J/A+A/666/A115ivo://CDS.VizieR/J/A+A/666/A115doi:10.26093/cds/vizier.36660115CDSPerez-Diaz B.Perez-Montero E.Fernandez-Ontiveros J.A.Vilchez J.M.2022-11-09T06:03:18Z2022-10-14T10:41:44ZCDS support team

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

cds-question@unistra.fractive-galactic-nucleichemical-abundancesinfrared-sourcesvisible-astronomyFuture and on-going infrared and radio observatories such as JWST, METIS or ALMA will increase the amount of rest-frame IR spectroscopic data for galaxies by several orders of magnitude. While studies of the chemical composition of the ISM based on optical observations have been widely spread over decades for SFG and, more recently, for AGN, similar studies need to be performed using IR data. This regime can be especially useful in the case of AGN given that it is less affected by temperature and dust extinction, traces higher ionic species and can also provide robust estimations of the chemical abundance ratio N/O. We present a new tool based on a bayesian-like methodology (HII-CHI-Mistry-IR) to estimate chemical abundances from IR emission lines in AGN. We use a sample of 58 AGN with IR spectroscopic data retrieved from the literature, composed by 43 Seyferts, 8 ULIRGs, 4 LIRGs and 3 LINERs, to probe the validity of our method. The estimations of the chemical abundances based on IR lines in our sample are later compared with the corresponding abundances derived from the optical emission lines in the same objects. HII-CHI-Mistry-IR takes advantage of photoionization models, characterized by the chemical abundance ratios O/H and N/O and the ionization parameter U, to compare their predicted emission- line fluxes with a set of observed values. Instead of matching single emission lines, the code uses some specific emission-line ratios sensitive to the above free parameters. We report mainly solar and also subsolar abundances for O/H in the nuclear region for our sample of AGN, whereas N/O clusters around solar values. We find a discrepancy between the chemical abundances derived from IR and optical emission lines, being the latter higher than the former. This discrepancy, also reported by previous studies of the composition of the ISM in AGN from IR observations, is independent from the gas density or the incident radiation field to the gas, and it is likely associated with dust obscuration and/or temperature stratification within the gas nebula.2022A&A...666A.115Phttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/666/A115CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/666/A115https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/666/A115http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/666/A115https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/666/A115https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/666/A115http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/666/A115GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/666/A115/tablea1 (IR emission line fluxes for the of AGN and their references)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/666/A115/tablea1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/666/A115/tablea1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/666/A115/tablea1?GETtext/xml+votable180.050000true5.473392222-79.1688770.005555555555555556Cone search capability for table J/A+A/666/A115/tablea3 (Optical emission line fluxes for the of AGN and their references)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/666/A115/tablea3?