J/A+A/662/L6ivo://CDS.VizieR/J/A+A/662/L6doi:10.26093/cds/vizier.36629006CDSBarnes 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.Williams T.G.2023-08-07T08:20:50Z2022-12-30T08:50:33ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frgalaxiesh-ii-regionsOne of the fundamental factors regulating the evolution of galaxies is stellar feedback. However, we still do not have 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. In this letter, 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. We combine measurements of ionised gas nebular lines obtained by PHANGS-MUSE, with high-resolution imaging from the HST in both the narrow-band H{alpha} and broad-band filters. We identify a sample of 40 isolated, compact HII regions in the HST H{alpha} image, for which we measure the sizes that were previously unresolved in seeing-limited ground-based observations. Additionally, we identify the ionisation source(s) for each HII region from catalogues produced as part of the PHANGS-HST survey. We find that the HII regions investigated 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). For nearby galaxies, here we provide 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 an HII region.2022A&A...662L...6Bhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/662/L6CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/662/L6https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/662/L6http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/662/L6https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/662/L6https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/662/L6http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/662/L6GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/662/L6/tablea1 (Properties of the HII region sample)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/662/L6/tablea1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/662/L6/tablea1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/662/L6/tablea1?GETtext/xml+votable180.050000true71.4523458830084-59.2564217951650.0055555555555555566/33920-33921https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/662/L6?format=asciidefaultJ/A+A/662/L6/tablea1Properties of the HII region samplerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintID[0/39] Identifiermeta.id;meta.mainintRAJ2000Central Right ascension (J2000)degpos.eq.ra;meta.mainDEJ2000Central Declination (J2000)degpos.eq.dec;meta.mainRadRadiuspcphys.size.radiusdoubleRgal/ReffGalactocentric radius (normalised by the effective radius)phys.size.radius;arith.ratiodoublelogHacExtinction corrected H{alpha} fluxlog(mW.m**-2)phot.flux;em.line.HalphadoubleE(B-V)Extinctionmagphot.color.excessdoublelogLHaExtinction corrected H{alpha} luminositylog(solLum)phys.luminosity;em.line.HalphadoubleMetMetallicity (units in 12+log10(O/H))phys.abund.FedoubleAgeStellar population ageMyrtime.agedoublelogMassStellar population masslog(solMass)phys.massdoublelogLbolStellar population bolometric luminositylog(solLum)phys.luminositydoublelogLmechMechanical luminositylog(1e-07W)phys.luminositydoubledM/dtMass loss ratelog(g.s**-1)phys.mass.lossdoubleneElectron densitycm**-3phys.density;phys.electrondoublelogPthermThermal pressurelog(K.cm**-3)phys.pressuredoublelogPradRadiation pressurelog(K.cm**-3)phys.absorptiondoublelogPwindWind pressurelog(K.cm**-3)phys.pressuredoubleSimbadSimbad column added by the CDSmeta.ref.urlchar