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<ri:Resource created="2017-05-30T14:35:19Z" 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 for all seven stars in Latham 1</title><shortName>J/AJ/152/176</shortName><identifier>ivo://CDS.VizieR/J/AJ/152/176</identifier><altIdentifier>doi:10.26093/cds/vizier.51520176</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>O'Connell J.E.</name></creator><creator><name>Martens K.</name></creator><creator><name>Frinchaboy P.M.</name></creator><date role="Updated">2017-07-18T15:13:54Z</date><date role="Created">2017-05-30T14:35:19Z</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>stellar-associations</subject><subject>line-intensities</subject><subject>chemical-abundances</subject><description>We present elemental abundances for all seven stars in Moving Group W11450 (Latham 1) to determine if they may be chemically related. These stars appear to be both spatially and kinematically related, but no spectroscopic abundance analysis exists in literature. Abundances for eight elements were derived via equivalent width analyses of high-resolution (R~60000), high-signal-to-noise ratio (&lt;S/N&gt; ~100) spectra obtained with the Otto Struve 2.1m telescope and the Sandiford Echelle Spectrograph at McDonald Observatory. The large star-to-star scatter in metallicity, -0.55{&lt;=}[Fe/H]{&lt;=}0.06dex ({sigma}=0.25), implies these stars were not produced from the same chemically homogeneous molecular cloud, and are therefore not part of a remnant or open cluster as previously proposed. Prior to this analysis, it was suggested that two stars in the group, W11449 and W11450, are possible wide binaries. The candidate wide binary pair show similar chemical abundance patterns with not only iron but with other elements analyzed in this study, suggesting the proposed connection between these two stars may be real.</description><source format="bibcode">2016AJ....152..176O</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/AJ/152/176</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/B/ocl">B/ocl : Optically visible open clusters and Candidates (Dias+ 2002-2015)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/VI/135">VI/135 : All-sky spectrally matched Tycho2 stars (Pickles+, 2010)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/V/136">V/136 : Teff and metallicities for Tycho-2 stars (Ammons+, 2006)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/I/259">I/259 : The Tycho-2 Catalogue (Hog+ 2000)</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/AJ/152/176</accessURL><mirrorURL title="VizieR at IUCAA: Pune, India">https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/AJ/152/176</mirrorURL><mirrorURL title="VizieR at SAAO: SAAO, South Africa">http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/AJ/152/176</mirrorURL></interface></capability><capability><interface xsi:type="vs:ParamHTTP"><accessURL use="base">https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/AJ/152/176</accessURL><mirrorURL title="VizieR at IUCAA: Pune, India">https://vizier.iucaa.in/viz-bin/votable?-source=J/AJ/152/176</mirrorURL><mirrorURL title="VizieR at SAAO: SAAO, South Africa">http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/AJ/152/176</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/AJ/152/176/table2 (Observation logs, 2013 and 2014)</description><interface xsi:type="vs:ParamHTTP" role="std"><accessURL use="base">https://vizier.cds.unistra.fr/viz-bin/conesearch/J/AJ/152/176/table2?</accessURL><mirrorURL title="VizieR at IUCAA: Pune, India">https://vizier.iucaa.in/viz-bin/conesearch/J/AJ/152/176/table2?</mirrorURL><mirrorURL title="VizieR at SAAO: SAAO, South Africa">http://vizieridia.saao.ac.za/viz-bin/conesearch/J/AJ/152/176/table2?</mirrorURL><queryType>GET</queryType><resultType>text/xml+votable</resultType></interface><maxSR>180.0</maxSR><maxRecords>50000</maxRecords><verbosity>true</verbosity><testQuery><ra>197.80010417</ra><dec>30.82718056</dec><sr>0.005555555555555556</sr></testQuery></capability><coverage><spatial>6/10394 10395 10416</spatial><spectral>3.322582951404819e-19 3.852589004194616e-19</spectral><footprint ivo-id="ivo://ivoa.net/std/moc">https://cdsarc.cds.unistra.fr/viz-bin/moc/J/AJ/152/176?format=ascii</footprint></coverage><tableset><schema><name>default</name><table><name>J/AJ/152/176/table2</name><description>Observation logs, 2013 and 2014</description><column><name>recno</name><description>Record number assigned by the VizieR team. 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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>[X/Fe]</name><description>Species</description><ucd>phys.abund</ucd><dataType xsi:type="vs:VOTableType" arraysize="10*">char</dataType></column><column><name>W11449</name><description>Abundance for the star W11449</description><unit>log(Sun)</unit><ucd>phys.abund</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>e_W11449</name><description>Error in W11449</description><unit>log(Sun)</unit><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>o_W11449</name><description>Number of absorption lines used for W11449 abundance analysis</description><ucd>meta.number</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>W11450</name><description>Abundance for the star W11450</description><unit>log(Sun)</unit><ucd>phys.abund</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>e_W11450</name><description>Error in W11450</description><unit>log(Sun)</unit><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>o_W11450</name><description>Number of absorption lines used for W11450 abundance analysis</description><ucd>meta.number</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>W12388</name><description>Abundance for the star W12388</description><unit>log(Sun)</unit><ucd>phys.abund</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>e_W12388</name><description>Error in W12388</description><unit>log(Sun)</unit><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>o_W12388</name><description>Number of absorption lines used for W12388 abundance analysis</description><ucd>meta.number</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>W13284</name><description>Abundance for the star W13284</description><unit>log(Sun)</unit><ucd>phys.abund</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>e_W13284</name><description>Error in W13284</description><unit>log(Sun)</unit><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>o_W13284</name><description>Number of absorption lines used for W13284 abundance analysis</description><ucd>meta.number</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>W21415</name><description>Abundance for the star W21415</description><unit>log(Sun)</unit><ucd>phys.abund</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>e_W21415</name><description>Error in W21415</description><unit>log(Sun)</unit><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>o_W21415</name><description>Number of absorption lines used for W21415 abundance analysis</description><ucd>meta.number</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>W23375</name><description>? 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