J/A+A/652/A23ivo://CDS.VizieR/J/A+A/652/A23doi:10.26093/cds/vizier.36520023CDSFernandez-Ontiveros J.A.Perez-Montero E.Vilchez J.M.Amorin R.,Spinoglio L.2022-01-17T11:48:24Z2021-08-05T08:33:15ZCDS support team

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

cds-question@unistra.frgalaxiesinfrared-sourcesspectroscopyinfrared-astronomychemical-abundancesWe provide a new method to derive heavy element abundances based on the unique suite of nebular lines in the mid- to far-infrared (IR) range. Using grids of photo-ionisation models that cover a wide range in O/H and N/O abundances, and ionisation parameter, our code HII-CHI-MISTRY-IR (HCm-IR) provides model-based abundances based on extinction free and temperature insensitive tracers, two significant advantages over optical diagnostics. The code is probed using a sample of 56 galaxies observed with Spitzer and Herschel covering a wide range in metallicity, 7.2~<12+log(O/H)~<8.9. The IR model-based metallicities obtained are robust within a scatter of 0.03dex when the hydrogen recombination lines, which are typically faint transitions in the IR range, are not available. When compared to the optical abundances obtained with the direct method,model- based methods, and strong-line calibrations, HCm-IR estimates show a typical dispersion of ~0.2dex, in line with previous studies comparing IR and optical abundances, a do not introduce a noticeable systematic above 12+log(O/H)>7.6. This accuracy can be achieved using the lines [SIV]10.5um, [SIII]18.7,33.5um, [NeIII]15.6um and [NeII]12.8um. Additionally, HCm-IR provides an independent N/O measurement when the [OIII]52,88um and [NIII]57um transitions are measured, and therefore the derived abundances in this case do not rely on particular assumptions in the N/O ratio. Large uncertainties (~0.4dex) may affect the abundance determinations of galaxies at sub- or over-solar metallicities when a solar-like N/O ratio is adopted. Finally, the code has been applied to 8 galaxies located at 1.8<z<7.5 with ground-based detections of far-IR lines redshifted in the submm range, revealing solar-like N/O and O/H abundances in agreement with recent studies.2021A&A...652A..23Fhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/652/A23CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/652/A23https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/652/A23http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/652/A23https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/652/A23https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/652/A23http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/652/A23GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/652/A23/table1 (IR line fluxes for star-forming galaxies)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/652/A23/table1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/652/A23/table1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/652/A23/table1?GETtext/xml+votable180.050000true9.21856-33.5546570.0055555555555555566/2409 3389 3506 4511 5116 5492 5715 5751 5950 6011 6042 6046 6090 6419 7281 7606 8028 8106 8707 9388 10431 10587 10689 10761 10970 11177 11382 15592 16655 16882 17741 18002 19934 20388 22721 22828 23078 23566 25594 25659 26271 26298 26470 26937 26971 27258 27305 27514 28393 28496 28631 31081 33986 34026 34273 35243 35576 36756 36831 38139 40124 43107 43874 43881 46079 46130https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/652/A23?format=asciiInfrareddefaultJ/A+A/652/A23/table1IR