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Using the results of a previous X‐ray photoionization modelling of blueshifted Fe K absorption lines on a sample of 42 local radio‐quiet AGNs observed with  XMM–Newton , in this Letter we estimate the location and energetics of the associated ultrafast outflows (UFOs). Due to significant uncertainties, we are essentially able to place only lower/upper limits. On average, their location is in the interval  ∼ 0.0003–0.03 pc ( ∼ 10 2  – 10 4  r s   ) from the central black hole, consistent with what is expected for accretion disc winds/outflows. The mass outflow rates are constrained between  ∼ 0.01 and 1 M ⊙  yr  −1  , corresponding to  &gt; rsim  5–10 per cent of the accretion rates. The average lower/upper limits on the mechanical power are log 42.6–44.6 erg s  −1  . However, the minimum possible value of the ratio between the mechanical power and bolometric luminosity is constrained to be comparable or higher than the minimum required by simulations of feedback induced by winds/outflows. Therefore, this work demonstrates that UFOs are indeed capable to provide a significant contribution to the AGN cosmological feedback, in agreement with theoretical expectations and the recent observation of interactions between AGN outflows and the interstellar medium in several Seyfert galaxies.

Evidence for ultrafast outflows in radio‐quiet AGNs – III. Location and energetics