The impact of pre-supernova feedback and its dependence on environment
  Integral field units enable resolved studies of a large number of
star-forming regions across entire nearby galaxies, providing insight on the
conversion of gas into stars and the feedback from the emerging stellar
populations over unprecedented dynamic ranges in terms of spatial scale,
star-forming region properties, and environments. We use the VLT/MUSE legacy
data set covering the central $35$ arcmin$^{2}$ (${\sim}12$ kpc$^{2}$) of the
nearby galaxy NGC 300 to quantify the effect of stellar feedback as a function
of the local galactic environment. We extract spectra from emission line
regions identified within dendrograms, combine emission line ratios and line
widths to distinguish between HII regions, planetary nebulae, and supernova
remnants, and compute their ionised gas properties, gas-phase oxygen
abundances, and feedback-related pressure terms. For the HII regions, we find
that the direct radiation pressure ($P_\mathrm{dir}$) and the pressure of the
ionised gas ($P_{HII}$) weakly increase towards larger galactocentric radii,
i.e. along the galaxy's (negative) abundance and (positive) extinction
gradients. While the increase of $P_{HII}$ with galactocentric radius is likely
due to higher photon fluxes from lower-metallicity stellar populations, we find
that the increase of $P_\mathrm{dir}$ is likely driven by the combination of
higher photon fluxes and enhanced dust content at larger galactocentric radii.
In light of the above, we investigate the effect of increased pre-supernova
feedback at larger galactocentric distances (lower metallicities and increased
dust mass surface density) on the ISM, finding that supernovae at lower
metallicities expand into lower-density environments, thereby enhancing the
impact of supernova feedback.