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/666/A115/tablea3?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/666/A115/tablea3?GETtext/xml+votable180.050000true5.473392222-79.1688770.0055555555555555566/1008 1701 2564 2774 4439 5116 6098 7552 7869 8106 8845 8922 9194 10355 10475 10912 10927 11101 11180 11206 14744 15351 17141 17754 18919 19283 19619 20230 21016 25907 25965 26148 26298 26937 28393 31081 31158 32930 33409 34531 34534 40818 41059 41586 43233 43262 43877 44660 45587 46079 46130 46399 46811 46987 47047 47154 49042https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/666/A115?format=asciiOpticalInfrareddefaultJ/A+A/666/A115/refsReferencesRefReference codemeta.notecharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintBibCodeBibCodemeta.bib.bibcodecharAutAuthor's namemeta.bib.authorcharComCommentsmeta.notecharJ/A+A/666/A115/tablea1IR emission line fluxes for the of AGN and their referencesIDName or identificator of the objectmeta.id;meta.maincharOIII88m[-2.04/1577.0]? [OIII] at 88 microns line flux (in 10^-14^erg/s/cm^2^)1e-17W.m**-2phot.flux;em.IR.60-100um;spect.linedoublenullablee_OIII88m[0.26/65.0]? [OIII] at 88 microns flux uncertainty (in 10^-14^erg/s/cm^2^)1e-17W.m**-2stat.errorfloatnullableNII122m[-19.0/459.34]? [NII] at 122 microns line flux (in 10^-14^erg/s/cm^2^)1e-17W.m**-2phot.flux;em.mm.1500-3000GHz;spect.linefloatnullableSimbadNameSimbad column added by the CDSmeta.idcharnullablerecnoRecord 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.mainzRedshiftsrc.redshiftdoubleTypeSpectral type (G1)src.spTypecharHI4m[-1.68/21.8]? Brackett alpha line flux (in 10^-14^erg/s/cm^2^)1e-17W.m**-2phot.flux;em.line.Halphafloatnullablee_HI4m[0.11/5.0]? Brackett alpha flux uncertainty (in 10^-14^erg/s/cm^2^)1e-17W.m**-2stat.errorfloatnullableHI7m? Pfund alpha line flux (in 10^-14^erg/s/cm^2^)1e-17W.m**-2phot.flux;em.line.Halphaintnullablee_HI7m? Pfund alpha flux uncertainty (in 10^-14^erg/s/cm^2^)1e-17W.m**-2stat.errorintnullableSIV10m[-2.83/536.1]? [SIV] at 10.5 microns line flux (in 10^-14^erg/s/cm^2^)1e-17W.m**-2phot.flux;em.IR.8-15um;spect.linefloatnullablee_SIV10m[0.11/53.2]? [SIV] at 10.5 microns flux uncertainty (in 10^-14^erg/s/cm^2^)1e-17W.m**-2stat.errorfloatnullableHI12m[-0.66/6.81]? Humphreys alpha line flux (in 10^-14^erg/s/cm^2^)1e-17W.m**-2phot.flux;em.line.Halphafloatnullablee_HI12m[0.06/1.53]? Humphreys alpha flux uncertainty (in 10^-14^erg/s/cm^2^)1e-17W.m**-2stat.errorfloatnullableNeII12m[1.35/698.4]? [NeII] at 12.8 microns line flux (in 10^-14^erg/s/cm^2^)1e-17W.m**-2phot.flux;em.IR.8-15um;spect.linefloatnullablee_NeII12m[0.09/67.5]? [NeII] at 12.8 microns flux uncertainty (in 10^-14^erg/s/cm^2^)1e-17W.m**-2stat.errorfloatnullableNeV14m[-3.0/899.0]? [NeV] at 14.3 microns line flux (in 10^-14^erg/s/cm^2^)1e-17W.m**-2phot.flux;em.IR.8-15um;spect.linefloatnullablee_NeV14m[0.05/22.9]? [NeV] at 14.3 microns flux uncertainty (in 10^-14^erg/s/cm^2^)1e-17W.m**-2stat.errorfloatnullableNeIII15m[1.27/1371.0]? [NeIII] at 15.6 microns line flux (in 10^-14^erg/s/cm^2^)1e-17W.m**-2phot.flux;em.IR.15-30um;spect.linedoublenullablee_NeIII15m[0.04/29.9]? [NeIII] at 15.6 microns flux