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We present observations of NGC 1068 covering the $19.7-53.0$ $\mu$mwavelength range using FORCAST and HAWC+ onboard SOFIA. Using theseobservations, high-angular resolution infrared (IR) and sub-mm observations, wefind an observational turn-over of the torus emission in the $30-40$ $\mu$mwavelength range with a characteristic temperature of $70-100$ K. Thiscomponent is clearly different from the diffuse extended emission in the narrowline and star formation regions at 10-100 $\mu$m within the central 700 pc. Wecompute $2.2-432$ $\mu$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 resultgives a small torus size ($<4$ pc radius) and a steep radial dust distribution.The computed torus using the $1-432$ $\mu$m SED provides comparable torussizes, $5.1^{+0.4}_{-0.4}$ pc radius, and morphology to the recently resolved432 $\mu$m ALMA observations. This result indicates that the $1-20$ $\mu$mwavelength range is not able to probe the full extent of the torus. Thecharacterization of the turn-over emission of the torus using the $30-60$$\mu$m wavelength range is sensitive to the detection of cold dust in thetorus. The morphology of the dust emission in our 2D image at 432 $\mu$m isspatially coincident with the cloud distribution, while the morphology of theemission in the $1-20$ $\mu$m wavelength range shows an elongated morphologyperpendicular to the cloud distribution. We find that our 2D \textsc{clumpy}torus image at 12 $\mu$m can produce comparable results to those observed usingIR interferometry.

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