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

Barnes, A. T.; Glover, S. C. O.; Kreckel, K.; Ostriker, E. C.; Bigiel, F.; Belfiore, F.; Beslic, I.; Blanc, G. A.; Chevance, M.; Dale, D. A.; Egorov, O.; Eibensteiner, C.; Emsellem, E.; Grasha, K.; Groves, B. A.; Klessen, R. S.; Kruijssen, J. M. D.; Leroy, A. K.; Longmore, S. N.; Lopez, L.; McElroy, R.; Meidt, S. E.; Murphy, E. J.; Rosolowsky, E.; Saito, T.; Santoro, F.; Schinnerer, E.; Schruba, A.; Sun, J.; Watkins, E. J.; Williams, T. G.

doi:10.1093/mnras/stab2958

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

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Schruba, A.
Infrared and Submillimeter Astronomy, MPI for Extraterrestrial Physics, Max Planck Society;

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Citation

Barnes, A. T., Glover, S. C. O., Kreckel, K., Ostriker, E. C., Bigiel, F., Belfiore, F., et al. (2021). Comparing the pre-SNe feedback and environmental pressures for 6000 H ii regions across 19 nearby spiral galaxies. Monthly Notices of the Royal Astronomical Society, 508(4), 5362-5389. doi:10.1093/mnras/stab2958.

Cite as: https://hdl.handle.net/21.11116/0000-0009-D7F5-0

Abstract

The feedback from young stars (i.e. pre-supernova) is thought to play a crucial role in molecular cloud destruction. In this paper, we assess the feedback mechanisms acting within a sample of 5810 H ii regions identified from the PHANGS-MUSE survey of 19 nearby (<20 Mpc) star-forming, main-sequence spiral galaxies [log(M_⋆/M_⊙) = 9.4–11]. These optical spectroscopic maps are essential to constrain the physical properties of the H ii regions, which we use to investigate their internal pressure terms. We estimate the photoionized gas (P_therm), direct radiation (P_rad), and mechanical wind pressure (P_wind), which we compare to the confining pressure of their host environment (P_de). The H ii regions remain unresolved within our ∼50–100 pc resolution observations, so we place upper (P_max) and lower (P_min) limits on each of the pressures by using a minimum (i.e. clumpy structure) and maximum (i.e. smooth structure) size, respectively. We find that the P_max measurements are broadly similar, and for P_min the P_therm is mildly dominant. We find that the majority of H ii regions are overpressured, P_tot/P_de = (P_therm + P_wind + P_rad)/P_de > 1, and expanding, yet there is a small sample of compact H ii regions with P_tot,max/P_de < 1 (∼1 per cent of the sample). These mostly reside in galaxy centres (R_gal < 1 kpc), or, specifically, environments of high gas surface density; log(Σ_gas/M_⊙ pc⁻²) ∼ 2.5 (measured on kpc-scales). Lastly, we compare to a sample of literature measurements for P_therm and P_rad to investigate how dominant pressure term transitions over around 5 dex in spatial dynamic range and 10 dex in pressure.