc{clumpy} torus model based on several nuclear spectral energy distribution (SED) coverages. We find that when \(1-20\) \(\mu\)m SED is used, the inferred result gives a small torus size (\(