  In this work, we investigate the strength and impact of ionised gas outflows
within $z \sim 0.04$ MaNGA galaxies. We find evidence for outflows in 322
galaxies ($12\%$ of the analysed line-emitting sample), 185 of which show
evidence for AGN activity. Most outflows are centrally concentrated with a
spatial extent that scales sublinearly with $R_{\rm e}$. The incidence of
outflows is enhanced at higher masses, central surface densities and deeper
gravitational potentials, as well as at higher SFR and AGN luminosity. We
quantify strong correlations between mass outflow rates and the mechanical
drivers of the outflow of the form $\dot{M}_{\rm out} \propto \rm SFR^{0.97}$
and $\dot{M}_{\rm out} \propto L_{\rm AGN}^{0.55}$. We derive a master scaling
relation describing the mass outflow rate of ionised gas as a function of
$M_{\star}$, SFR, $R_{\rm e}$ and $L_{\rm AGN}$. Most of the observed winds are
anticipated to act as galactic fountains, with the fraction of galaxies with
escaping winds increasing with decreasing potential well depth. We further
investigate the physical properties of the outflowing gas finding evidence for
enhanced attenuation in the outflow, possibly due to metal-enriched winds, and
higher excitation compared to the gas in the galactic disk. Given that the
majority of previous studies have focused on more extreme systems with higher
SFRs and/or more luminous AGN, our study provides a unique view of the
non-gravitational gaseous motions within `typical' galaxies in the low-redshift
Universe, where low-luminosity AGN and star formation contribute jointly to the
observed outflow phenomenology.
