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<ri:Resource created="2024-11-25T08:24:05Z" status="active" updated="2025-07-18T20:13:18Z" version="1.2" xmlns:cs="http://www.ivoa.net/xml/ConeSearch/v1.0" xmlns:ri="http://www.ivoa.net/xml/RegistryInterface/v1.0" xmlns:vr="http://www.ivoa.net/xml/VOResource/v1.0" xmlns:vs="http://www.ivoa.net/xml/VODataService/v1.1" xmlns:xsi="http://www.w3.org/2001/XMLSchema-instance" xsi:schemaLocation="http://www.ivoa.net/xml/ConeSearch/v1.0 http://vo.ari.uni-heidelberg.de/docs/schemata/ConeSearch.xsd http://www.ivoa.net/xml/VOResource/v1.0 http://vo.ari.uni-heidelberg.de/docs/schemata/VOResource.xsd http://www.ivoa.net/xml/VODataService/v1.1 http://vo.ari.uni-heidelberg.de/docs/schemata/VODataService.xsd" xsi:type="vs:CatalogService"><title>z&lt;0.8 AGNs from MQC with robust lags from ZTF</title><shortName>J/ApJ/940/20</shortName><identifier>ivo://CDS.VizieR/J/ApJ/940/20</identifier><altIdentifier>doi:10.26093/cds/vizier.19400020</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Guo H.</name></creator><creator><name>Barth A.J.</name></creator><creator><name>Wang S.</name></creator><date role="Updated">2025-07-18T20:13:18Z</date><date role="Created">2024-11-25T08:24:05Z</date><contact><name>CDS support team</name><address>CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France</address><email>cds-question@unistra.fr</email></contact></curation><content><subject>active-galactic-nuclei</subject><subject>photometry</subject><subject>visible-astronomy</subject><subject>black-holes</subject><subject>redshifted</subject><description>We perform a systematic survey of active galactic nuclei (AGNs) continuum lags using ~3days cadence gri-band light curves from the Zwicky Transient Facility. We select a sample of 94 type 1 AGNs at z&lt;0.8 with significant and consistent inter-band lags based on the interpolated cross-correlation function method and the Bayesian method JAVELIN. Within the framework of the "lamp-post" reprocessing model, our findings are: (1) The continuum emission (CE) sizes inferred from the data are larger than the disk sizes predicted by the standard thin-disk model. (2) For a subset of the sample, the CE size exceeds the theoretical limit of the self-gravity radius (12 lt-days) for geometrically thin disks. (3) The CE size scales with continuum luminosity as R_CE_{propto}L^0.48+/-0.04^ with a scatter of 0.2dex, analogous to the well-known radius-luminosity relation of broad H{beta}. These findings suggest a significant contribution of diffuse continuum emission from the broad-line region (BLR) to AGN continuum lags. We find that the R_CE_-L relation can be explained by a photoionization model that assumes ~23% of the total flux comes from the diffuse BLR emission. In addition, the ratio of the CE size and model-predicted disk size anticorrelates with the continuum luminosity, which is indicative of a potential nondisk BLR lag contribution evolving with the luminosity. Finally, a robust positive correlation between the CE size and black hole mass is detected.</description><source format="bibcode">2022ApJ...940...20G</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/940/20</referenceURL><type>Catalog</type><contentLevel>Research</contentLevel><relationship><relationshipType>IsServedBy</relationshipType><relatedResource ivo-id="ivo://CDS.VizieR/TAP">TAP VizieR generic service</relatedResource></relationship><relationship><relationshipType>IsServedBy</relationshipType><relatedResource>Conesearch service</relatedResource></relationship><relationship><relationshipType>related-to</relationshipType><relatedResource ivo-id="ivo://CDS.VizieR/VII/294">VII/294 : The Million Quasars (Milliquas) catalogue, version 8 (Flesch, 2023)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+AS/110/469">J/A+AS/110/469 : AGN from the RASS (Bade+, 1995)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+AS/128/507">J/A+AS/128/507 : The Hamburg Quasar Survey. 