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<ri:Resource created="2000-10-08T10:00:05Z" status="active" updated="2025-05-19T09:50:00Z" 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>Variability &amp; polarization of luminous quasars</title><shortName>J/A+A/353/77</shortName><identifier>ivo://CDS.VizieR/J/A+A/353/77</identifier><altIdentifier>doi:10.26093/cds/vizier.33530077</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Teerikorpi P.</name></creator><date role="Updated">2012-11-13T12:39:25Z</date><date role="Created">2000-10-08T10:00:05Z</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>quasars</subject><subject>visible-astronomy</subject><subject>broad-band-photometry</subject><subject>polarimetry</subject><description>We use 250 radio loud quasars with UBV photometry available and z&lt;1.65, to study whether there is a gap in the distribution of absolute magnitudes, from M_V_~-25.8 (for H_0_=100km/s/Mpc, q_0_=0.5) to -25.3, as was suggested by Teerikorpi (1981A&amp;A....98..309T; Paper I). In Paper I it was also proposed that there is a class of the most luminous radio quasars, differing in some properties from fainter quasars on the other side of the gap. The main conclusion of Paper I remains intact. The gap in the distribution of absolute magnitudes is confirmed with the new formalism of cosmological Malmquist bias (Teerikorpi, 1998A&amp;A...339..647T), which allows one to use heterogeneous samples with magnitude inhomogeneity.</description><source format="bibcode">2000A&amp;A...353...77T</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/353/77</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/J/A+A/321/123">J/A+A/321/123 : Optical variability of QSOs (Cristiani+ 1997)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+AS/143/357">J/A+AS/143/357 : Tuorla Quasar Monitoring (Katajainen+ 2000)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/MNRAS/260/202">J/MNRAS/260/202 : Quasar luminosity function (Hawkins+, 1993)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/MNRAS/268/305">J/MNRAS/268/305 : Variability of optically selected quasars (Hook+ 1994)</relatedResource></relationship></content><rights>https://cds.unistra.fr/vizier-org/licences_vizier.html</rights><capability><interface xsi:type="vr:WebBrowser"><accessURL use="full">https://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/353/77</accessURL><mirrorURL title="VizieR at IUCAA: Pune, India">https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/353/77</mirrorURL><mirrorURL title="VizieR at SAAO: SAAO, South Africa">http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/353/77</mirrorURL></interface></capability><capability><interface xsi:type="vs:ParamHTTP"><accessURL 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