  Giant (>100 kpc) nebulae associated with active galaxies provide rich
information about the circumgalactic medium (CGM) around galaxies, its link
with the interstellar medium (ISM) of the hosts and the mechanisms involved in
their evolution. We have studied the giant nebula associated with the Teacup
(z=0.085) quasar based on VLT MUSE integral field spectroscopy with two main
scientific aims: to investigate whether the well known giant (10 kpc) AGN
induced outflow has an impact on the distribution of heavy elements in and
outside the host galaxy, and to establish whether there is a physical and/or
evolutionary link between the CGM and the ISM. We have mapped the O/H and N/O
gas abundances in two spatial dimensions across the giant nebula and within the
galaxy by means of comparing emission line ratios with photoionization model
predictions. We have also compared the kinematics of the giant nebula with that
of the gas and the stars in the host galaxy. The widely studied AGN driven
outflow responsible for the 10 kpc ionized bubble is enhancing the gas metal
abundance up to 10 kpc from the AGN. O/H is solar or slightly higher in the
bubble edges, in comparison with the subsolar abundances across the rest of the
nebula median (O/H~0.63 (O/H)). The giant nebula shows complex kinematics. In
addition to non circular motions, we propose that there is a rotational
component that extends up to the nebular edge. It seems to be kinematically
coupled at least partially with the stellar component and the ISM of the host
galaxy. We conclude that AGN feedback can produce metal enrichment at large
extranuclear distances in galaxies (~10 kpc). The dynamics of the giant nebula
is consistent with CGM studies based on absorption lines that show evidence for
a substantial rotation component in the CGM of numerous galaxies which,
moreover, is often kinematically coupled with the ISM and stars of the
galaxies.
