Schematic pictures of AGN structure in nonmergers (top) and late mergers (bottom). Light pink, dark pink, and orange circles represent the chaotic quasi-spherical inflows, dusty torus region, and outflowing material, respectively. In a late merger, X-ray emission from the hot corona is effectively blocked by optically thick failed winds, and stronger UV-driven winds (UFOs) are launched than in a nonmerger (see text). In the high Eddington ratio AGN in a late merger, a part of the inflowing material is blown away by the radiation pressure. These inflows and/or outflows make the AGN deeply “buried.”