Orateur
Description
A significant number of Active Galactic Nuclei (AGN) are known to be heavily obscured: the strong UV-X emission arising from the accretion disk and the associated broad emission lines cannot be directy observed. It is now commonly accepted that this obscuration is due to a structure surrounding the central engine, called the dusty torus. This torus is known to be made of gaz and dust, to be clumpy and to be parsec-scale.
I present my modelling of NGC 1068's dusty torus, constrained with a GRAVITY observation. This instrument is incredibly well designed for such a study: its spectral range (K band, 2.0 - 2.4 microns) is very sensitive to the hot dust at ~1500K which is present in the inner region of the torus, and more importantly its incredibly high angular resolution (up to 4 mas) allows to fully resolve the dusty torus.
Our analysis reveals a structure significantly different from what was expected.
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