  We characterize the ionized gas outflows in 15 low-redshift star-forming
galaxies, a Valpara\'iso ALMA Line Emission Survey (VALES) subsample, using
MUSE integral field spectroscopy and GAMA photometric broadband data. We
measure the emission-line spectra by fitting a double-component profile, with
the second and broader component being related to the outflowing gas. This
interpretation is in agreement with the correlation between the observed
star-formation rate surface density ($\Sigma_{\mathrm{SFR}}$) and the
second-component velocity dispersion ($\sigma_{\mathrm{2nd}}$), expected when
tracing the feedback component. By modelling the broadband spectra with spectra
energy distribution (SED) fitting and obtaining the star-formation histories of
the sample, we observe a small decrease in SFR between 100 and 10 Myr in
galaxies when the outflow H$\alpha$ luminosity contribution is increased,
indicating that the feedback somewhat inhibits the star formation within these
timescales. The observed emission-line ratios are best reproduced by
photoionization models when compared to shock-ionization, indicating that
radiation from young stellar population is dominant, and seems to be a
consequence of a continuous star-formation activity instead of a bursty event.
The outflow properties such as mass outflow rate ($\sim 0.1\,$M$_\odot$
yr$^{-1}$), outflow kinetic power ($\sim 5.2 \times 10^{-4}\%
L_{\mathrm{bol}}$) and mass loading factor ($\sim 0.12$) point towards a
scenario where the measured feedback is not strong and has a low impact on the
evolution of galaxies in general.