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Log monochromatic luminosity at 5100{AA} from L19 (Liu+ 2019, J/ApJS/243/21); erg/s (L5100_L19)</description><unit>log(1e-07W)</unit><ucd>phys.luminosity;em.opt.V</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>logBHL19</name><description>[6/9.2]? Log virial BH mass based on H{beta} from L19 (LOGBH_L19) (3)</description><unit>log(solMass)</unit><ucd>phys.mass</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>L19</name><description>Display data from Liu+ 2019, J/ApJS/243/21 within 3"</description><ucd>meta.ref.url</ucd><dataType xsi:type="vs:VOTableType">int</dataType><flag>nullable</flag></column><column><name>L5100R20</name><description>[43.8/46.3]? Log monochromatic luminosity at 5100{AA} from R20 (Rakshit+ 2020, J/ApJS/249/17); erg/s (L5100_R20)</description><unit>log(1e-07W)</unit><ucd>phys.luminosity;em.opt.V</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>logBHR20</name><description>[7/10]? Log virial BH mass based on H{beta} from R20 (LOGBH_R20) (4)</description><unit>log(solMass)</unit><ucd>phys.mass</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>L5100S18</name><description>[43.6/46.2]? Log monochromatic luminosity at 5100{AA} from S18 (Shangguan+ 2018, J/ApJ/854/158); erg/s (L5100_S18)</description><unit>log(1e-07W)</unit><ucd>phys.luminosity;em.opt.V</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>logBHS18</name><description>[7/10]? Log virial BH mass based on H{beta} from S18 (LOGBH_S18) (4)</description><unit>log(solMass)</unit><ucd>phys.mass</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>S18</name><description>Display data from Shangguan+ 2018, J/ApJ/854/158 within 3"</description><ucd>meta.ref.url</ucd><dataType xsi:type="vs:VOTableType">int</dataType><flag>nullable</flag></column><column><name>L5100RM</name><description>[42.88/45.7]? Log monochromatic luminosity at 5100{AA} from RM (L5100_RM)</description><unit>log(1e-07W)</unit><ucd>phys.luminosity;em.opt.V</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>logBHRM</name><description>[6.9/9.1]? Log RM BH mass based on H{beta} (LOGBH_RM) (5)</description><unit>log(solMass)</unit><ucd>phys.mass</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>L5100LA</name><description>[0/46.2]? Log monochromatic luminosity at 5100{AA} from LAMOST (L5100_LAMOST)</description><unit>log(1e-07W)</unit><ucd>phys.luminosity;em.opt.V</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>logBHLA</name><description>[0/10]? Log virial BH mass based on H{beta} from LAMOST DR1 to DR5 (LOGBH_LAMOST) (4)</description><unit>log(solMass)</unit><ucd>phys.mass</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>L5100m</name><description>[43/46.2]? Log monochromatic luminosity at 5100{AA} from self-measurements (L5100_MEASURED)</description><unit>log(1e-07W)</unit><ucd>phys.luminosity;em.opt.V</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>logBHm</name><description>[6.6/9.5]? Log virial BH mass based on H{beta} (LOGBH_MEASURED) (4)</description><unit>log(solMass)</unit><ucd>phys.mass</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>L5100</name><description>[42.47/46.3]? Log adopted fiducial monochromatic luminosity at 5100{AA} (L5100)</description><unit>log(1e-07W)</unit><ucd>phys.luminosity;em.opt.V</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>logBH</name><description>[6/10]? Log adopted fiducial virial BH mass (LOGBH)</description><unit>log(solMass)</unit><ucd>phys.mass</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>logEdd</name><description>[0.003/4]? Eddington ratio based on fiducial luminosity &amp; BH mass (LOG_EDD)</description><ucd>phys.luminosity;arith.ratio</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>R2500SSD</name><description>[0.04/7.6]? Shakura-Sunyaev disk (SSD) predicted disk size at 2500{AA} based on Eq 2 (R2500_SSD) (6)</description><ucd>phys.size;em.UV.200-300nm</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>R2500ICCF</name><description>[0.08/13.2]? CE size at 2500{AA} based on observed inter-band lag modeling (R2500_ICCF) (6)</description><ucd>phys.size;em.UV.200-300nm</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>e_R2500ICCF</name><description>[0/3]? Measurement error in R2500-ICCF (R2500_ERR_ICCF) (6)</description><ucd>stat.error;phys.size;em.UV.200-300nm</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column></table></schema></tableset></ri:Resource>