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<ri:Resource created="2013-03-11T13:50:50Z" 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>Abundances of 19 K-type giants in moving groups</title><shortName>J/MNRAS/422/2969</shortName><identifier>ivo://CDS.VizieR/J/MNRAS/422/2969</identifier><altIdentifier>doi:10.26093/cds/vizier.74222969</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Liu F.</name></creator><creator><name>Chen Y.Q.</name></creator><creator><name>Zhao G.</name></creator><creator><name>Han I.</name></creator><creator><name>Lee B.C.</name></creator><creator><name>Kim K.M.</name></creator><creator><name>Zhao Z.S.</name></creator><date role="Updated">2024-07-17T20:15:44Z</date><date role="Created">2013-03-11T13:50:50Z</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>open-star-clusters</subject><subject>giant-stars</subject><subject>k-stars</subject><subject>chemical-abundances</subject><description>We present the stellar parameters of 19 K-type giants and their abundances for 13 chemical elements (Al, Ba, Ca, Fe, K, Mg, Mn, Na, Ni, Sc, Si, Ti and V), selected from two moving groups, covering the metallicity range of -0.6&lt;[Fe/H]&lt;0.2, based on high-resolution spectra. Most of the elemental abundances show similar trends as in previous studies, except for Al, Na and Ba, which are seriously affected by evolution. The abundance ratios of [Na/Mg] increase smoothly with higher [Mg/H], and those of [Al/Mg] decrease slightly with increasing [Mg/H]. The abundance ratios of [Mg/Ba] show a distinction between these two moving groups, which is mainly induced by chemical evolution and also partly by kinematic effects. The inhomogeneous metallicity of each star from the moving groups demonstrates that these stars had different chemical origins before they were kinematically aggregated. This favours a dynamical resonant theory.</description><source format="bibcode">2012MNRAS.422.2969L</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/422/2969</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/328/175">J/A+A/328/175 : K + M giants equivalent widths (Aoki+ 1997)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/636/821">J/ApJ/636/821 : Abundances of Baade's Window K giants (Fulbright+, 2006)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/735/L46">J/ApJ/735/L46 : Spectroscopy of 64 K red giants (Bensby+, 2011)</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/422/2969</accessURL><mirrorURL title="VizieR at IUCAA: Pune, India">https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/422/2969</mirrorURL><mirrorURL title="VizieR at SAAO: SAAO, South Africa">http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/422/2969</mirrorURL></interface></capability><capability><interface xsi:type="vs:ParamHTTP"><accessURL use="base">https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/422/2969</accessURL><mirrorURL title="VizieR at IUCAA: Pune, India">https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/422/2969</mirrorURL><mirrorURL title="VizieR at SAAO: SAAO, South Africa">http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/422/2969</mirrorURL><queryType>GET</queryType><resultType>text/xml+votable</resultType></interface></capability><capability standardID="ivo://ivoa.net/std/TAP#aux"><interface xsi:type="vs:ParamHTTP" role="std"><accessURL use="base">https://tapvizier.cds.unistra.fr/TAPVizieR/tap</accessURL></interface></capability><capability xsi:type="cs:ConeSearch" standardID="ivo://ivoa.net/std/ConeSearch"><description>Cone search capability for table J/MNRAS/422/2969/table5 (Stellar abundance ratios [X/Fe])</description><interface xsi:type="vs:ParamHTTP" role="std"><accessURL use="base">https://vizier.cds.unistra.fr/viz-bin/conesearch/J/MNRAS/422/2969/table5?</accessURL><mirrorURL title="VizieR at IUCAA: Pune, India">https://vizier.iucaa.in/viz-bin/conesearch/J/MNRAS/422/2969/table5?</mirrorURL><mirrorURL title="VizieR at SAAO: SAAO, South Africa">http://vizieridia.saao.ac.za/viz-bin/conesearch/J/MNRAS/422/2969/table5?</mirrorURL><queryType>GET</queryType><resultType>text/xml+votable</resultType></interface><maxSR>180.0</maxSR><maxRecords>50000</maxRecords><verbosity>true</verbosity><testQuery><ra>36.8657142</ra><dec>31.8012794</dec><sr>0.005555555555555556</sr></testQuery></capability><coverage><spatial>6/943 1204 1282 1917 5349 5666 6458 6486 6706 6933 6953 7155 7379 7434 7674 7772 23807 24271 24436</spatial><footprint ivo-id="ivo://ivoa.net/std/moc">https://cdsarc.cds.unistra.fr/viz-bin/moc/J/MNRAS/422/2969?format=ascii</footprint><waveband>Optical</waveband></coverage><tableset><schema><name>default</name><table><name>J/MNRAS/422/2969/table5</name><description>Stellar abundance ratios [X/Fe]</description><column><name>recno</name><description>Record number assigned by the VizieR team. Should Not be used for identification.</description><ucd>meta.record</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>Star</name><description>Star name</description><ucd>meta.id;meta.main</ucd><dataType xsi:type="vs:VOTableType" arraysize="8*">char</dataType><flag>primary</flag></column><column><name>[Al/Fe]</name><description>Abundance ratio [Al/Fe]</description><unit>log(Sun)</unit><ucd>phys.abund</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>[Ba/Fe]</name><description>Abundance ratio [Ba/Fe] (1)</description><unit>log(Sun)</unit><ucd>phys.abund</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>[Ca/Fe]</name><description>Abundance ratio [Ca/Fe]</description><unit>log(Sun)</unit><ucd>phys.abund</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>[K/Fe]</name><description>? 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