Unifying the Micro and Macro Properties of AGN Feeding and Feedback

We unify the feeding and feedback of supermassive black holes with the global properties of galaxies, groups, and clusters by linking for the first time the physical mechanical efficiency at the horizon and megaparsec scale. The macro hot halo is tightly constrained by the absence of overheating and overcooling as probed by X-ray data and hydrodynamic simulations (\varepsilon_BH ≃ 10^-3 T_{x,7.4}). The micro flow is shaped by general-relativistic effects tracked by state-of-the-art GR-RMHD simulations (\varepsilon_\bullet ≃ 0.03). The supermassive black hole properties are tied to the X-ray halo temperature T_x, or related cosmic scaling relation (as L_x). The model is minimally based on first principles, such as conservation of energy and mass recycling. The inflow occurs via chaotic cold accretion (CCA), the rain of cold clouds condensing out of the quenched cooling flow and then recurrently funneled via inelastic collisions. Within 100s gravitational radii, the accretion energy is transformed into ultrafast 10^4 km s^-1 outflows (UFOs) ejecting most of the inflowing mass. At larger radii, the energy-driven outflow entrains progressively more mass: at roughly kiloparsec scale, the velocities of the hot/warm/cold outflows are a few 10^3, 1000, and 500 km s^-1, with median mass rates ∼ 10, 100, and several 100 M_☉ yr-1, respectively. The unified CCA model is consistent with the observations of nuclear UFOs and ionized, neutral, and molecular macro outflows. We provide step-by-step implementation for subgrid simulations, (semi)analytic works, or observational interpretations that require self-regulated AGN feedback at coarse scales, avoiding the a-posteriori fine-tuning of efficiencies.