uncertainty (in 10^-14^erg/s/cm^2^)1e-17W.m**-2stat.errorfloatnullableSIII18m[-15.0/240.6]? [SIII] at 18 microns line flux (in 10^-14^erg/s/cm^2^)1e-17W.m**-2phot.flux;em.IR.15-30um;spect.linefloatnullablee_SIII18m[0.03/26.2]? [SIII] at 18 microns flux uncertainty (in 10^-14^erg/s/cm^2^)1e-17W.m**-2stat.errorfloatnullableNeV24m[-50.9/816.0]? [NeV] at 24 microns line flux (in 10^-14^erg/s/cm^2^)1e-17W.m**-2phot.flux;em.IR.15-30um;spect.linefloatnullablee_NeV24m[0.08/58.8]? [NeV] at 24 microns flux uncertainty (in 10^-14^erg/s/cm^2^)1e-17W.m**-2stat.errorfloatnullableOIV26m[-9.5/2030.0]? [OIV] at 26 microns line flux (in 10^-14^erg/s/cm^2^)1e-17W.m**-2phot.flux;em.IR.15-30um;spect.linedoublenullablee_OIV26m[-9.5/2030.0]? [OIV] at 26 microns flux uncertainty (in 10^-14^erg/s/cm^2^)1e-17W.m**-2stat.errordoublenullableSIII33m[-13.0/848.02]? [SIII] at 33 microns line flux (in 10^-14^erg/s/cm^2^)1e-17W.m**-2phot.flux;em.IR.30-60um;spect.linefloatnullablee_SIII33m[0.08/102.0]? [SIII] at 33 microns flux uncertainty (in 10^-14^erg/s/cm^2^)1e-17W.m**-2stat.errorfloatnullableOIII52m[-461.77/1514.0]? [OIII] at 52 microns line flux (in 10^-14^erg/s/cm^2^)1e-17W.m**-2phot.flux;em.IR.30-60um;spect.linedoublenullablee_OIII52m[1.21/201.0]? [OIII] at 52 microns flux uncertainty (in 10^-14^erg/s/cm^2^)1e-17W.m**-2stat.errorfloatnullableNIII57m[-25.99/637.37]? [NIII] at 57 microns line flux (in 10^-14^erg/s/cm^2^)1e-17W.m**-2phot.flux;em.IR.30-60um;spect.linefloatnullablee_NIII57m[0.37/59.0]? [NIII] at 57 microns flux uncertainty (in 10^-14^erg/s/cm^2^)1e-17W.m**-2stat.errorfloatnullablee_NII122m[0.1/17.37]? [NII] at 122 microns flux uncertainty (in 10^-14^erg/s/cm^2^)1e-17W.m**-2stat.errorfloatnullableNII205m[0.49/186.65]? [NII] at 205 microns line flux (in 10^-14^erg/s/cm^2^)1e-17W.m**-2phot.flux;em.mm.750-1500GHz;spect.linefloatnullablee_NII205m[0.1/6.83]? [NII] at 205 microns flux uncertainty (in 10^-14^erg/s/cm^2^)1e-17W.m**-2stat.errorfloatnullableRefsReferences for IR emission lines, in refs.dat filemeta.ref;pos.framecharJ/A+A/666/A115/tablea2Chemical abundances estimated from IR emission linesIDName or identificator of the objectmeta.id;meta.maincharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordint12+log(O/H)ir[7.66/8.52]? IR-based oxygen abundance 12+log(O/H)phys.abundfloatnullablee_12+log(O/H)ir[0.22/0.43]? IR-based oxygen abundance 12+log(O/H) errorstat.errorfloatnullable12+log(N/O)ir[-1.11/-0.22]? IR-based nitrogen-to-oxygen abundance ratio log(N/O)phys.abundfloatnullablee_12+log(N/O)ir[0.11/0.35]? IR-based nitrogen-to-oxygen abundance ratio log(N/O) errorstat.errorfloatnullablelogUir[-3.6/-1.0]? IR-based ionization parameter log(U)phys.ionizParam.radfloatnullablee_logUir[0.07/0.49]? IR-based ionization parameter log(U) errorstat.errorfloatnullableJ/A+A/666/A115/tablea3Optical emission line fluxes for the of AGN and their referencesOIII5007[0.08/29.62]? Relative flux of emission lines [OIII] at 5007{AA} referred to Hbeta fluxphot.flux;spect.linefloatnullablee_OIII5007[0.0/8.27]? Relative flux error of emission lines [OIII] at 5007{AA} referred to Hbeta fluxstat.errorfloatnullableNII6584[0.11/9.8]? Relative flux of emission lines [NII] at 6584{AA} referred to Hbeta fluxphot.flux;spect.linefloatnullablee_NII6584[0.01/3.86]? Relative flux error of emission lines [NII] at 6584{AA} referred to Hbeta