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We have used the Atacama Large Millimeter Array (ALMA) to map the emission ofthe CO(6-5) molecular line and the 432 {\mu}m continuum emission from the 300pc-sized circumnuclear disk (CND) of the nearby Seyfert 2 galaxy NGC 1068 witha spatial resolution of ~4 pc. These observations spatially resolve the CNDand, for the first time, image the dust emission, the molecular gasdistribution, and the kinematics from a 7-10 pc-diameter disk that representsthe submillimeter counterpart of the putative torus of NGC 1068. We fitted thenuclear spectral energy distribution of the torus using ALMA and near andmid-infrared (NIR/MIR) data with CLUMPY models. The mass and radius of thebest-fit solution for the torus are both consistent with the values derivedfrom the ALMA data alone: Mgas_torus=(1+-0.3)x10^5 Msun and Rtorus=3.5+-0.5 pc.The dynamics of the molecular gas in the torus show non-circular motions andenhanced turbulence superposed on the rotating pattern of the disk. Thekinematic major axis of the CO torus is tilted relative to its morphologicalmajor axis. By contrast with the nearly edge-on orientation of the H2Omegamaser disk, we have found evidence suggesting that the molecular torus isless inclined (i=34deg-66deg) at larger radii. The lopsided morphology andcomplex kinematics of the torus could be the signature of thePapaloizou-Pringle instability, long predicted to likely drive the dynamicalevolution of active galactic nuclei (AGN) tori.

ALMA resolves the torus of NGC 1068: continuum and molecular line emission