  Stellar feedback plays a significant role in modulating star formation,
redistributing metals, and shaping the baryonic and dark structure of galaxies
-- however, the efficiency of its energy deposition to the interstellar medium
is challenging to constrain observationally. Here we leverage HST and ALMA
imaging of a molecular gas and dust shell ($M_{H2} \sim 2\times 10^{5} ~{\rm
M}_{\odot}$) in an outflow from the nuclear star forming ring of the galaxy NGC
3351, to serve as a boundary condition for a dynamical and energetic analysis
of the outflowing ionised gas seen in our MUSE TIMER survey. We use
\texttt{STARBURST99} models and prescriptions for feedback from simulations to
demonstrate that the observed star formation energetics can reproduce the
ionised and molecular gas dynamics -- provided a dominant component of the
momentum injection comes from direct photon pressure from young stars, on top
of supernovae, photoionisation heating and stellar winds. The mechanical energy
budget from these sources is comparable to low luminosity AGN, suggesting that
stellar feedback can be a relevant driver of bulk gas motions in galaxy centres
- although here $\lesssim 10^{-3}$ of the ionized gas mass is escaping the
galaxy. We test several scenarios for the survival/formation of the cold gas in
the outflow, including in-situ condensation and cooling. Interestingly, the
geometry of the molecular gas shell, observed magnetic field strengths and
emission line diagnostics are consistent with a scenario where magnetic field
lines aided survival of the dusty ISM as it was initially launched (with mass
loading factor $\lesssim 1$) from the ring by stellar feedback. This system's
unique feedback driven morphology can hopefully serve as a useful litmus test
for feedback prescriptions in magnetohydrodynamical galaxy simulations.
