García-Burillo, S.S.García-BurilloCombes, F.F.CombesRamos Almeida, C.C.Ramos AlmeidaUsero, A.A.UseroKrips, M.M.KripsAlonso-Herrero, A.A.Alonso-HerreroAalto, S.S.AaltoCASASOLA, VIVIANAVIVIANACASASOLAHUNT, Leslie KippLeslie KippHUNTMartín, S.S.MartínViti, S.S.VitiColina, L.L.ColinaCostagliola, F.F.CostagliolaEckart, A.A.EckartFuente, A.A.FuenteHenkel, C.C.HenkelMárquez, I.I.MárquezNeri, R.R.NeriSchinnerer, E.E.SchinnererTacconi, L. J.L. J.Tacconivan der Werf, P. P.P. P.van der Werf2020-05-222020-05-2220162041-8205http://hdl.handle.net/20.500.12386/25070We used the Atacama Large Millimeter Array (ALMA) to map the emission of the CO(6-5) molecular line and the 432 μm continuum emission from the 300 pc sized circumnuclear disk (CND) of the nearby Seyfert 2 galaxy NGC 1068 with a spatial resolution of ∼4 pc. These observations spatially resolve the CND and, for the first time, image the dust emission, the molecular gas distribution, and the kinematics from a 7-10 pc diameter disk that represents the submillimeter counterpart of the putative torus of NGC 1068. We fitted the nuclear spectral energy distribution of the torus using ALMA and near- and mid-infrared (NIR/MIR) data with CLUMPY torus models. The mass and radius of the best-fit solution for the torus are both consistent with the values derived from the ALMA data alone: {M}<SUB>{{gas</SUB>}}<SUP>{{torus</SUP>}}=(1+/- 0.3)× {10}<SUP>5</SUP> {M}<SUB>☉ </SUB> and R <SUB>torus</SUB> = 3.5 ± 0.5 pc. The dynamics of the molecular gas in the torus show strong non-circular motions and enhanced turbulence superposed on a surprisingly slow rotation pattern of the disk. By contrast with the nearly edge-on orientation of the H<SUB>2</SUB>O megamaser disk, we found evidence suggesting that the molecular torus is less inclined (I = 34°-66°) at larger radii. The lopsided morphology and complex kinematics of the torus could be the signature of the Papaloizou-Pringle instability, long predicted to likely drive the dynamical evolution of active galactic nuclei tori.STAMPAenArticle10.3847/2041-8205/823/1/L122-s2.0-84971529991000376391700012https://iopscience.iop.org/article/10.3847/2041-8205/823/1/L122016ApJ...823L..12GFIS/05 - ASTRONOMIA E ASTROFISICA