The Sub-parsec, Geometrically Thick, Self-Gravitating Accretion Disk in the Nucleus of NGC 3079

We have mapped, for the first time, the full velocity extent of the water maser emission in NGC 3079. Based on the analysis of the spectral-line maps, we propose a nearly edge-on, massive, thick, and .ared disk for the geometric model of the inner parsec. The disk orbits a mass of ∼ 2 x 106 Mcircledot enclosed within 0.4 pc, most likely a supermassive black hole. The disk is most likely self-gravitating, clumpy, and supportive of star formation. The presence in our VLBI continuum images of an aging synchrotron component, which is not collinear with the previously imaged jet, might be suggestive of changes in jet orientation. The jet may coexist on pc-scales with a wide-angle out flow, that is related to the kpc-scale superbubble and that is inferred from the observation of dense molecular material at high latitudes above the disk