Galaxies metallicity gradientsJ/A+A/693/A150ivo://CDS.VizieR/J/A+A/693/A150doi:10.26093/cds/vizier.36930150CDSKhoram A.H.Belfiore F.2025-03-03T20:01:13Z2025-01-13T08:26:52ZCDS support teamCDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, Francecds-question@unistra.frgalaxieschemical-abundancesspectroscopyChemical abundances are key tracers of the cycle of baryons driving the evolution of galaxies. Most measurements of interstellar medium (ISM) abundance and metallicity gradients in galaxies are based, however, on model-dependent strong-line methods. Direct chemical abundances can be obtained via the detection of weak auroral lines, but such lines are too faint to be detected across large spectroscopic surveys of the local Universe. In this work we overcome this limitation and obtain metallicity gradients from direct method abundances by stacking spectra from the MaNGA integral field spectroscopy survey. In particular we stack 4150 star-forming galaxies across the star formation rate-stellar mass (SFR-M_star_) plane and across six radial bins. We calculate electron temperatures for [OII], [SII], [NII], [SIII] and [OIII] across the majority of stacks. We find that the T[OII]~T[SII]~T[OII], as expected since these ions all trace the low-ionization zone of nebulae. The [OIII] temperatures become substantially larger than those of other ions at high metallicity, indicating potentially unaccounted for spectral contamination or additional physics. In light of this uncertainty we base our abundance calculation on the temperatures of [SIII] and the low-ionization ions. We recover a mass-metallicity relation (MZR) similar to that obtained with different empirical calibrations. We do not find evidence, however, for a secondary dependence on SFR using direct metallicities. Finally, we derive metallicity gradients that becomes steeper with stellar mass for log(M_star_/M_{sun}_)<10.5. At higher masses, the gradients flatten again, confirming with auroral line determinations the trends previously defined with strong-line calibrators.2025A&A...693A.150Khttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/693/A150CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/693/A150https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/693/A150http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/693/A150https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/693/A150https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/693/A150http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/693/A150GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefault
J/A+A/693/A150/tableb3Radially binned emission line fluxes and their uncertaintiesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordinte_FHeI4987HeI4987 emission-line flux uncertainty (G2)1e-20W.m**-2stat.errorfloate_FOIII5006OIII5006 emission-line flux uncertainty (G2)1e-20W.m**-2stat.errorfloatBinIDNumber of the bin in SFR-M* space, starting from the lowest stellar-mass and SFRmeta.idintlogMassMedian stellar masses estimate of all galaxies within each SFR-M* bin using glog(solMass)phys.massfloatlogSFRRepresentative SFR for individual SFR-M* bins, obtained from extinction corrected Ha flux using MaNGA DAP cataloglog(solMass.yr**-1)phys.SFRfloatFOII3726OII3726 emission-line flux (G1)1e-20W.m**-2phot.fluxdoubleFOII3728OII3728 emission-line flux (G1)1e-20W.m**-2phot.fluxdoubleFH93751H93751 emission-line flux (G1)1e-20W.m**-2phot.fluxdoubleFH103771H103771 emission-line flux (G1)1e-20W.m**-2phot.fluxdoubleFHth3798Hth3798 emission-line flux (G1)1e-20W.m**-2phot.fluxdoubleFHt3836Ht3836 emission-line flux (G1)1e-20W.m**-2phot.fluxdoubleFNeIII3868NeIII3868 emission-line flux (G1)1e-20W.m**-2phot.fluxdoubleFSII4068SII4068 emission-line flux (G1)1e-20W.m**-2phot.fluxdoubleFSII4076SII4076 emission-line flux (G1)1e-20W.m**-2phot.fluxdoubleFHd4101Hd4101 emission-line flux (G1)1e-20W.m**-2phot.fluxdoubleFHg4340Hg4340 emission-line flux (G1)1e-20W.m**-2phot.fluxdoubleFFeII4288FeII4288 emission-line flux (G1)1e-20W.m**-2phot.fluxdoubleFOIII4363OIII4363 emission-line flux (G1)1e-20W.m**-2phot.fluxdoubleFFeII4359FeII4359 emission-line flux (G1)1e-20W.m**-2phot.fluxdoubleFHb4861Hb4861 emission-line flux (G1)1e-20W.m**-2phot.fluxdoubleFHeII4685HeII4685 emission-line flux (G1)1e-20W.m**-2phot.fluxdoubleFFeIII4659FeIII4659 emission-line flux (G1)1e-20W.m**-2phot.fluxdoubleFArIV4713ArIV4713 emission-line flux (G1)1e-20W.m**-2phot.fluxdoubleFOIII4958OIII4958 emission-line flux (G1)1e-20W.m**-2phot.fluxdoubleFHeI4987HeI4987 emission-line flux (G1)1e-20W.m**-2phot.fluxdoubleFOIII5006OIII5006 emission-line flux (G1)1e-20W.m**-2phot.fluxdoubleFHeI5016HeI5016 emission-line flux (G1)1e-20W.m**-2phot.fluxdoubleFNII5754NII5754 emission-line flux (G1)1e-20W.m**-2phot.fluxdoubleFHeI5875HeI5875 emission-line flux (G1)1e-20W.m**-2phot.fluxdoubleFOI6300OI6300 emission-line flux (G1)1e-20W.m**-2phot.fluxdoubleFSIII6312SIII6312 emission-line flux (G1)1e-20W.m**-2phot.fluxdoubleFOI6363OI6363 emission-line flux (G1)1e-20W.m**-2phot.fluxdoubleFNII6548NII6548 emission-line flux (G1)1e-20W.m**-2phot.fluxdoubleFHa6562Ha6562 emission-line flux (G1)1e-20W.m**-2phot.fluxdoubleFNII6583NII6583 emission-line flux (G1)1e-20W.m**-2phot.fluxdoubleFHeI6678HeI6678 emission-line flux (G1)1e-20W.m**-2phot.fluxdoubleFHeI6680HeI6680 emission-line flux (G1)1e-20W.m**-2phot.fluxdoubleFSII6716SII6716 emission-line flux (G1)1e-20W.m**-2phot.fluxdoubleFSII6730SII6730 emission-line flux (G1)1e-20W.m**-2phot.fluxdoubleFArIII7135ArIII7135 emission-line flux (G1)1e-20W.m**-2phot.fluxdoubleFOII7329OII7329 emission-line flux (G1)1e-20W.m**-2phot.fluxfloatFOII7330OII7330 emission-line flux (G1)1e-20W.m**-2phot.fluxfloatFOII7318OII7318 emission-line flux (G1)1e-20W.m**-2phot.fluxfloatFOII7319OII7319 emission-line flux (G1)1e-20W.m**-2phot.fluxfloatFNNII7303NNII7303 emission-line flux (G1)1e-20W.m**-2phot.fluxfloatFSIII9068SIII9068 emission-line flux (G1)1e-20W.m**-2phot.fluxdoublee_FOII3726OII3726 emission-line flux uncertainty (G2)1e-20W.m**-2stat.errorfloate_FOII3728OII3728 emission-line flux uncertainty (G2)1e-20W.m**-2stat.errorfloate_FH93751H93751 emission-line flux uncertainty (G2)1e-20W.m**-2stat.errorfloate_FH103771H103771 emission-line flux uncertainty (G2)1e-20W.m**-2stat.errorfloate_FHth3798Hth3798 emission-line flux uncertainty (G2)1e-20W.m**-2stat.errorfloate_FHt3836Ht3836 emission-line flux uncertainty (G2)1e-20W.m**-2stat.errorfloate_FNeIII3868NeIII3868 emission-line flux uncertainty (G2)1e-20W.m**-2stat.errorfloate_FSII4068SII4068 emission-line flux uncertainty (G2)1e-20W.m**-2stat.errorfloate_FSII4076SII4076 emission-line flux uncertainty (G2)1e-20W.m**-2stat.errorfloate_FHd4101Hd4101 emission-line flux uncertainty (G2)1e-20W.m**-2stat.errorfloate_FHg4340Hg4340 emission-line flux uncertainty (G2)1e-20W.m**-2stat.errorfloate_FFeII4288FeII4288 