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The global influence of AGN-driven outflows remains uncertain, due to a lackof large samples with accurately-determined outflow properties. In the secondpaper of this series, we determine the mass and energetics of ionized outflowsis 234 type II AGN, the largest such sample to date, by combining the infraredemission of the dust in the wind (paper I) with the emission line properties.We provide new general expressions for the properties of the outflowing gas,which depend on the ionization state of the gas. We also present a novel methodto estimate the electron density in the outflow, based on optical line ratiosand on the known location of the wind. The inferred electron densities,$n_{\mathrm{e}} \sim 10^{4.5}\,\mathrm{(cm^{-3})}$, are two orders of magnitudelarger than typically found in most other cases of ionized outflows. We arguethat the discrepancy is due to the fact that the commonly-used [SII]-basedmethod underestimates the true density by a large factor. As a result, theinferred mass outflow rates and kinetic coupling efficiencies are$\dot{M}_{\mathrm{out}} \sim 10^{-2}\, \mathrm{(M_{\odot}/yr)}$ and $\epsilon =\dot{E}_{\mathrm{kin}}/L_{\mathrm{bol}} \sim 10^{-5}$ respectively, 1--2 ordersof magnitude lower than previous estimates. Our analysis suggests the existenceof a significant amount of neutral atomic gas at the back of the outflowingionized gas clouds, with mass that is a factor of a few larger than theobserved ionized gas mass. This has significant implications for the estimatedmass and energetics of such flows.

Discovering AGN-driven winds through their infrared emission: II. Mass outflow rate and energetics