A quantitative demonstration that stellar feedback locally regulates
  galaxy growth
  We have applied stellar population synthesis to 500 pc sized regions in a
sample of 102 galaxy discs observed with the MUSE spectrograph. We derived the
star formation history and analyse specifically the "recent" ($20\rm{Myr}$) and
"past" ($570\rm{Myr}$) age bins. Using a star formation self-regulator model we
can derive local mass-loading factors, $\eta$ for specific regions, and find
that this factor depends on the local stellar mass surface density, $\Sigma_*$,
in agreement with the predictions form hydrodynamical simulations including
supernova feedback. We integrate the local $\eta$-$\Sigma_*$ relation using the
stellar mass surface density profiles from the Spitzer Survey of Stellar
Structure in Galaxies (S4G) to derive global mass-loading factors,
$\eta_{\rm{G}}$, as a function of stellar mass, $M_*$. The
$\eta_{\rm{G}}$-$M_*$ relation found is in very good agreement with
hydrodynamical cosmological zoom-in galaxy simulations. The method developed
here offers a powerful way of testing different implementations of stellar
feedback, to check on how realistic are their predictions.
