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We study the detectability of the emission associated with the AGN dustystructure at sub-mm wavelengths using ALMA, in a theoretical and observationalway. Theoretically, we use the Clumpy models from Nenkova et al. together withthe mid-infrared to X-ray and the radio fundamental plane scaling relations. Wefind that it is more likely to detect bigger and denser dusty tori at thehighest ALMA frequency (666 GHz/450 micron). We also find that with 1h at 353GHz/850 micron and 10h at 666 GHz/450 micron we can detect, with a highdetection limit, a 1 mJy torus (characteristic of bright AGN). This means, anobject for which the unresolved SED at 12 micron has a flux ~1mJy.Observationally, we use four prototypical AGN: NGC\,1052 (low-luminosity AGN),NGC\,1068 (Type-2), NGC\,3516 (Type 1.5), and IZw1 (QSO), with radio,sub-millimeter, and mid-IR data available. All the mid-infrared spectra arebest fit with the smooth model reported by Fritz et al. A power law and asingle, or a composition of, synchrotron component/s reproduce the cm radiowavelengths. We combined and extrapolated both fits to compare theextrapolation of both torus and jet contributors at sub-mm wavelengths withdata at these wavelengths. Our observational results are consistent with ourtheoretical results. The most promising candidate to detect the torus is theQSO IZw1 (therefore, highly accreting sources in general), although it cannotbe resolved due to the distance of this source. We suggest that to explore thedetection of a torus at sub-mm wavelengths, it is necessary to perform an SEDanalysis including radio data, with particular attention to the angularresolution.

AGN torus detectability at sub-millimeter wavelengths: What to expect from ALMA continuum data