AGN TORUS DETECTABILITY AT SUB-MILLIMETER WAVELENGTHS: WHAT TO EXPECT FROM ALMA CONTINUUM DATA

In this talk I will show you a study on the detectability of the emission associated with the AGN dusty structure at sub-mm wavelengths using ALMA, in a theoretical and observational way. Theoretically, we use the Clumpy models from Nenkova et al. together with the mid-infrared to X-ray and the radio fundamental plane scaling relations. We find that it is more likely to detect bigger and denser dusty tori at the highest ALMA frequency (666 GHz/450 μm). Observationally, we use four prototypical AGN: NGC 1052, NGC 1068, NGC 3516, and IZw1, with radio, sub-millimeter, and mid-IR available data.
We fit the mid-IR and radio spectra and we combined and extrapolated both fits to compare the extrapolation of both torus and jet contributors at sub-mm wavelengths. Our observational results are consistent with our theoretical results. The most promising candidate to detect the torus is the QSO IZw1 (therefore, highly accreting sources in general), although it cannot be resolved due to its large distance. We suggest that to explore the detection of a torus at sub-mm wavelengths, it is necessary to perform an SED analysis including radio data, with particular attention to the angular resolution.
 

Date: 
17/01/2019 - 12:30
Speaker: 
Dr. Alice Pasetto
Filiation: 
CRYA, México


Seminars