line fluxes for star-forming galaxieszRedshiftsrc.redshiftdoubleNameGalaxy namemeta.id;meta.maincharRefsReferences (1)meta.ref;pos.framecharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintRAJ2000Right ascension (J2000.0)pos.eq.ra;meta.mainDEJ2000Declination (J2000.0)pos.eq.dec;meta.mainTypeSpectral typesrc.spTypecharbra-4p05? Brackett alpha line flux1e-17W.m**-2phot.flux;em.line.Halphafloatnullablee_bra-4p05? Brackett alpha flux uncertainty1e-17W.m**-2stat.errorfloatnullablepfa-7p5? Pfund alpha line flux1e-17W.m**-2phot.flux;em.line.Halphadoublenullablee_pfa-7p5? Pfund alpha flux uncertainty1e-17W.m**-2stat.errordoublenullables4-10p5? [SIV]10.5 line flux1e-17W.m**-2phot.flux;spect.linefloatnullablee_s4-10p5? [SIV]10.5 flux uncertainty1e-17W.m**-2stat.errorfloatnullablehua-12p4? Humphreys alpha line flux1e-17W.m**-2phot.flux;em.line.Halphafloatnullablee_hua-12p4? Humphreys alpha flux uncertainty1e-17W.m**-2stat.errorfloatnullablen2-12p8? [NeII]12.8 line flux1e-17W.m**-2phot.flux;spect.linedoublenullablee_n2-12p8? [NeII]12.8 flux uncertainty1e-17W.m**-2stat.errorfloatnullablen3-15p6? [NeIII]15.6 line flux1e-17W.m**-2phot.flux;spect.linefloatnullablee_n3-15p6? [NeIII]15.6 flux uncertainty1e-17W.m**-2stat.errorfloatnullables3-18p7? [SIII]18.7 line flux1e-17W.m**-2phot.flux;spect.linefloatnullablee_s3-18p7? [SIII]18.7 flux uncertainty1e-17W.m**-2stat.errorfloatnullables3-33p5? [SIII]33.5 line flux1e-17W.m**-2phot.flux;spect.linedoublenullablee_s3-33p5? [SIII]33.5 flux uncertainty1e-17W.m**-2stat.errorfloatnullableo3-52? [OIII]52 line flux1e-17W.m**-2phot.flux;spect.linedoublenullablee_o3-52? [OIII]52 flux uncertainty1e-17W.m**-2stat.errorfloatnullablen3-57? [NIII]57 line flux1e-17W.m**-2phot.flux;spect.linedoublenullablee_n3-57? [NIII]57 flux uncertainty1e-17W.m**-2stat.errorfloatnullableo3-88? [OIII]88 line flux1e-17W.m**-2phot.flux;spect.linedoublenullablee_o3-88? [OIII]88 flux uncertainty1e-17W.m**-2stat.errorfloatnullablen2-122? [NII]122 line flux1e-17W.m**-2phot.flux;spect.linedoublenullablee_n2-122? [NII]122 flux uncertainty1e-17W.m**-2stat.errorfloatnullableSimbadNameSimbad column added by the CDSmeta.idcharJ/A+A/652/A23/table3*HCm-IR abundances compared with optical line-based methodsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameGalaxy namemeta.id;meta.maincharO/H-ir? IR-based O/H abundance, 12+log(O/H)_IR_phys.abundfloatnullablee_O/H-ir? IR-based O/H abundance errorstat.error;phys.abundfloatnullableN/O-ir? IR-based N/O abundance, log(N/O)_IR_phys.abundfloatnullablee_N/O-ir? IR-based N/O abundance errorstat.error;phys.abundfloatnullableO/H-hcm? Optical-based O/H abundance, 12+log(O/H)_HCm_phys.abundfloatnullablee_O/H-hcm? Optical-based O/H abundance errorstat.error;phys.abundfloatnullableN/O-hcm? Optical-based N/O abundance, log(N/O)_HCm_phys.abundfloatnullablee_N/O-hcm? Optical-based N/O abundance errorstat.error;phys.abundfloatnullableO/H-lit? Optical-based O/H abundance from literature, 12+log(O/H)_lit_phys.abundfloatnullablee_O/H-lit? Optical-based O/H abundance error from literaturestat.error;phys.abundfloatnullabler_O/H-litReference for O/H-lit (1)meta.ref;pos.framecharO/H-R? Optical O/H abundance estimated obtained using Pilyugin & Grebel (2016MNRAS.457.3678P) R-calibration, 12+log(O/H)_R_phys.abundfloatnullableO/H-S? Optical O/H abundance estimated obtained using Pilyugin & Grebel (2016MNRAS.457.3678P) S-calibration, 12+log(O/H)_S_phys.abundfloatnullable