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<ri:Resource created="2020-10-27T09:36:48Z" 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>Multiple populations of extrasolar gas giants</title><shortName>J/ApJ/876/23</shortName><identifier>ivo://CDS.VizieR/J/ApJ/876/23</identifier><altIdentifier>doi:10.26093/cds/vizier.18760023</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Goda S.</name></creator><creator><name>Matsuo T.</name></creator><date role="Updated">2021-09-08T13:15:42Z</date><date role="Created">2020-10-27T09:36:48Z</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>exoplanets</subject><subject>stellar-masses</subject><subject>metallicity</subject><description>There are two planetary formation scenarios: core accretion and gravitational disk instability. Based on the fact that gaseous objects are preferentially observed around metal-rich host stars, most extrasolar gaseous objects discovered to date are thought to have been formed by core accretion. Here, we present 569 samples of gaseous planets and brown dwarfs found in 485 planetary systems that span three mass regimes with boundary values at 4 and 25 Jupiter-mass masses through performing cluster analyses of these samples regarding the host-star metallicity, after minimizing the impact of the selection effect of radial-velocity measurement on the cluster analysis. The larger mass is thought to be the upper mass limit of the objects that were formed during the planetary formation processes. In contrast, the lower mass limit appears to reflect the difference between planetary formation processes around early-type and G-type stars; disk instability plays a greater role in the planetary formation process around early-type stars than that around G-type stars. Populations with masses between 4 and 25 Jupiter masses that orbit early-type stars comprise planets formed not only via the core-accretion process but also via gravitational disk instability because the population preferentially orbits metal-poor stars or is independent of the host-star metallicity. Therefore, it is essential to have a hybrid scenario for the planetary formation of the diverse systems.</description><source format="bibcode">2019ApJ...876...23G</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/876/23</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+AS/141/371">J/A+AS/141/371 : Low-mass stars evolutionary tracks (Girardi+, 2000)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/398/363">J/A+A/398/363 : Statistical properties of exoplanets II (Santos+, 2003)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/622/1102">J/ApJ/622/1102 : The planet-metallicity correlation. (Fischer+, 2005)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/646/505">J/ApJ/646/505 : Catalog of nearby exoplanets (Butler+, 2006)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/654/625">J/ApJ/654/625 : Radial velocities of 9 long-period objects (Wittenmyer+, 2007)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/487/373">J/A+A/487/373 : Spectroscopic parameters of 451 HARPS-GTO stars (Sousa+, 2008)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/505/1311">J/A+A/505/1311 : Radial velocity curves of 11 UMa &amp; HD 32518 (Dollinger+, 2009)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/507/1659">J/A+A/507/1659 : Radial velocity measurements of 30 Ari B (Guenther+, 2009)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/530/A138">J/A+A/530/A138 : Geneva-Copenhagen survey re-analysis (Casagrande+, 2011)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/556/A150">J/A+A/556/A150 : SWEETCat I. 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DR25 reliability (Thompson+, 2018)</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/ApJ/876/23</accessURL><mirrorURL title="VizieR at IUCAA: Pune, India">https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJ/876/23</mirrorURL><mirrorURL title="VizieR at SAAO: SAAO, South Africa">http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJ/876/23</mirrorURL></interface></capability><capability><interface xsi:type="vs:ParamHTTP"><accessURL use="base">https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJ/876/23</accessURL><mirrorURL title="VizieR at IUCAA: Pune, India">https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJ/876/23</mirrorURL><mirrorURL title="VizieR at SAAO: SAAO, South 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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>ID</name><description>Planet identifier</description><ucd>meta.id;meta.main</ucd><dataType xsi:type="vs:VOTableType" arraysize="18*">char</dataType></column><column><name>MajAxis</name><description>[0.02/22] Semi-major axis (1)</description><unit>AU</unit><ucd>phys.size.smajAxis</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>e_MajAxis</name><description>[0/3.4] Uncertainty in MajAxis</description><unit>AU</unit><ucd>stat.error;phys.angSize</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>l_Msini</name><description>[l] l=lower limit of companion mass was applied as that listed in Ref</description><ucd>meta.code.error</ucd><dataType xsi:type="vs:VOTableType" arraysize="1*">char</dataType></column><column><name>Msini</name><description>[0.3/103.1] Planet mass times sine of inclination</description><unit>(1.898187x10+27kg)</unit><ucd>phys.mass</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>e_Msini</name><description>[0/28.7] Uncertainty in Msini</description><unit>(1.898187x10+27kg)</unit><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>K</name><description>[3.1/6114]? 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