J/MNRAS/454/766ivo://CDS.VizieR/J/MNRAS/454/766doi:10.26093/cds/vizier.74540766CDSAsmus D.Gandhi P.Honig S.F.Smette A.Duschl W.J.2024-08-15T20:16:25Z2018-01-15T08:17:35ZCDS support team

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

cds-question@unistra.fractive-galactic-nucleiseyfert-galaxiesgalaxiesinfrared-sourcesx-ray-sourcesWe present an updated mid-infrared (MIR) versus X-ray correlation for the local active galactic nuclei (AGN) population based on the high angular resolution 12 and 18{mu}m continuum fluxes from the AGN subarcsecond MIR atlas and 2-10 keV and 14-195 keV data collected from the literature. We isolate a sample of 152 objects with reliable AGN nature and multi-epoch X-ray data and minimal MIR contribution from star formation. Although the sample is not homogeneous or complete, we show that our results are unlikely to be affected by significant biases. The MIR-X-ray correlation is nearly linear and within a factor of 2 independent of the AGN type and the wavebands used. The observed scatter is <0.4 dex. A possible flattening of the correlation slope at the highest luminosities probed (~10^45^ erg/s) towards low MIR luminosities for a given X-ray luminosity is indicated but not significant. Unobscured objects have, on average, an MIR-X-ray ratio that is only <=0.15 dex higher than that of obscured objects. Objects with intermediate X-ray column densities (22<logN_H_<23) actually show the highest MIR-X-ray ratio on average. Radio-loud objects show a higher mean MIR-X-ray ratio at low luminosities while the ratio is lower than average at high luminosities. This may be explained by synchrotron emission from the jet contributing to the MIR at low luminosities and additional X-ray emission at high luminosities. True Seyfert 2 candidates do not show any deviation from the general behaviour suggesting that they possess a dusty obscurer as in other AGN. Double AGN also do not deviate. Finally, we show that the MIR-X-ray correlation can be used to investigate the AGN nature of uncertain objects. Specifically, we give equations that allow us to determine the intrinsic 2-10 keV luminosities and column densities for objects with complex X-ray properties to within 0.34 dex. These techniques are applied to the uncertain objects of the remaining AGN MIR atlas, demonstrating the usefulness of the MIR-X-ray correlation as an empirical tool.2015MNRAS.454..766Ahttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/454/766CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/A+A/418/465 : Mid-infrared and hard X-ray emission in AGN (Lutz+, 2004)J/ApJ/610/128 : NIR colors of hard X-ray-selected AGN (Watanabe+, 2004)J/ApJ/705/14 : Seyfert galaxies in the mid-IR (Deo+, 2009)J/A+A/524/A64 : The 54-month Palermo BAT-survey catalogue (Cusumano+, 2010)J/ApJ/725/2270 : Mid-IR emission lines in AGNs (Pereira-Santaella+, 2010)J/ApJ/754/45 : IR properties of Swift/BAT X-ray AGNs (Ichikawa+, 2012)J/ApJS/207/19 : Hard X-ray survey from Swift-BAT 2004-2010J/MNRAS/439/1648 : Subarcsecond mid-infrared atlas of local AGN (Asmus+, 2014)J/ApJ/807/129 : X-ray to MIR luminosities relation of AGNs (Stern, 2015)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/454/766https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/454/766http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/454/766https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/454/766https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/454/766http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/454/766GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/MNRAS/454/766/table2 (Reliable sample)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/MNRAS/454/766/table2?https://vizier.iucaa.in/viz-bin/conesearch/J/MNRAS/454/766/table2?