J/A+A/676/A67ivo://CDS.VizieR/J/A+A/676/A67doi:10.26093/cds/vizier.36760067CDSWatkins E.J.Kreckel K.Groves B.Glover S.C.O.Whitmore B.C.,Leroy A.K.Schinnerer E.Meidt S.E.Egorov O.V.Barnes A.T.Lee J.C.,Boquien M.Chandar R.Chevance M.Dale D.A.Grasha K.Klessen R.S.,Kruijssen J.M.D.Larson K.L.Li J.Mendez-Delgado J.E.Pessa I.,Saito T.Sanchez-Blazquez P.Sarbadhicary S.K.Scheuermann F.,Thilker D.A.Williams T.G.2024-11-06T20:05:33Z2023-08-09T09:43:59ZCDS support team

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

cds-question@unistra.frgalaxiesmolecular-physicsco-line-emissionradio-sourcesStar formation and stellar feedback are interlinked processes that redistribute energy, turbulence, and material throughout galaxies. Because young and massive stars form in spatially clustered environments, they create pockets of expanding gas termed superbubbles, which retain information about the physical processes that drive them. As these processes play a critical role in shaping galaxy discs and regulating the baryon cycle, measuring the properties of superbubbles provides important input for galaxy evolution models. With the wide coverage and high angular resolution (~50-150pc) of the PHANGS-ALMA CO (J=2-1) survey, we can now resolve, identify and characterise a statistically representative number of superbubbles using molecular gas in nearby galaxies. We identify superbubbles by requiring spatial correspondence between shells in CO with stellar populations identified in PHANGS-HST. Then, by combining the properties of the stellar populations with the CO, we quantify the energetics of the stars and constrain feedback models. We visually find 325 cavities across 18 PHANGS--ALMA galaxies, 88 of which have clear superbubble signatures (unbroken shells, central clusters, kinematic signatures of expansion). We measure their radii and expansion velocities using CO (2-1) to dynamically derive their ages and the mechanical power driving the bubbles, which we use to compute the expected properties of the parent stellar populations driving the bubbles. We find consistency between the predicted and derived stellar ages and masses of the stellar populations if we use a supernova (SN) model that injects energy with a coupling efficiency of ~10%. Not only does this confirm that molecular gas accurately traces superbubble properties, but it also provides key observational constraints for superbubble models. We also find evidence that the bubbles are sweeping up gas as they expand, and speculate that these sites have the potential to host new generations of stars. This work demonstrates that molecular superbubbles provide novel quantitative constraints on SNe feedback efficiencies and gas clearing times, and represent a promising environment to search for the propagation of star formation, all of which are needed to understand what sets the observed star formation rates in galaxies.2023A&A...676A..67Whttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/676/A67CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/676/A67https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/676/A67http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/676/A67https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/676/A67https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/676/A67http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/676/A67GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/676/A67/table2 (Superbubble properties ordered by RA derived using CO)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/676/A67/table2?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/676/A67/table2?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/676/A67/table2?GETtext/xml+votable180.050000true24.152888915.77591670.0055555555555555566/17747 17753 18398 24912 26303 27514 27728 27861 28035 28167 33920 33958 34343 34404 34531 36134 36261 40328 46481https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/676/A67?format=asciiRadiodefaultJ/A+A/676/A67/table2Superbubble properties ordered by RA derived using COrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintID[1/88] Bubble ID numbermeta.id;meta.mainintGalaxyWhich galaxy the bubble is located insrc.class.starGalaxycharRAJ2000Right ascension (J2000) (RA_D)pos.eq.ra;meta.mainDEJ2000Declination (J2000) (DEC_D)pos.eq.dec;meta.mainRadBubble Radius (RAD_PC)pcphys.size.radiusintVexpExpansion velocity (V_EXP_KMS)km/sphys.veloc.expansionfloatAgeDynamical age assuming eta=1/4 (AGE_MYR)Myrpos.parallax.dynfloatMshellMolecular mass of the bubble (M_SHELL_MSUN)solMassphys.massdoubleKEKinetic energy of the shell (in erg) (KE_ERG)1e-07Jphys.energydoubleMclusterMass of the cluster with injected energy with a coupling efficiency of ~10% (M_CLST_MSUN)solMassphys.massdoubleNotesLocation of the bubble using Querejeta et al., 2021A&A...656A.133Q (NOTES)meta.notecharJ/A+A/676/A67/table3Mass averaged weighted ages, total mass, and number of clusters found for the multi-scale association catalogues found inside the superbubblesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintID[1/88] Bubble ID number (ID)meta.id;meta.mainintAge16? Mass-weighted avg age of 16pc stellar populations (AGE_16_MYR)Myrtime.agefloatnullablee_Age16? Mass-weighted avg age of 16pc stellar populations error (AGE_16_MYR_ERR)Myrstat.errorfloatnullableMass16? Total mass of 16pc stellar populations (MASS_16_MSUN)solMassphys.massdoublenullablee_Mass16? Total mass of 16pc stellar populations (MASS_16_MSUN_ERR)solMassstat.errordoublenullableN16Number of 16pc stellar populations found/used (NUM_16)meta.numberintAge32? Mass-weighted avg age of 32pc stellar populations (AGE_32_MYR)Myrtime.agefloatnullablee_Age32? Mass-weighted avg age of 32pc stellar populations (AGE_32_MYR_ERR)Myrstat.errorfloatnullableMass32? Total mass of 32pc stellar populations (MASS_32_MSUN)solMassphys.massdoublenullablee_Mass32? Total mass of 32pc stellar populations (MASS_32_MSUN_ERR)solMassstat.errordoublenullableN32Number of 32pc stellar populations found/used (NUM_32)meta.numberintAge64? Mass-weighted avg age of 64pc stellar populations (AGE_64_MYR)Myrtime.agefloatnullablee_Age64? Mass-weighted avg age of 64pc stellar populations (AGE_64_MYR_ERR)Myrstat.errorfloatnullableMass64? Total mass of 64pc stellar populations (MASS_64_MSUN)solMassphys.massdoublenullablee_Mass64? Total mass of 64pc stellar populations (MASS_64_MSUN_ERR)solMassstat.errordoublenullableN64Number of 64pc stellar populations found/used (NUM_64)meta.numberint