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<ri:Resource created="2017-03-07T10:23:50Z" status="active" updated="2025-06-13T15:25:00Z" 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 properties of z &lt; 0.3 quasars</title><shortName>J/MNRAS/466/921</shortName><identifier>ivo://CDS.VizieR/J/MNRAS/466/921</identifier><altIdentifier>doi:10.26093/cds/vizier.74660921</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Coziol R.</name></creator><creator><name>Andernach H.</name></creator><creator><name>Torres-Papaqui J.P.</name></creator><creator><name>Ortega-Minakata R.A.,Moreno del Rio F.</name></creator><date role="Updated">2024-08-17T20:18:05Z</date><date role="Created">2017-03-07T10:23:50Z</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>quasars</subject><subject>radio-sources</subject><subject>surveys</subject><description>To better constrain the hypotheses proposed to explain why only a few quasars are radio loud (R_L_), we compare the characteristics of 1958 nearby (z&lt;=0.3) SDSS (Sloan Digital Sky Survey) quasars, covered by the FIRST (Faint Images of the Radio Sky at Twenty Centimeters) and NVSS (NRAO VLA Sky Survey) radio surveys. Only 22 per cent are R_L_ with log(L_1.4GHz_)&gt;=22.5W/Hz, the majority being compact (C), weak radio sources (WRS), with log(L_1.4GHz_)&lt;24.5W/Hz. 15 per cent of the RL quasars have extended radio morphologies: 3 per cent have a core and a jet (J), 2 per cent have a core with one lobe (L), and 10 per cent have a core with two lobes (T), the majority being powerful radio sources (PRS), with log(L_1.4GHz_)&gt;=24.5W/Hz. In general, RL quasars have higher bolometric luminosities and ionization powers than radio-quiet (RQ) quasars. The WRS have comparable black hole (BH) masses as the RQ quasars, but higher accretion rates or radiative efficiencies. The PRS have higher BH masses than the WRS, but comparable accretion rates or radiative efficiencies. The WRS also have higher FWHM_{[OIII]} than the PRS, consistent with a coupling of the spectral characteristics of the quasars with their radio morphologies. Inspecting the SDSS images and applying a neighbour search algorithm reveal no difference between the RQ and RL quasars of their host galaxies, environments, and interaction. Our results prompt the conjecture that the phenomenon that sparks the RL phase in quasars is transient, intrinsic to the active galactic nuclei, and stochastic, due to the chaotic nature of the accretion process of matter on to the BHs.</description><source format="bibcode">2017MNRAS.466..921C</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/466/921</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/VIII/65">VIII/65 : 1.4GHz NRAO VLA Sky Survey (NVSS) (Condon+ 1998)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/VII/260">VII/260 : The 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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>SDSS</name><description>SDSS DR7 object designation (1)</description><ucd>meta.id;meta.main</ucd><dataType xsi:type="vs:VOTableType" arraysize="19*">char</dataType></column><column><name>z</name><description>SDSS redshift from 2010AJ....139.2360S</description><ucd>src.redshift</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>FWHMHb</name><description>Width of H{beta} emission line</description><unit>km/s</unit><ucd>spect.line.width;em.line.Hbeta</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>lgL5100</name><description>log10 of 5100{AA} continuum luminosity (2)</description><unit>log(W)</unit><ucd>phys.luminosity</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>lgMBH</name><description>log10 of black hole mass in solar masses (2)</description><unit>log(solMass)</unit><ucd>phys.mass</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>lgLbol</name><description>log10 of bolometric luminosity (2)</description><unit>log(W)</unit><ucd>phys.luminosity</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>Gamma</name><description>Eddington ratio L_bol_/L_Edd_</description><ucd>phys.luminosity;arith.ratio</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>FWHMOIII</name><description>Width of the OIII emission line</description><unit>km/s</unit><ucd>spect.line.width;em.line.OIII</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>lgLOIII</name><description>log10 of OIII emission-line luminosity (2)</description><unit>log(W)</unit><ucd>phys.luminosity;em.line.OIII</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>N0.5</name><description>? Number of neighbors within 0.5Mpc (3)</description><ucd>meta.number</ucd><dataType xsi:type="vs:VOTableType">int</dataType><flag>nullable</flag></column><column><name>N1.0</name><description>? Number of neighbors within 1.0Mpc (3)</description><ucd>meta.number</ucd><dataType xsi:type="vs:VOTableType">int</dataType><flag>nullable</flag></column><column><name>N1.5</name><description>? Number of neighbors within 1.5Mpc (3)</description><ucd>meta.number</ucd><dataType xsi:type="vs:VOTableType">int</dataType><flag>nullable</flag></column><column><name>Rmorph</name><description>Morphological type of radio emission (4)</description><ucd>src.morph.type</ucd><dataType xsi:type="vs:VOTableType" arraysize="2*">char</dataType></column><column><name>l_lgLrad</name><description>[&lt;] Limit flag on lgLrad</description><ucd>meta.code.error</ucd><dataType xsi:type="vs:VOTableType" arraysize="1*">char</dataType></column><column><name>lgLrad</name><description>Monochromatic 1.4-GHz luminosity (2)</description><unit>log(W.Hz**-1)</unit><ucd>phys.luminosity;em.radio.750-1500MHz</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>LLS</name><description>? 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