  A prominent jet-driven outflow of CO(2-1) molecular gas is found along the
kinematic minor axis of the Seyfert 2 galaxy ESO 420-G13, at a distance of
$340-600\, \rm{pc}$ from the nucleus. The wind morphology resembles a
characteristic funnel shape, formed by a highly collimated filamentary emission
at the base, likely tracing the jet propagation through a tenuous medium, until
a bifurcation point at $440\, \rm{pc}$ where the jet hits a dense molecular
core and shatters, dispersing the molecular gas into several clumps and
filaments within the expansion cone. We also trace the jet in ionised gas
within the inner $\lesssim 340\, \rm{pc}$ using the [NeII]$_{\rm 12.8 \mu m}$
line emission, where the molecular gas follows a circular rotation pattern. The
wind outflow carries a mass of $\sim 8 \times 10^6\, \rm{M_\odot}$ at an
average wind projected speed of $\sim 160\, \rm{km\,s^{-1}}$, which implies a
mass outflow rate of $\sim 14\, \rm{M_\odot\,yr^{-1}}$. Based on the structure
of the outflow and the budget of energy and momentum, we discard radiation
pressure from the active nucleus, star formation, and supernovae as possible
launching mechanisms. ESO 420-G13 is the second case after NGC 1377 where the
presence of a previously unknown jet is revealed due to its interaction with
the interstellar medium, suggesting that unknown jets in feeble radio nuclei
might be more common than expected. Two possible jet-cloud configurations are
discussed to explain the presence of an outflow at such distance from the AGN.
The outflowing gas will likely not escape, thus a delay in the star formation
rather than quenching is expected from this interaction, while the feedback
effect would be confined within the central few hundred parsecs of the galaxy.