emission-line flux uncertainty (G2)1e-20W.m**-2stat.errorfloate_FOIII4363OIII4363 emission-line flux uncertainty (G2)1e-20W.m**-2stat.errorfloate_FFeII4359FeII4359 emission-line flux uncertainty (G2)1e-20W.m**-2stat.errorfloate_FHb4861Hb4861 emission-line flux uncertainty (G2)1e-20W.m**-2stat.errorfloate_FHeII4685HeII4685 emission-line flux uncertainty (G2)1e-20W.m**-2stat.errorfloate_FFeIII4659FeIII4659 emission-line flux uncertainty (G2)1e-20W.m**-2stat.errorfloate_FArIV4713ArIV4713 emission-line flux uncertainty (G2)1e-20W.m**-2stat.errorfloate_FOIII4958OIII4958 emission-line flux uncertainty (G2)1e-20W.m**-2stat.errorfloate_FHeI5016HeI5016 emission-line flux uncertainty (G2)1e-20W.m**-2stat.errorfloate_FNII5754NII5754 emission-line flux uncertainty (G2)1e-20W.m**-2stat.errorfloate_FHeI5875HeI5875 emission-line flux uncertainty (G2)1e-20W.m**-2stat.errorfloate_FOI6300OI6300 emission-line flux uncertainty (G2)1e-20W.m**-2stat.errordoublee_FSIII6312SIII6312 emission-line flux uncertainty (G2)1e-20W.m**-2stat.errorfloate_FOI6363OI6363 emission-line flux uncertainty (G2)1e-20W.m**-2stat.errorfloate_FNII6548NII6548 emission-line flux uncertainty (G2)1e-20W.m**-2stat.errorfloate_FHa6562Ha6562 emission-line flux error uncertainty (G2)1e-20W.m**-2stat.errorfloate_FNII6583NII6583 emission-line flux uncertainty (G2)1e-20W.m**-2stat.errorfloate_FHeI6678HeI6678 emission-line flux uncertainty (G2)1e-20W.m**-2stat.errorfloate_FHeI6680HeI6680 emission-line flux uncertainty (G2)1e-20W.m**-2stat.errorfloate_FSII6716SII6716 emission-line flux uncertainty (G2)1e-20W.m**-2stat.errorfloate_FSII6730SII6730 emission-line flux uncertainty (G2)1e-20W.m**-2stat.errorfloate_FArIII7135ArIII7135 emission-line flux uncertainty (G2)1e-20W.m**-2stat.errorfloate_FOII7329OII7329 emission-line flux uncertainty (G2)1e-20W.m**-2stat.errordoublee_FOII7330OII7330 emission-line flux uncertainty (G2)1e-20W.m**-2stat.errordoublee_FOII7318OII7318 emission-line flux uncertainty (G2)1e-20W.m**-2stat.errordoublee_FOII7319OII7319 emission-line flux uncertainty (G2)1e-20W.m**-2stat.errordoublee_FNNII7303NNII7303 emission-line flux uncertainty (G2)1e-20W.m**-2stat.errorfloate_FSIII9068SIII9068 emission-line flux uncertainty (G2)1e-20W.m**-2stat.errorfloatRadBinThe radial bin considered for individual galaxies within each SFR-M* bin, in Re unitstat.paramchar
J/A+A/693/A150/tableb5Radially binned inferred physical parameters, electron temperature, ionic abundance, Te and strong-line metallicity for all the binslogMassMedian stellar masses estimate of all galaxies within each SFR-M* bin using MaNGA DRP catalog (NSA_ELPETRO_MASS)log(solMass)phys.massfloatTNII? Electron temperature of [NII]Kphys.temperature.electron;phys.electrondoublenullablerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintBinIDNumber of the bin in SFR-M* space, starting from the lowest stellar-mass and SFRmeta.idintlogSFRRepresentative SFR for individual SFR-M* bins, obtained from extinction corrected Ha flux using MaNGA DAP cataloglog(solMass.yr**-1)phys.SFRfloate_TNII? Electron temperature uncertainty of [NII] obtained via MC methodKstat.errorfloatnullableTOII? Electron temperature of [OII]Kphys.temperature.electron;phys.electrondoublenullablee_TOII? Electron temperature uncertainty of [OII] obtained via MC methodKstat.errorfloatnullableTSII? Electron temperature of [SII]Kphys.temperature.electron;phys.electrondoublenullablee_TSII? Electron