fluxstat.errorfloatnullableSII6725[0.02/4.5]? Sum of the relative fluxes of emission lines [SII] at 6717{AA} and [SII] at 6731{AA} referred to Hbeta fluxphot.fluxfloatnullablerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIDName or identificator of the objectmeta.id;meta.maincharRAJ2000Right ascension (J2000.0)pos.eq.ra;meta.mainDEJ2000Declination (J2000.0)pos.eq.dec;meta.mainzRedshiftsrc.redshiftdoubleTypeSpectral type (G1)src.spTypecharOII3727[0.09/45.9]? Sum of the relative fluxes of emission lines [OII] at 3726{AA} and [OII] at 3729{AA} referred to Hbeta fluxphot.fluxfloatnullablee_OII3727[0.02/12.48]? Sum of the relative flux errors of emission lines [OII] at 3726{AA} and [OII] at 3729{AA} referred to Hbeta fluxstat.errorfloatnullableNeIII3868[0.05/5.77]? Relative flux of emission lines [NeIII] at 3868{AA} referred to Hbeta fluxphot.flux;spect.linefloatnullablee_NeIII3868[0.01/6.13]? Relative flux error of emission lines [NeIII] at 3868{AA} referred to Hbeta fluxstat.errorfloatnullableOIII4363[0.05/0.69]? Relative flux of emission lines [OIII] at 4363{AA} referred to Hbeta fluxphot.flux;spect.linefloatnullablee_OIII4363[0.01/0.16]? Relative flux error of emission lines [OIII] at 4363{AA} referred to Hbeta fluxstat.errorfloatnullableOIII4959[0.08/9.9]? Relative flux of emission lines [OIII] at 4959{AA} referred to Hbeta fluxphot.flux;spect.linefloatnullablee_OIII4959[0.0/3.17]? Relative flux error of emission lines [OIII] at 4959{AA} referred to Hbeta fluxstat.errorfloatnullablee_SII6725[0.0/1.1]? Sum of the relative flux errors of emission lines [SII] at 6717{AA} and [SII] at 6731{AA} referred to Hbeta fluxstat.errorfloatnullableFHbeta[0.08/16767.73] Balmer line Hbeta flux (in 10^-14^erg/s/cm^2^)1e-17W.m**-2phot.flux;spect.linedoublee_FHbeta[0.06/1678.98]? Balmer line Hbeta flux error (in 10^-14^erg/s/cm^2^)1e-147W.m**-2stat.errordoublenullableRefsReferences for optical emission lines, in refs.dat filesmeta.ref;pos.framecharJ/A+A/666/A115/tablea4Chemical abundances estimated from optical emission linesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIDName or identificator of the objectmeta.id;meta.mainchar12+log(O/H)opt[7.58/8.84] Opt-based oxygen abundance 12+log(O/H)phys.abundfloate_12+log(O/H)opt[0.07/0.53] Opt-based oxygen abundance 12+log(O/H) errorstat.errorfloat12+log(N/O)opt[-1.28/-0.17]? Opt-based nitrogen-to-oxygen abundance ratio log(N/O)phys.abundfloatnullablee_12+log(N/O)opt[0.09/0.42]? Opt-based nitrogen-to-oxygen abundance ratio log(N/O) errorstat.errorfloatnullablelogUopt[-3.89/-0.81] Opt-based ionization parameter log(U)phys.ionizParam.radfloate_logUopt[0.01/0.73] Opt-based ionization parameter log(U) errorstat.errorfloat12+log(O/H)FM20[7.57/8.73]? Oxygen abundance 12+log(O/H) obtained after applying the calibration from Flury & Morgan (2020MNRAS.496.2191F)phys.abundfloatnullablee_12+log(O/H)FM20? Oxygen abundance 12+log(O/H) error obtained after applying the calibration from Flury & Morgan (2020MNRAS.496.2191F)stat.errorfloatnullable12+log(O/H)Ca20[8.27/8.98]? Oxygen abundance 12+log(O/H) obtained after applying the calibration from Carvalho et al. (2020MNRAS.492.5675C)phys.abundfloatnullablee_12+log(O/H)Ca20[0.01/0.5]? Oxygen abundance 12+log(O/H) error obtained after applying the calibration from Carvalho et al. (2020MNRAS.492.5675C)stat.errorfloatnullable