J/MNRAS/422/3268ivo://CDS.VizieR/J/MNRAS/422/3268doi:10.26093/cds/vizier.74223268CDSJin C.Ward M.Done C.2024-07-17T20:15:48Z2013-03-20T13:20:19ZCDS support team

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

cds-question@unistra.fractive-galactic-nucleix-ray-sourcesIn this second paper in a series of three, we study the properties of the various emission features and underlying continuum in the optical spectra of type 1 active galactic nuclei (AGNs) by using the unobscured hard X-ray emission as a diagnostic. We introduce the use of the "correlation spectrum technique" (CST) for the first time. We use this to show the strength of the correlation between the hard X-ray luminosity and each wavelength of the optical spectrum. This shows that for broad-line Seyfert 1 galaxies all the strong emission lines (the broad component of H{alpha} and H{beta}, [NeIII] {lambda}{lambda}3869/3967, [OI] {lambda}{lambda}6300/6364, [OII] {lambda}{lambda}3726/3729 and [OIII] {lambda}{lambda}4959/5007) and the optical underlying continuum all strongly correlate with the hard X-ray emission. In contrast, the narrow-line Seyfert 1 galaxies show a stronger correlation in the optical continuum but a weaker correlation in the lines.2012MNRAS.422.3268Jhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/422/3268CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/422/3268https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/422/3268http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/422/3268https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/422/3268https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/422/3268http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/422/3268GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapX-raydefaultJ/MNRAS/422/3268/tableb1Spearman's Rank Correlation Coefficients of SED components vs. H{alpha}, H{beta} and [OIII]5007 line parameters.recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintParamLine parameter designationmeta.id;stat.fit.paramcharCompComponent (1)meta.code.multipcharDisc1rSpearman's rank correlation coefficient, Disc composant, SED component luminositystat.correlationfloatDisc1dLogarithm of the significance level of being random distribution, Disc composant, SED component luminosity (2)stat.fit.goodnessintComp1rSpearman's rank correlation coefficient, soft X-ray Comptonisation component, SED component luminositystat.correlationfloatComp1dLogarithm of the significance level of being random distribution, soft X-ray Comptonisation component, SED component luminosity (2)stat.fit.goodnessintPL1dSpearman's rank correlation coefficient, hard X-ray Comptonisation component composant, SED component luminositystat.fit.goodnessfloatPL1rLogarithm of the significance level of being random distribution, hard X-ray Comptonisation component composant, SED component luminosity (2)stat.correlationintC+P1dSpearman's rank correlation coefficient, sum of soft and hard X-ray Comptonisation emission (i.e. corona emission), SED component luminositystat.fit.goodnessfloatC+P1rLogarithm of the significance level of being random distribution, sum of soft and hard X-ray Comptonisation emission (i.e. corona emission), SED component luminosity (2)stat.correlationintBol1dSpearman's rank correlation coefficient, Bolometric composant, SED component luminositystat.fit.goodnessfloatBol1rLogarithm of the significance level of being random distribution, Bolometric composant, SED component luminosity (2)stat.correlationintDisc2rSpearman's rank correlation coefficient, Disc composant, SED component fraction (fraction of each component in the bolometric luminosity)stat.correlationfloatDisc2dLogarithm of the significance level of being random distribution, Disc composant, SED component fraction (fraction of each component in the bolometric luminosity) (2)stat.fit.goodnessintComp2rSpearman's rank correlation coefficient, soft X-ray Comptonisation component, SED component fraction (fraction of each component in the bolometric luminosity)stat.correlationfloatComp2dLogarithm of the significance level of being random distribution, soft X-ray Comptonisation component, SED component fraction (fraction of each component in the bolometric luminosity) (2)stat.fit.goodnessintPL2dSpearman's rank correlation coefficient, hard X-ray Comptonisation component composant, SED component fraction (fraction of each component in the bolometric luminosity)stat.fit.goodnessfloatPL2rLogarithm of the significance level of being random distribution, hard X-ray Comptonisation component composant, SED component fraction (fraction of each component in the bolometric luminosity) (2)stat.correlationintC+P2dSpearman's rank correlation coefficient, sum of soft and hard X-ray Comptonisation emission (i.e. corona emission), SED component fraction (fraction of each component in the bolometric luminosity)stat.fit.goodnessfloatC+P2rLogarithm of the significance level of being random distribution, sum of soft and hard X-ray Comptonisation emission (i.e. corona emission), SED component fraction (fraction of each component in the bolometric luminosity) (2)stat.correlationintGammarSpearman's rank correlation coefficient, {Gamma}_2-10keV_, 2-10keV energy bandstat.correlationfloatGammadLogarithm of the significance level of being random distribution, {Gamma}_2-10keV_, 2-10keV energy band (2)stat.fit.goodnessintLuminrSpearman's rank correlation coefficient, Luminosity, 2-10keV energy bandstat.correlationfloatLumindLogarithm of the significance level of being random distribution, Luminosity, 2-10keV energy band (2)stat.fit.goodnessintfracdSpearman's rank correlation coefficient, fraction of 2-10keV luminosity related to bolometric luminosity, 2-10keV energy bandstat.fit.goodnessfloatfracrLogarithm of the significance level of being random distribution, fraction of 2-10keV luminosity related to bolometric luminosity, 2-10keV energy band (2)stat.correlationint