respectively. These velocities are above the escape velocity from the gravitational potential of massive galaxies, suggesting this gas is outflowing [@villar03; @nesvadba06a; @nesvadba08]. These structures are in most cases elongated along an axis that is approximately aligned with the axis of the radio jet, and have sizes that are smaller than the jet size, and dynamical times comparable to the radio-jet lifetime. This has previously been considered evidence that these are outflows of warm ionized gas that has been entrained by the expanding cocoon of hot, shocked gas inflated by the radio jet [@nesvadba06a; @nesvadba08].

Here we present an analysis of 33 powerful radio galaxies at redshifts z$\ge$2 with new SINFONI observations, revisiting the kinematic and energetic signatures of AGN feedback as previously described for individual sources by @nesvadba06a [@nesvadba07b; @nesvadba08] and for a small sample of lower-power radio galaxies by @collet14b. We confirm the basic previous results, and significantly expand them, in particular by studying the trends between radio power and various gas properties. We find a good overall qualitative agreement with hydrodynamic jet models, but significant differences when compared with more detailed predictions.

The paper is organized as follows: In §\[sec:observations\] we describe our sample and observations before 