J/ApJ/903/86ivo://CDS.VizieR/J/ApJ/903/86doi:10.26093/cds/vizier.19030086CDSMartinez-AldamaMartinez-Aldama M.L.Zajacek M.Czerny B.Panda S.2022-05-19T08:10:18Z2022-02-22T07:46:25ZCDS support team

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

cds-question@unistra.fractive-galactic-nucleiblack-holesultraviolet-astronomyThe usage of the radius-luminosity (R-L) relation for the determination of black hole masses across the cosmic history, as well as its application for cosmological studies, motivates us to analyze its scatter, which has recently increased significantly for both the optical (H{beta}) and UV (MgII) lines. To this purpose, we determined the scatter along the R-L relation for an up- to-date reverberation-mapped MgII sample. Studying linear combinations of the luminosity at 3000{AA} with independent parameters such as the FWHM, the UV FeII strength (R FeII ), and the fractional variability (F var) for the whole sample, we get only a small decrease in the scatter ({sigma}_rms_=0.29-0.30dex). Linear combinations with the dimensionless accretion rate (M) and the Eddington ratio lead to significant reductions of the scatter ({sigma}_rms_~0.1dex), albeit both suffering from the interdependency on the observed time delay. After the division into two subsamples considering the median value of the M in the full sample, we find that the scatter decreases significantly for the highly accreting subsample. In particular, the smallest scatter of {sigma}_rms_=0.17dex is associated with the independent parameter R FeII, followed by the combination with F var with {sigma}_rms_=0.19dex. Both of these independent observationally inferred parameters are in turn correlated with M and L_bol_/L_Edd_. These results suggest that the large scatter along the R-L relation is driven mainly by the accretion rate intensity.2020ApJ...903...86Mhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/903/86CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/MNRAS/268/305 : Variability of optically selected quasars (Hook+ 1994)J/ApJ/633/638 : Variable quasar sample from SDSS (Wilhite+, 2005)J/ApJ/698/895 : Variations in QSOs optical flux (Kelly+, 2009)J/ApJ/699/800 : Mass functions of active black holes (Vestergaard+, 2009)J/ApJ/736/86 : FeII emission in SDSS type 1 AGNs (Dong+, 2011)J/ApJ/782/45 : SEAMBHs. I. Mrk 142, Mrk 335, and IRAS F12397+3333 (Du+, 2014)J/ApJ/793/108 : SEAMBHs. II. Continuum and Hbeta LCs (Wang+, 2014)J/ApJ/806/22 : SEAMBHs IV. H{beta} time lags (Du+, 2015)J/ApJ/825/126 : SEAMBHs. V. The third year (Du+, 2016)J/ApJ/851/21 : SDSS RM project first year of observations (Grier+, 2017)J/ApJ/856/6 : SEAMBHs IX. 10 new H{beta} light curves (Du+, 2018)J/ApJ/865/56 : Emission line & R-band continuum LCs of 17 QSOs (Lira+, 2018)J/ApJ/880/46 : Spectroscopy & V-band monitoring of CTS C30.10 (Czerny+, 2019)J/ApJ/886/42 : Reverberation mapping & opt. spectra data of AGNs (Du+, 2019)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJ/903/86https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJ/903/86http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJ/903/86https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJ/903/86https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJ/903/86http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJ/903/86GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/ApJ/903/86/tableb1 (Observational properties for the full sample)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/ApJ/903/86/tableb1?https://vizier.iucaa.in/viz-bin/conesearch/J/ApJ/903/86/tableb1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/ApJ/903/86/tableb1?GETtext/xml+votable180.050000true213.346953.17620.0055555555555555565/2856 6/10741 10743 10749 11403 11428 11430 11432-11433https://cdsarc.cds.unistra.fr/viz-bin/moc/J/ApJ/903/86?format=asciiUVdefaultJ/ApJ/903/86/tableb1Observational properties for the full samplerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSample[1/2] Sample code (1)meta.code;src.sampleintIDObject identifiermeta.id;meta.maincharL3000[42.8/46.8] log continuum luminosity at 3000{AA}; erg/slog(1e-07W)phys.luminosityfloate_L3000[0.0002/0.2] Uncertainty in logL3000log(1e-07W)stat.errorfloattau[5.3/564] Time delay (2)dtime.intervalfloatE_tau[1.7/109] Upper uncertainty in taudstat.error;stat.maxfloate_tau[1.8/114] Lower uncertainty in taudstat.errorfloatFWHM[2214/10594] MgII line width; Full-Width Half-Maximumkm/sspect.line.widthinte_FWHM[14/2835] Uncertainty in FWHMkm/sstat.error;phys.angSizeintMdot[-2.08/2.52] log dimensionless accretion ratearith.rate;pos.distance;phys.sizefloatE_Mdot[0.2/1.3] Upper uncertainty in logMdotstat.error;stat.maxfloate_Mdot[0.2/1.3] Lower uncertainty in logMdotstat.errorfloatLb/LE[0.004/5.4] Eddington ratiostat.fit.omcfloatE_Lb/LE[0.003/3.1] Upper uncertainty in Lb/LEstat.error;stat.maxfloate_Lb/LE[0.002/4.2] Lower uncertainty in Lb/LEstat.error;phys.abundfloatRFeII[0.1/2.35]? The FeII strengthspect.line.intensity;arith.ratiofloatnullableE_RFeII[0.005/0.005]? Upper uncertainty in RFeIIstat.error;stat.maxfloatnullablee_RFeII[0.003/0.4]? Lower uncertainty in RFeIIstat.errorfloatnullableFvar[0.03/0.53] Fractional variabilitysrc.var.indexfloatClass[1/2] Classification (3)src.classint_RAPosition from Shen+, 2019, J/ApJS/241/34 (right ascension part)degpos.eq.ra;meta.mainnullable_DEPosition from Shen+, 2019, J/ApJS/241/34 (declination part)degpos.eq.dec;meta.mainnullable