Speaker
Description
Massive stars in star-forming regions inject huge amounts of energy and momentum into the ISM, producing ubiquitous superbubbles, turbulent gas motions and outflows. The coupling efficiency of mechanical stellar feedback and its dependence on metallicity remains uncertain in simulations. High angular resolution observations with integral-field spectrographs (e.g., MUSE), combined with the observations from HST and JWST, allow us to quantitatively compare the energetics of the expanding superbubbles and turbulent motions in ISM, with the star clusters and individual massive stars providing the energy for the observed supersonic gas motions. I will present our recent findings from such observational measurements of the coupling efficiency of mechanical stellar feedback in nearby galaxies. In particular, our results are indicative of a metallicity dependence of the kinetic energy of the feedback-driven structures in the ISM and a significant contribution of pre-SN feedback in their formation.