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/MNRAS/454/766/table2?GETtext/xml+votable180.050000true66.5029792-57.20047060.0055555555555555566/18 1701 4116 4439 5091 5975-5976 7606 7659 7869 7959 8264 8299 8922 10265 10355 10454 10475 10839 10912 10924-10925 10927 10977 11027 12241 12380 13707 14744 14858 16301 16690 17075 17369 17525 17727 17748 17754 17795 17814 17819 18017 18365 18484 18524 18683 18935 19283 19433 19619 19730 19746 19932 20489 21036 21450 22890 22912 23167 23269 23323 23469 24842 25035 25083 25182 25610 25790 25907 26148 26292 26393 26547 27191 27382 27426 27714 27721 27765 27767 27773 27914 28075 28259 28495 28535 29795 30140 31080 33034 33716 33930 33954 33958 34104 34294 34318 34412 34493 34531 34881 34913 35246 35608 35623 35993 36005 36158 36668 36765 36785-36786 36861 36896 37650 38268 38479 38653 38868 38948 39182 39487 40221 40410 40777 40818 41586 42016 43262 43625 43634 43677 43806 43877 43925 44507 44551 44650 44660 45735 45779 45883 46568 46615 46987 47047 47107 47120 47154 47169 49042https://cdsarc.cds.unistra.fr/viz-bin/moc/J/MNRAS/454/766?format=asciiX-rayInfrareddefaultJ/MNRAS/454/766/table2Reliable sampleSimbadNameSimbad column added by the CDSmeta.idcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameShort object namemeta.id;meta.maincharDistDistanceMpcpos.distance;pos.heliocentricfloatOClassOptical class (1)src.classcharl_logL12[<= ] Limit flag on logL12meta.code.errorcharlogL12Nuclear 12{mu}m luminosity from Asmus et al. (2014, J/MNRAS/439/1648) (in erg/s)log(1e-07W)phys.luminosity;em.IR.8-15umfloate_logL12? Uncertainty in logL12log(1e-07W)stat.errorfloatnullablel_logL18[<= ] Limit flag on logL18meta.code.errorcharlogL18? Nuclear 18{mu}m luminosity from Asmus et al. (2014, J/MNRAS/439/1648) (in erg/s)log(1e-07W)phys.luminosity;em.IRfloatnullablee_logL18? Uncertainty in logL18log(1e-07W)stat.errorfloatnullableNepNumber of 2-10 keV epochs usedmeta.numbercharlogLobsAverage observed 2-10 keV luminosity (in erg/s)log(1e-07W)phys.luminosity;em.X-rayfloate_logLobsUncertainty in logLobslog(1e-07W)stat.errorfloatl_logNH[<>= ] Limit flag on logNHmeta.code.errorcharlogNHAverage X-ray column densitylog(cm**-2)phys.columnDensity;stat.meanfloate_logNH? Uncertainty in logNHlog(cm**-2)stat.errorfloatnullablelogLintAverage absorption-corrected 2-10 keV luminositylog(1e-07W)phys.luminosity;em.X-rayfloate_logLint? Uncertainty in logLintlog(1e-07W)stat.errorfloatnullablel_logL[<= ] Limit flag on logLmeta.code.errorcharlogLAverage observed 14-195 keV luminosity from Swift/BAT (2)log(1e-07W)phys.luminosity;em.X-rayfloate_logL? Uncertainty in logLlog(1e-07W)stat.errorfloatnullableFlag[01?] Radio-loudness flag (see Section 4.6 for explanation) (3)meta.code.errorcharRefReference(s) for the 2-10 keV luminosities and column densities (see refs.dat file)meta.ref;pos.framecharPapIDisplay data from Paper I (Asmus+, 2014, J/MNRAS/439/1648) for this objectmeta.ref.urlchar_RARight Ascension (J2000) from SIMBAD (not part of the original data)degpos.eq.ra;meta.main_DEDeclination (J2000) from SIMBAD (not part of the original data)degpos.eq.dec;meta.mainJ/MNRAS/454/766/refsReferencesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintRef[1/209] Reference numbermeta.id;meta.mainintAutAuthor's name(s)meta.bib.authorcharBibcodeBibcodemeta.bib.bibcodecharComComment on referencemeta.notechar