Comparing the pre-SNe feedback and environmental pressures for 6000 HII regions across 19 nearby spiral galaxies
Date Issued
2021
Author(s)
Barnes, A. T.
•
Glover, S. C. O.
•
Kreckel, K.
•
Ostriker, E. C.
•
Bigiel, F.
•
•
Bešlić, 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.
•
E. Rosolowsky,
•
Saito, T.
•
Santoro, F.
•
Schinnerer, E.
•
Schruba, A.
•
Sun, J.
•
Watkins, E. J.
•
Williams, T. G.
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 HII regions identified from
the PHANGS-MUSE survey of 19 nearby ($<$ 20 Mpc) star-forming, main sequence
spiral galaxies (log($M_\star$/M$_\odot$)= 9.4 $-$ 11). These optical
spectroscopic maps are essential to constrain the physical properties of the
HII regions, which we use to investigate their internal pressure terms. We
estimate the photoionised gas ($P_\mathrm{therm}$), direct radiation
($P_\mathrm{rad}$), and mechanical wind pressure ($P_\mathrm{wind}$), which we
compare to the confining pressure of their host environment ($P_\mathrm{de}$).
The HII regions remain unresolved within our ${\sim}50{-}100$ pc resolution
observations, 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) and
maximum (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 regions
are over-pressured, $P_\mathrm{tot}/P_\mathrm{de} =
(P_\mathrm{therm}+P_\mathrm{wind}+P_\mathrm{rad})/P_\mathrm{de} > 1$, and
expanding, yet there is a small sample of compact HII regions with
$P_\mathrm{tot,max}/P_\mathrm{de} < 1$ ($\sim$1% of the sample). These mostly
reside in galaxy centres ($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 (measured
on kpc-scales). Lastly, we compare to a sample of literature measurements for
$P_\mathrm{therm}$ and $P_\mathrm{rad}$ to investigate how dominant pressure
term transitions over around 5dex in spatial dynamic range and 10 dex in
pressure.
Volume
508
Issue
4
Start page
5362
Issn Identifier
0035-8711
Ads BibCode
2021MNRAS.508.5362B
Rights
open.access
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