Stellar Feedback and Resolved Stellar IFU Spectroscopy in the nearby
  Spiral Galaxy NGC 300
  We present MUSE Integral Field Unit (IFU) observations of five individual HII
regions in two giant (>100 pc in radius) star-forming complexes in the
low-metallicity ($Z$~0.33 $Z_{\odot}$) nearby (D ~ 2 Mpc) dwarf spiral galaxy
NGC 300. We combine the IFU data with high spatial resolution HST photometry to
demonstrate the extraction of stellar spectra and the classification of
individual stars from ground-based data at the distance of 2 Mpc. For the two
star-forming complexes, in which no O-type stars had previously been
identified, we find a total of 13 newly identified O-type stars in the mass
range 15-50 M$_{\odot}$, as well as 4 Wolf-Rayet stars. We use the derived
massive stellar content to analyze the impact of stellar feedback on the HII
regions. As already found for HII regions in the Magellanic Clouds, the
dynamics of the analyzed NGC 300 HII regions are dominated by a combination of
the pressure of the ionized gas and stellar winds. By comparing the derived
ionized gas mass loading factors to the total gas mass loading factor across
the NGC 300 disk, we find that the latter is an order of magnitude higher,
either indicating very early evolutionary stages for these HII regions, or
being a direct result of the multi-phase nature of feedback-driven bubbles.
Moreover, we analyze the relation between the star formation rate and the
pressure of the ionized gas as derived from small (<100 pc) scales, as both
quantities are systematically overestimated when derived on galactic scales.
With the wealth of ongoing and upcoming IFU instruments and programs, this
study serves as a pathfinder for the systematic investigation of resolved
stellar feedback in nearby galaxies, and it delivers the necessary analysis
tools to enable massive stellar content and feedback studies sampling an
unprecedented range of HII region properties across entire galaxies in the
nearby Universe.
