J/A+A/703/A103ivo://CDS.VizieR/J/A+A/703/A103doi:10.26093/cds/vizier/bc-nz/lbadCDSEgorov O.V.Leroy A.K.Sandstrom K.Kreckel K.Baron D.Belfiore F.,Chown R.Sutter J.Boquien M.Canal i Saguer M.Congiu E.Dale D.A.,Egorova E.Huber M.Li J.Williams T.G.Chastenet J.Chiang I-D.,Gerasimov I.Hassani H.Kim H.Koziol H.Lee J.C.McClain R.L.,Mendez Delgado J.E.Pan H.-A.Pathak D.Rosolowsky E.,Sarbadhicary S.K.Schinnerer E.Thilker D.Ubeda L.Weinbeck T.2026-08-03T06:58:56Z2025-11-18T11:18:40ZCDS support team

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

cds-question@unistra.frgalaxiesinterstellar-mediuminfrared-photometryh-ii-regionssupernova-remnantschemical-abundancesPolycyclic aromatic hydrocarbons (PAHs) are widespread in the interstellar medium (ISM) of solar metallicity galaxies, where they play a critical role in ISM heating, cooling, and reprocessing stellar radiation. The PAH fraction, the abundance of PAHs relative to total dust mass, is a key parameter in ISM physics. Using JWST and MUSE observations of 42 galaxies from the PHANGS survey, we analyze the PAH fraction in over 17000 HII regions spanning a gas-phase oxygen abundance of 12+log(O/H)=8.0-8.8 (Z~0.2-1.3Z_{sun}_), and ~400 isolated supernova remnants (SNRs). We find a significantly lower PAH fraction toward HII regions compared to a reference sample of diffuse ISM areas at matched metallicity. At 12+log(O/H)>8.2, the PAH fraction toward HII regions is strongly anti-correlated with the local ionization parameter, suggesting that PAH destruction is correlated with ionized gas and/or hydrogen-ionizing UV radiation. At lower metallicities, the PAH fraction declines steeply in both HII regions and the diffuse ISM, likely reflecting less efficient PAH formation in metal-poor environments. Carefully isolating dust emission from the vicinity of optically-identified supernova remnants, we see evidence for selective PAH destruction from measurements of lower PAH fractions, which is, however, indistinguishable at ~50pc scales. Overall, our results point to ionizing radiation as the dominant agent of PAH destruction within HII regions, with metallicity playing a key role in their global abundance in galaxies.2025A&A...703A.103Ehttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/703/A103CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/A+A/690/A161 : Discovery of ~2200 new supernova remnants (Li+, 2024)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/703/A103https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/703/A103http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/703/A103https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/703/A103https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/703/A103http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/703/A103GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/703/A103/tabled1 (Catalog with our measurements)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/703/A103/tabled1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/703/A103/tabled1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/703/A103/tabled1?GETtext/xml+votable180.050000true52.8957-51.899020.0055555555555555566/4149 4511 17747 17753-17754 18398 24912 25762 25790 26119 26303 26338 26472 27030 27512 27514 27643 27728 27738 27861 27905 27942 28033 28035 28167 28208 28264 33654 33920-33921 33958 34273 34343 34382 34404 34493 34495 34531 35993 36134 36261 40328 46481 46495 46519 46549https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/703/A103?format=asciiInfrareddefaultJ/A+A/703/A103/tabled1Catalog