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 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 ( < 4 pc radius ) and a steep radial dust distribution .
The computed torus using the 1 - 432 \mu m SED provides comparable torus sizes , 5.1 ^ { +0.4 } _ { -0.4 } pc radius , and morphology to the recently resolved 432 \mu m ALMA observations .
This result indicates that the 1 - 20 \mu m wavelength range is not able to probe the full extent of the torus .
The characterization 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 the torus .
The morphology of the dust emission in our 2D image at 432 \mu m is spatially coincident with the cloud distribution , while the morphology of the emission in the 1 - 20 \mu m wavelength range shows an elongated morphology perpendicular to the cloud distribution .
We find that our 2D clumpy torus image at 12 \mu m can produce comparable results to those observed using IR interferometry .