  We use the MusE GAs FLOw and Wind (MEGAFLOW) survey to study the kinematics
of extended disk-like structures of cold gas around $z\approx1$ star-forming
galaxies. The combination of VLT/MUSE and VLT/UVES observations allows us to
connect the kinematics of the gas measured through MgII quasar absorption
spectroscopy to the kinematics and orientation of the associated galaxies
constrained through integral field spectroscopy. Confirming previous results,
we find that the galaxy-absorber pairs of the MEGAFLOW survey follow a strong
bimodal distribution, consistent with a picture of MgII absorption being
predominantly present in outflow cones and extended disk-like structures. This
allows us to select a bona-fide sample of galaxy-absorber pairs probing these
disks for impact parameters of 10-70 kpc. We test the hypothesis that the
disk-like gas is co-rotating with the galaxy disks, and find that for 7 out of
9 pairs the absorption velocity shares the sign of the disk velocity,
disfavouring random orbits. We further show that the data are roughly
consistent with inflow velocities and angular momenta predicted by simulations,
and that the corresponding mass accretion rates are sufficient to balance the
star formation rates.
