2022A&A...662L...6B

Query : 2022A&A...662L...6B

2022A&A...662L...6B - Astronomy and Astrophysics, volume 662L6-6 (2022/6-1)

Linking stellar populations to H II regions across nearby galaxies. I. Constraining pre-supernova feedback from young clusters in NGC 1672.

BARNES A.T., CHANDAR R., KRECKEL K., GLOVER S.C.O., SCHEUERMANN F., BELFIORE F., BIGIEL F., BLANC G.A., BOQUIEN M., DEN BROK J., CONGIU E., CHEVANCE M., DALE D.A., DEGER S., KRUIJSSEN J.M.D., EGOROV O.V., EIBENSTEINER C., EMSELLEM E., GRASHA K., GROVES B., KLESSEN R.S., HANNON S., HASSANI H., LEE J.C., LEROY A.K., LOPEZ L.A., McLEOD A.F., PAN H., SANCHEZ-BLAZQUEZ P., SCHINNERER E., SORMANI M.C., THILKER D.A., UBEDA L., WATKINS E.J. and WILLIAMS T.G.

Abstract (from CDS):


Context. Stellar feedback is one of the fundamental factors regulating the evolution of galaxies. However, we still do not have access to strong observational constraints on the relative importance of the different feedback mechanisms (e.g. radiation, ionised gas pressure, stellar winds) in driving HII region evolution and molecular cloud disruption. To quantify and compare the different feedback mechanisms, the size of an HII region is crucial, whereas samples of well-resolved HII regions are scarce.
Aims. We constrain the relative importance of the various feedback mechanisms from young massive star populations by resolving HII regions across the disk of the nearby star-forming galaxy NGC 1672.
Methods. We combined measurements of ionised gas nebular lines obtained by PHANGS-MUSE, with high-resolution (PSF FWHM ∼ 0.1''; ∼10 pc) imaging from Hubble Space Telescope (HST) in both the narrow-band Hα and broad-band (NUV, U, B, V, I) filters. We identified a sample of 40 isolated, compact HII regions in the HST Hα image. We measured the sizes of these HII regions, which were previously unresolved in seeing-limited ground-based observations. In addition, we identified the ionisation source(s) for each HII region from catalogues produced as part of the PHANGS-HST survey. In doing so, we were able to link young stellar populations with the properties of their surrounding HII regions.
Results. The HST observations allowed us to resolve all 40 regions, with radii between 5 and 40 pc. The HII regions investigated here are mildly dominated by thermal or wind pressure, yet their elevation above the radiation pressure is within the expected uncertainty range. We see that radiation pressure provides a substantially higher contribution to the total pressure than previously found in the literature over similar size scales. In general, we find higher pressures within more compact HII regions, which is driven by the inherent size scaling relations of each pressure term, albeit with significant scatter introduced by the variation in the stellar population properties (e.g. luminosity, mass, age, metallicity).
Conclusions. For nearby galaxies, the combination of MUSE/VLT observations with stellar population and resolved Hα observations from HST provides a promising approach that could yield the statistics required to map out how the importance of different stellar feedback mechanisms evolve over the lifetime of a HII region.

Abstract Copyright: © A. T. Barnes et al. 2022

Journal keyword(s): H II regions - galaxies: evolution - galaxies: star clusters: general

VizieR on-line data: <Available at CDS (J/A+A/662/L6): tablea1.dat>

Nomenclature: Table A.1: [BCK2022] NN (Nos 0-39).

