  We present observations of ionized gas outflows in eleven z$ =1.39-2.59$
radio-loud quasar host galaxies. Data was taken with the integral field
spectrograph (IFS) OSIRIS and the adaptive optics system at the W.M. Keck
Observatory targeting nebular emission lines (H$\beta$, [OIII], H$\alpha$,
[NII] and [SII]) redshifted into the near-infrared (1-2.4 \micron). Outflows
with velocities of 500 - 1700 km\,s$^{-1}$ are detected in 10 systems on scales
ranging from $<1$ kpc to 10 kpc with outflow rates from 8-2400
M$_\odot$yr$^{-1}$. For five sources, the outflow momentum rates are 4-80 times
$L_{AGN}$/c, consistent with outflows being driven by an energy conserving
shock. The five other outflows are either driven by radiation pressure or an
isothermal shock. The outflows are the dominant source of gas depletion, and we
find no evidence for star formation along the outflow paths. For eight objects,
the outflow paths are consistent with the orientation of the jets. Yet, given
the calculated pressures, we find no evidence of the jets currently doing work
on these galactic-scale ionized outflows. We find that galactic-scale feedback
occurs well before galaxies establish a substantial fraction of their stellar
mass, as expected from local scaling relationships.
