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The feedback from young stars (i.e. pre-supernova) is thought to play acrucial role in molecular cloud destruction. In this paper, we assess thefeedback mechanisms acting within a sample of 5810 HII regions identified fromthe PHANGS-MUSE survey of 19 nearby ($<$ 20 Mpc) star-forming, main sequencespiral galaxies (log($M_\star$/M$_\odot$)= 9.4 $-$ 11). These opticalspectroscopic maps are essential to constrain the physical properties of theHII regions, which we use to investigate their internal pressure terms. Weestimate the photoionised gas ($P_\mathrm{therm}$), direct radiation($P_\mathrm{rad}$), and mechanical wind pressure ($P_\mathrm{wind}$), which wecompare to the confining pressure of their host environment ($P_\mathrm{de}$).The HII regions remain unresolved within our ${\sim}50{-}100$ pc resolutionobservations, so we place upper ($P_\mathrm{max}$) and lower ($P_\mathrm{min}$)limits on each of the pressures by using a minimum (i.e. clumpy structure) andmaximum (i.e. smooth structure) size, respectively. We find that the$P_\mathrm{max}$ measurements are broadly similar, and for $P_\mathrm{min}$ the$P_\mathrm{therm}$ is mildly dominant. We find that the majority of HII regionsare over-pressured, $P_\mathrm{tot}/P_\mathrm{de} =(P_\mathrm{therm}+P_\mathrm{wind}+P_\mathrm{rad})/P_\mathrm{de} > 1$, andexpanding, yet there is a small sample of compact HII regions with$P_\mathrm{tot,max}/P_\mathrm{de} < 1$ ($\sim$1% of the sample). These mostlyreside in galaxy centres ($R_\mathrm{gal}<1$kpc), or, specifically,environments of high gas surface density;log($\Sigma_\mathrm{gas}/\mathrm{M_\odot} \mathrm{pc}^{-2}$)$\sim$2.5 (measuredon kpc-scales). Lastly, we compare to a sample of literature measurements for$P_\mathrm{therm}$ and $P_\mathrm{rad}$ to investigate how dominant pressureterm transitions over around 5dex in spatial dynamic range and 10 dex inpressure.

Comparing the pre-SNe feedback and environmental pressures for 6000 HII regions across 19 nearby spiral galaxies