Simbad objects: 44

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Number of rows : 44
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 12317 1
2 NGC 300 GiG 00 54 53.4465638304 -37 41 03.168402396 8.83 8.69 8.13 7.46   ~ 1614 2
3 [BCK2022] 16 HII 04 45 28.462 -59 15 26.50           ~ 2 0
4 [BCK2022] 15 HII 04 45 29.847 -59 15 03.91           ~ 2 0
5 [BCK2022] 19 HII 04 45 29.900 -59 15 00.51           ~ 2 0
6 [BCK2022] 13 HII 04 45 30.217 -59 14 24.11           ~ 2 0
7 [BCK2022] 23 HII 04 45 30.920 -59 14 34.92           ~ 2 0
8 [BCK2022] 12 HII 04 45 31.20770749 -59 14 41.5847447           ~ 1 0
9 [BCK2022] 11 HII 04 45 31.28363074 -59 15 00.8122321           ~ 1 0
10 [BCK2022] 17 HII 04 45 32.303 -59 14 28.93           ~ 2 0
11 [BCK2022] 2 HII 04 45 33.473 -59 14 56.53           ~ 3 0
12 [BCK2022] 24 HII 04 45 33.709 -59 14 38.54           ~ 2 0
13 [BCK2022] 18 HII 04 45 34.181 -59 14 11.74           ~ 2 0
14 [BCK2022] 27 HII 04 45 34.728 -59 14 24.74           ~ 2 0
15 [BCK2022] 36 HII 04 45 35.064 -59 14 54.14           ~ 2 0
16 [BCK2022] 1 HII 04 45 35.894 -59 15 36.55           ~ 2 0
17 [BCK2022] 22 HII 04 45 36.395 -59 14 37.55           ~ 2 0
18 [BCK2022] 28 HII 04 45 36.703 -59 15 34.75           ~ 2 0
19 [BCK2022] 35 HII 04 45 37.981 -59 15 38.56           ~ 3 0
20 [BCK2022] 14 HII 04 45 39.421 -59 14 05.96           ~ 2 0
21 [BCK2022] 37 HII 04 45 39.808 -59 15 17.77           ~ 3 0
22 [BCK2022] 33 HII 04 45 40.278 -59 15 22.97           ~ 2 0
23 [BCK2022] 34 HII 04 45 40.434 -59 15 25.57           ~ 3 0
24 [BCK2022] 25 HII 04 45 40.958 -59 14 27.97           ~ 2 0
25 NGC 1672 SyG 04 45 42.552 -59 14 50.68 10.29 10.53 9.68 9.53 10.2 ~ 461 2
26 [BCK2022] 9 HII 04 45 42.72908784 -59 14 09.1469740           ~ 1 0
27 [BCK2022] 26 HII 04 45 43.931 -59 14 11.98           ~ 2 0
28 [BCK2022] 5 HII 04 45 44.973 -59 14 41.78           ~ 2 0
29 [BCK2022] 39 HII 04 45 48.232 -59 15 04.98           ~ 2 0
30 [BCK2022] 20 HII 04 45 48.233 -59 15 31.18           ~ 3 0
31 [BCK2022] 0 HII 04 45 48.572 -59 15 23.18           ~ 2 0
32 [BCK2022] 32 HII 04 45 48.832 -59 14 30.57           ~ 2 0
33 [BCK2022] 29 HII 04 45 49.015 -59 15 22.77           ~ 2 0
34 [BCK2022] 4 HII 04 45 50.083 -59 14 46.77           ~ 2 0
35 [BCK2022] 38 HII 04 45 51.048 -59 14 39.37           ~ 2 0
36 [BCK2022] 6 HII 04 45 52.247 -59 14 25.57           ~ 2 0
37 [BCK2022] 31 HII 04 45 52.55428856 -59 13 37.9617060           ~ 2 0
38 [BCK2022] 8 HII 04 45 52.948 -59 13 41.17           ~ 3 0
39 [BCK2022] 3 HII 04 45 54.278 -59 13 54.56           ~ 2 0
40 [BCK2022] 30 HII 04 45 54.646 -59 14 38.76           ~ 2 0
41 [BCK2022] 21 HII 04 45 55.089 -59 14 33.36           ~ 2 0
42 [BCK2022] 7 HII 04 45 55.895 -59 14 02.76           ~ 2 0
43 [BCK2022] 10 HII 04 45 55.976 -59 14 43.95           ~ 2 0
44 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 19090 0

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