with our measurementsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIDRegion ID (1)meta.id;meta.mainintGalNameGalaxy namemeta.id.parentcharRAJ2000Right ascension (J2000) of the regiondegpos.eq.ra;meta.mainindexedDEJ2000Declination (J2000) of the regiondegpos.eq.dec;meta.mainindexednebTypeType of nebula (HII region or SNR)src.classcharrcircangCircularized radius, based on the MUSE data (2)arcsecphys.angSize;srcdoublercircangHST? Circularized radius, based on the HST data (3)arcsecphys.angSize;srcdoublenullablercircMUSEpsfRatio of r_circ_ang to the average PSF of the MUSE dataphys.angSize;srcdoublePhysAreaPhysical area covered by the region based on its borders derived from the MUSE data (2)pc**2phys.area;obs.fielddoublePhysAreaHST? Physical area covered by the region based on its borders derived from the MUSE data (3)pc**2phys.area;obs.fielddoublenullableF770WAverage brightness in F770W JWST/MIRI band (4)MJy/srphot.flux.density;em.opt.I;stat.meandoublee_F770WUncertainty of the average F770W brightness (4)MJy/srstat.errordoubleF770WssAverage brightness in F770W band, corrected for stellar continuum (4)MJy/srphot.flux.density;em.opt.I;stat.meandoublee_F770WssUncertainty of the average star-subtracted F770W brightness (4)MJy/srstat.errordoubleF1130W? Average brightness in F1130W JWST/MIRI band (4)MJy/srphot.flux.density;stat.meandoublenullablee_F1130W? Uncertainty of the average F1130W brightness (4)MJy/srstat.errordoublenullablee_FHaUncertainties of the flux in Halpha emission line (in 10^-17^erg/cm^2/s) (5)1e-20W.m**-2stat.errordoubleFHb? Total flux in Hbeta emission line (in 10^-17^erg/cm^2/s) (5)1e-20W.m**-2phot.flux;em.line.Hbetadoublenullablee_FHb? Uncertainties of the flux in Hbeta emission line (in 10^-17^erg/cm^2/s) (5)1e-20W.m**-2stat.errordoublenullableFOIII5007Total flux in [OIII]5007A emission line (in 10^-17^erg/cm^2/s) (5)1e-20W.m**-2phot.flux;spect.linedoublee_FOIII5007? Uncertainties of the flux in [OIII]5007A line (in 10^-17^erg/cm^2/s) (5)1e-20W.m**-2stat.errordoublenullableFNII6584Total flux in [NII]6584A emission line (in 10^-17^erg/cm^2/s) (5)1e-20W.m**-2phot.flux;spect.linedoubleF2100WAverage brightness in F2100W JWST/MIRI band (4)MJy/srphot.flux.density;stat.meandoublee_F2100WUncertainty of the average F2100W brightness (4)MJy/srstat.errordoubleFHaTotal flux in Halpha emission line (in 10^-17^erg/cm^2/s) (5)1e-20W.m**-2phot.flux;em.line.Halphadoublee_FNII6584Uncertainties of the flux in [NII]6584A line (in 10^-17^erg/cm^2/s) (5)1e-20W.m**-2stat.errordoubleFSII6717Total flux in [SII]6717A emission line (in 10^-17^erg/cm^2/s) (5)1e-20W.m**-2phot.flux;spect.linedoublee_FSII6717Uncertainties of the flux in [SII]6717A line (in 10^-17^erg/cm^2/s) (5)1e-20W.m**-2stat.errordoubleFSII6731Total flux in [SII]6731A emission line (in 10^-17^erg/cm^2/s) (5)1e-20W.m**-2phot.flux;spect.linedoublee_FSII6731Uncertainties of the flux in [SII]6731A line (in 10^-17^erg/cm^2/s) (5)1e-20W.m**-2stat.errordoubleFSIII9069Total flux in [SIII]9069A emission line (in 10^-17^erg/cm^2/s) (5)1e-20W.m**-2phot.flux;spect.linedoublee_FSIII9069Uncertainties of the flux in [SIII]9069A line (in 10^-17^erg/cm^2/s) (5)1e-20W.m**-2stat.errordoubleMetScalOxygen abundance (6)phys.abunddoublee_MetScalUncertainties of the oxygen abundance (6)stat.errordoubleRPAH? R_PAH_ measurements (7)stat.fit.paramdoublenullablee_RPAH? Uncertainties of RPAHstat.errordoublenullableRPAHstR_PAH_* measurements (8)stat.fit.paramdoublee_RPAHstUncertainties of RPAH*stat.errordouble