  We use optical Integral Field Spectroscopy (IFU) to study the gas emission
structure and kinematics in the inner 3.4$\times$4.9 kpc$^2$ region of the
galaxy UGC 8782 (3C 293), host of a radio loud Active Galactic Nucleus (AGN).
The observations were performed with the GMOS-IFU on the Gemini North
telescope, resulting in a spatial resolution of $\sim725$ pc at the distance of
the galaxy. While the stars present ordered rotation following the orientation
of the large scale disc, the gas shows a disturbed kinematics. The
emission-line profiles present two kinematic components: a narrow
($\sigma\lesssim200$ km s$^{-1}$) component associated with the gas in the disc
of the galaxy and a broad ($\sigma\gtrsim200$ km s$^{-1}$) component produced
by gas outflows. Emission-line ratio diagrams indicate that the gas in the disc
is excited by the AGN radiation field, while the emission of the outflow
includes additional contribution of shock excitation due to the interaction of
the radio jet with the environment gas. Deviations from pure rotation, of up to
30 km s$^{-1}$, are observed in the disc component and likely produced by a
previous merger event. The broad component is blueshifted by $\sim150-500$ km
s$^{-1}$ relative to the systemic velocity of the galaxy in all locations. We
construct radial profiles of the mass outflow rate and kinetic power of the
ionized gas outflows, which have the maximum values at $\sim1$ kpc from the
nucleus with peak values of $\dot{M}_{\rm out,\Delta R}=0.5\pm0.1$ M$_\odot$
yr$^{-1}$ and $\dot{K}_{\rm out,\Delta R} =$(6.8$\pm$1.1)$\times$10$^{41}$ erg
s$^{-1}$. The kinetic coupling efficiency of these outflows is in the range of
1$-$3 per cent, indicating that they could be powerful enough to affect the
star formation in the host galaxy as predicted by theoretical simulations.