temperature uncertainty of [SII] obtained via MC methodKstat.errorfloatnullableTOIII? Electron temperature of [OIII]Kphys.temperature.electron;phys.electrondoublenullablee_TOIII? Electron temperature uncertainty of [OIII] obtained via MC methodKstat.errorfloatnullableTSIII? Electron temperature of [SIII]Kphys.temperature.electron;phys.electrondoublenullablee_TSIII? Electron temperature uncertainty of [SIII] obtained via MC methodKstat.errorfloatnullableO+? Abundance of O+/H+phot.fluxdoublenullablee_O+? Abundance uncertainty of O+/H+ obtained via MC methodstat.errordoublenullableO++? Abundance of O++/H+phot.fluxdoublenullablee_O++? Abundance uncertainty of O++/H+ obtained via MC methodstat.errordoublenullableP04Met? Strong-line metallicity estimate based on Pettini & Pagel (2004MNRAS.348L..59P) O3N2 calibrationphys.abund.Zdoublenullablee_P04Met? Strong-line metallicity uncertainty estimatestat.errordoublenullableTeMet? Direct-method metallicity estimate via electron temperaturesphys.abund.Zdoublenullablee_TeMet? Direct-method metallicity uncertainty obtained via MC methodcb1stat.errordoublenullableRadBinThe radial bin considered for individual galaxies within each SFR-M* bin in Re unitstat.paramchar
J/A+A/693/A150/tableb6Global inferred physical parameters, including electron temperature, ionic abundances, Te-based metallicity, and strong-line metallicity for all binsO++? Abundance of O++/H+phot.fluxdoublenullablee_O+? Abundance uncertainty of O+/H+ obtained via MC methodstat.errordoublenullablee_O++? Abundance uncertainty of O++/H+ obtained via MC methodstat.errordoublenullablerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintBinIDNumber of the bin in SFR-M* space, starting from the lowest stellar-mass and SFRphys.veloc;em.binintlogMassMedian stellar masses estimate of all galaxies within each SFR-M* bin using MaNGA DRP catalog (NSA_ELPETRO_MASS)log(solMass)phys.massfloatlogSFRRepresentative SFR for individual SFR-M* bins, obtained from extinction corrected Ha flux using MaNGA DAP cataloglog(solMass.yr**-1)phys.SFRfloatTNII? Electron temperature of [NII]Kphys.temperature.electron;phys.electrondoublenullablee_TNII? Electron temperature uncertainty of [NII] obtained via MC methodKstat.errorfloatnullableTOII? Electron temperature of [OII]Kphys.temperature.electron;phys.electrondoublenullablee_TOII? Electron temperature uncertainty of [OII] obtained via MC methodKstat.errorfloatnullableTSII? Electron temperature of [SII]Kphys.temperature.electron;phys.electrondoublenullablee_TSII? Electron temperature uncertainty of [SII] obtained via MC methodKstat.errorfloatnullableTOIII? Electron temperature of [OIII]Kphys.temperature.electron;phys.electrondoublenullablee_TOIII? Electron temperature uncertainty of [OIII] obtained via MC methodKstat.errorfloatnullableTSIII? Electron temperature of [SIII]Kphys.temperature.electron;phys.electrondoublenullablee_TSIII? Electron temperature uncertainty of [SIII] obtained via MC methodKstat.errorfloatnullableO+? Abundance of O+/H+phot.fluxdoublenullableP04MetStrong-line metallicity estimate based on Pettini & Pagel (2004MNRAS.348L..59P) O3N2 calibrationphys.abund.Zdoublee_P04MetStrong-line metallicity uncertainty estimatestat.errordoubleTeMet? Direct-method metallicity estimate via electron temperaturesphys.abund.Zdoublenullablee_TeMet? Direct-method metallicity uncertainty obtained via MC methodcb1stat.errordoublenullable