  We present gravitational-arc tomography of the cool-warm enriched
circumgalactic medium (CGM) of an isolated galaxy (``G1'') at $z \approx 0.77$.
Combining VLT/MUSE adaptive-optics and Magellan/MagE echelle spectroscopy we
obtain partially-resolved kinematics of MgII in absorption and [OII] in
emission. The unique arc configuration allows us to probe 42 spatially
independent arc positions transverse to G1, plus 4 positions in front of it.
The transverse positions cover G1's minor and major axes at impact parameters
of $\approx 10-30$ kpc and $\approx 60$ kpc, respectively. We observe a direct
kinematic connection between the cool-warm enriched CGM (traced by MgII) and
the interstellar medium (traced by [OII]). This provides strong evidence for
the existence of an extended disc that co-rotates with the galaxy out to tens
of kiloparsecs. The MgII velocity dispersion ($\sigma \approx 30-100$ km
s$^{-1}$, depending on position) is of the same order as the modeled galaxy
rotational velocity ($v_{\rm rot} \approx 80$ km s$^{-1}$), providing evidence
for the presence of a turbulent and pressure-supported CGM component. We regard
the absorption to be modulated by a galactic-scale outflow, as it offers a
natural scenario for the observed line-of-sight dispersion and asymmetric
profiles observed against both the arcs and the galaxy. An extended enriched
co-rotating disc together with the signatures of a galactic outflow, are
telltale signs of metal recycling in the $z\sim 1$ CGM.
