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<ri:Resource created="2022-08-01T09:53:26Z" 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>Radio-loud quasars luminosity distances</title><shortName>J/MNRAS/515/1358</shortName><identifier>ivo://CDS.VizieR/J/MNRAS/515/1358</identifier><altIdentifier>doi:10.26093/cds/vizier.75151358</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Huang L.</name></creator><creator><name>Chang Z.X.</name></creator><date role="Updated">2024-08-22T20:15:58Z</date><date role="Created">2022-08-01T09:53:26Z</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>radio-sources</subject><subject>stellar-distance</subject><description>We use the X-ray luminosity relation of radio-loud quasars (RLQs) to measure these luminosity distances as well as estimate cosmological parameters. We adopt four parametric models of X-ray luminosity to test luminosity correlation for RLQs and radio-intermediate quasars (RIQs) and give these cosmological distances. By Bayesian information criterion (BIC), the data suggest that the luminosity relation L_X_{prop.to}L_UV_^gamma-uv^L_Radio_^gamma-radio^ for RLQs has better goodness of fit, relative to other models, which can be interpreted as this relation being preferred for RLQs. Meanwhile, we compare the results from flat-spectrum radio-loud quasars (FSRLQs) and steep-spectrum radio-loud quasars (SSRLQs), which indicate that their luminosity correlations are not exactly the same. We also consider dividing the RLQs sample into various redshift bins, which can be used to check if the X-ray luminosity relation depends on the redshift. Finally, we apply a combination of RLQs and SNla Pantheon to verify the nature of dark energy concerning.</description><source format="bibcode">2022MNRAS.515.1358H</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/515/1358</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></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/MNRAS/515/1358</accessURL><mirrorURL title="VizieR at IUCAA: Pune, India">https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/515/1358</mirrorURL><mirrorURL title="VizieR at 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Should Not be used for identification.</description><ucd>meta.record</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>Name</name><description>SDSS name of radio-loud quasars (HHMMSS.ss+DDMMSS.s)</description><ucd>meta.id;meta.main</ucd><dataType xsi:type="vs:VOTableType" arraysize="18*">char</dataType></column><column><name>imag</name><description>SDSS i magnitude</description><unit>mag</unit><ucd>phot.mag;em.opt.I</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>FUV</name><description>Rest-frame flux at 2500 Angstroem (in erg/s/Hz/m^2^)</description><unit>1e-07W.Hz**-1.m**-2</unit><ucd>phot.flux;em.UV</ucd><dataType xsi:type="vs:VOTableType">double</dataType></column><column><name>Fradio</name><description>Rest-frame flux at 5GHz (in erg/s/Hz/m^2^)</description><unit>1e-07W.Hz**-1.m**-2</unit><ucd>phot.flux.density;em.radio</ucd><dataType xsi:type="vs:VOTableType">double</dataType></column><column><name>FX</name><description>Rest-frame flux at 2keV (in erg/s/Hz/m^2^)</description><unit>1e-07W.Hz**-1.m**-2</unit><ucd>phot.flux;em.X-ray</ucd><dataType xsi:type="vs:VOTableType">double</dataType></column><column><name>logR</name><description>The radio loudness (in logarithm scale)</description><ucd>phot.flux;arith.ratio</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>alphar</name><description>Radio slope</description><ucd>spect.index</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>DM</name><description>Distance modulus</description><ucd>phot.mag.distMod</ucd><dataType xsi:type="vs:VOTableType">double</dataType></column><column><name>e_DM</name><description>Error on distance modulus</description><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">double</dataType></column><column><name>Sloan</name><description>Display the online SDSS data</description><ucd>meta.ref.url</ucd><dataType xsi:type="vs:VOTableType" arraysize="*">char</dataType></column><column><name>_RA</name><description>Positions from SDSS name (right ascension part)</description><unit>deg</unit><ucd>pos.eq.ra;meta.main</ucd></column><column><name>_DE</name><description>Positions from SDSS name (declination part)</description><unit>deg</unit><ucd>pos.eq.dec;meta.main</ucd></column></table></schema></tableset></ri:Resource>