J/MNRAS/508/5425ivo://CDS.VizieR/J/MNRAS/508/5425doi:10.26093/cds/vizier.75085425CDSMcleod A.F.Ali A.A.Chevance M.Della Bruna L.Schruba A.,Stevance H.F.Adamo A.Kruijssen J.M.D.Longmore S.N.Weisz D.R.,Zeidler P.2024-12-04T20:14:20Z2024-10-10T14:22:04ZCDS support team

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

cds-question@unistra.frgalaxiesh-ii-regionssupernova-remnantsnebulaevisible-astronomyspectrophotometryspectroscopygalaxy-radiichemical-abundancesnarrow-band-photometryatomic-spectroscopyastrometryIntegral field units enable resolved studies of a large number of star-forming regions across entire nearby galaxies, providing insight on the conversion of gas into stars and the feedback from the emerging stellar populations over unprecedented dynamic ranges in terms of spatial scale, star-forming region properties, and environments. We use the Very Large Telescope (VLT) MUSE (Multi Unit Spectroscopic Explorer) legacy data set covering the central 35 arcmin^2^ (~12 kpc^2^) of the nearby galaxy NGC 300 to quantify the effect of stellar feedback as a function of the local galactic environment. We extract spectra from emission line regions identified within dendrograms, combine emission line ratios and line widths to distinguish between H II regions, planetary nebulae, and supernova remnants, and compute their ionized gas properties, gas-phase oxygen abundances, and feedback-related pressure terms. For the H II regions, we find that the direct radiation pressure (P_dir_) and the pressure of the ionized gas (P_HII_) weakly increase towards larger galactocentric radii, i.e. along the galaxy's (negative) abundance and (positive) extinction gradients. While the increase of P_HII_ with galactocentric radius is likely due to higher photon fluxes from lower-metallicity stellar populations, we find that the increase of P_dir_ is likely driven by the combination of higher photon fluxes and enhanced dust content at larger galactocentric radii. In light of the above, we investigate the effect of increased pre-supernova feedback at larger galactocentric distances (lower metallicities and increased dust mass surface density) on the ISM, finding that supernovae at lower metallicities expand into lower-density environments, thereby enhancing the impact of supernova feedback.2021MNRAS.508.5425Mhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/508/5425CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/other/Ser/184.19 : NGC 300 candidate supernova remnants (Millar+, 2012)J/A+A/552/A12 : Abundances of PNe in NGC 300 (Stasisnka+, 2013)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/508/5425https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/508/5425http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/508/5425https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/508/5425https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/508/5425http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/508/5425GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/MNRAS/508/5425/tableb1 (Our SNR properties)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/MNRAS/508/5425/tableb1?https://vizier.iucaa.in/viz-bin/conesearch/J/MNRAS/508/5425/tableb1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/MNRAS/508/5425/tableb1?GETtext/xml+votable180.050000true13.69415-37.662440.005555555555555556Cone search capability for table J/MNRAS/508/5425/tableb2 (Our PNe properties)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/MNRAS/508/5425/tableb2?https://vizier.iucaa.in/viz-bin/conesearch/J/MNRAS/508/5425/tableb2?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/MNRAS/508/5425/tableb2?GETtext/xml+votable180.050000true13.64214-37.693270.005555555555555556Cone search capability for table J/MNRAS/508/5425/tableb3 (Our H II region properties)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/MNRAS/508/5425/tableb3?https://vizier.iucaa.in/viz-bin/conesearch/J/MNRAS/508/5425/tableb3?