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<ri:Resource created="2019-08-14T06:55:52Z" status="active" updated="2025-05-19T09:50:00Z" version="1.2" 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/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>Radial velocity time series of EK Eridani</title><shortName>J/A+A/628/A106</shortName><identifier>ivo://CDS.VizieR/J/A+A/628/A106</identifier><altIdentifier>doi:10.26093/cds/vizier.36280106</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Bonanno A.</name></creator><creator><name>Corsaro E.</name></creator><creator><name>Del Sordo F.</name></creator><creator><name>Palle P.L.</name></creator><creator><name>Stello D.</name></creator><creator><name>Hon M.</name></creator><date role="Updated">2019-11-22T14:36:17Z</date><date role="Created">2019-08-14T06:55:52Z</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>giant-stars</subject><subject>variable-stars</subject><subject>radial-velocity</subject><subject>magnetic-fields</subject><description>We present further evidence of acoustic oscillations in the slowly rotating overactive G8 sub-giant EK Eri. This star was observed with the 1m Hertzsprung SONG telescope at the Observatorio del Teide for two different runs of 8 and 13 nights, respectively, that were separated by about a year. We determined a significant excess of power around {nu}_max_=253+/-3uHz in the first observing run and were able to determine a large separation, {Delta}_{nu}_=16.430+/-22uHz. No significant excess of power was instead detected in a subsequent SONG observing season, as also supported by our analysis of the simultaneous TESS photometric observations. We propose a new amplitude-luminosity relation in order to account for the missing power in the power spectrum. Based on the evolutionary stage of this object, we argue that a standard {alpha}^2^{OMEGA} dynamo cannot be excluded as the possible origin for the observed magnetic field.</description><source format="bibcode">2019A&amp;A...628A.106B</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/628/A106</referenceURL><type>Catalog</type><contentLevel>Research</contentLevel><relationship><relationshipType>IsServedBy</relationshipType><relatedResource ivo-id="ivo://CDS.VizieR/TAP">TAP VizieR generic 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/A+A/628/A106</accessURL><mirrorURL title="VizieR at IUCAA: Pune, India">https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/628/A106</mirrorURL><mirrorURL title="VizieR at SAAO: SAAO, South Africa">http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/628/A106</mirrorURL></interface></capability><capability><interface xsi:type="vs:ParamHTTP"><accessURL use="base">https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/628/A106</accessURL><mirrorURL title="VizieR at IUCAA: Pune, India">https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/628/A106</mirrorURL><mirrorURL title="VizieR at SAAO: SAAO, South Africa">http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/628/A106</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><coverage><footprint ivo-id="ivo://ivoa.net/std/moc"/></coverage><tableset><schema><name>default</name><table><name>J/A+A/628/A106/table1</name><description>Radial velocities of EK Eridani for 2017</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>BJD</name><description>Barycentric Julian Date</description><unit>d</unit><ucd>time.epoch</ucd><dataType xsi:type="vs:VOTableType">double</dataType></column><column><name>BRV</name><description>Barycentric corrected radial velocity (1)</description><unit>m/s</unit><ucd>phys.veloc;pos.barycenter</ucd><dataType xsi:type="vs:VOTableType">double</dataType></column><column><name>e_BRV</name><description>Uncertainty on RV (2)</description><unit>m/s</unit><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">double</dataType></column></table><table><name>J/A+A/628/A106/table2</name><description>Radial velocities of EK Eridani for 2018</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>BJD</name><description>Barycentric Julian Date</description><unit>d</unit><ucd>time.epoch</ucd><dataType xsi:type="vs:VOTableType">double</dataType></column><column><name>BRV</name><description>Barycentric corrected radial velocity (1)</description><unit>m/s</unit><ucd>phys.veloc;pos.barycenter</ucd><dataType xsi:type="vs:VOTableType">double</dataType></column><column><name>e_BRV</name><description>Uncertainty on RV (2)</description><unit>m/s</unit><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">double</dataType></column></table></schema></tableset></ri:Resource>