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/MNRAS/508/5425/tableb3?GETtext/xml+votable180.050000true13.70028-37.725890.0055555555555555560/https://cdsarc.cds.unistra.fr/viz-bin/moc/J/MNRAS/508/5425?format=asciiOpticaldefaultJ/MNRAS/508/5425/tableb1Our SNR propertiesMillarIDSNR number ID (Millar12id) (1)meta.id;meta.maincharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintID? Dendogram identifier number (Dendrogramid) (2)meta.idintnullableDEJ2000Declination (J2000)degpos.eq.dec;meta.mainlog([NII/Ha])? [N II/H_{alpha}_] line ratio of [N II] at 658.4 nm and H_{alpha}_ at 656.28 nm ([N II/H_{alpha}_])spect.line.intensity;arith.ratiofloatnullablee_log([NII/Ha])? Mean error on [N II/H_{alpha}_]stat.errorfloatnullablelog([SII/Ha])? [S II/H_{alpha}_] line ratio of [S II] at 671.7 nm and H_{alpha}_ at 656.28 nm ([S II/H_{alpha}_])spect.line.intensity;arith.ratiofloatnullablee_log([SII/Ha])? Mean error on [S II/H_{alpha}_]stat.errorfloatnullableFWHMSII? The full width at half-maximum of [S II] at 671.7 nm line (FWHM_[S II]_)0.1nmspect.line.widthfloatnullablee_FWHMSII? Mean error on FWHM of [S II]0.1nmstat.errorfloatnullableNotesNotes on object characteristics (Notes)meta.notecharRAJ2000Right Ascension (J2000)degpos.eq.ra;meta.mainJ/MNRAS/508/5425/tableb2Our PNe propertiesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintStasinskaID? PNe number ID (Stasinska13id) (1)meta.id;meta.mainintnullableID? Dendogram identifier number (Dendrogramid) (2)meta.idintnullableRAJ2000Right Ascension (J2000)degpos.eq.ra;meta.mainDEJ2000Declination (J2000)degpos.eq.dec;meta.mainlog([NII/Ha])? [N II/H_{alpha}_] line ratio of [N II] at 658.4 nm and H_{alpha}_ at 656.28 nm ([N II/H_{alpha}_])spect.line.intensity;arith.ratiofloatnullablee_log([NII/Ha])? Mean error on [N II/H_{alpha}_]stat.errorfloatnullablelog([OIII/Hb])? [O III/H_{beta}_] line ratio of [O III] at 500.7 nm and H_{beta}_ at 486.13 nm ([O III/H_{beta}_])spect.line.intensity;arith.ratiofloatnullablee_log([OIII/Hb])? Mean error on [O III/H_{beta}_]stat.errorfloatnullableNotesNotes on object characteristics (Notes)meta.notecharJ/MNRAS/508/5425/tableb3Our H II region propertiesrRadius of the observed H II region (r) (3)pcphys.size.radius;obs.fieldfloat12+[O/H]Logarithm of oxygen abundance 12+log(O/H) (12+logO/H)phys.abundfloate_12+[O/H]Mean error of 12+log(O/H) (e_12+logO/H)stat.error;phys.abundfloatrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordinte_log([SII/Ha])Mean error on [S II/H_{alpha}_]stat.errorfloatlog(Pdir/kb)Direct radiation pressure P_dir_ divided by the Boltzmann's constant k_b_ (logPdir/k_b_) (4)K.cm**-3phys.pressurefloate_log(Pdir/kb)Mean error on log(P_dir_/k_b_) (e_logPdir/k_b_)K.cm**-3stat.errorfloatlog(PHII/kb)? Pressure of the ionized gas P_HII_ divided by the Boltzmann's constant k_b_ (logPHII/k_b_) (4)K.cm**-3phys.pressurefloatnullablee_log(PHII/kb)? Mean error on log(P_HII_/k_b_)K.cm**-3stat.errorfloatnullableEtaNIIThe radiation softness parameter {eta}_NII_ as 'ratio of ratios' ({eta}_NII_) (5)spect.line.intensity;arith.ratiofloate_EtaNIIMean error on {eta}_NII_stat.errorfloatS32Logarithm of ratio between [S III] at 906.8nm and [S II] at 671.7nm and at 673.1nm (S32)spect.line.intensity;arith.ratiofloate_S32Mean error on S32 (e_S32)stat.errorfloatIDDendogram identifier number (Dendrogramid) (1)meta.id;meta.mainintRAJ2000Right Ascension (J2000)degpos.eq.ra;meta.mainDEJ2000Declination (J2000)degpos.eq.dec;meta.mainRGalactocentric radius in R_25_ unit (R) (2)pos.distance;pos.galactocentricfloatlog([NII/Ha])Logarithm of [N II/H_{alpha}_] line ratio of [N II] at 658.4 nm and H_{alpha}_ at 656.28 nm ([N II/H_{alpha}_])spect.line.intensity;arith.ratiofloate_log([NII/Ha])Mean error on [N II/H_{alpha}_]stat.errorfloatlog([OIII/Hb])Logarithm of [O III/H_{beta}_] line ratio of [O III] at 500.7 nm and H_{beta}_ at 486.13 nm ([O III/H_{beta}_])spect.line.intensity;arith.ratiofloate_log([OIII/Hb])Mean error on [O III/H_{beta}_]stat.errorfloatlog([SII/Ha])Logarithm of [S II/H_{alpha}_] line ratio of [S II] at 671.7 nm and H_{alpha}_ at 656.28 nm ([S II/H_{alpha}_])spect.line.intensity;arith.ratiofloat