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<ri:Resource created="2017-06-12T08:54:10Z" 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>KIC 10670103 frequency spectrum</title><shortName>J/MNRAS/440/3809</shortName><identifier>ivo://CDS.VizieR/J/MNRAS/440/3809</identifier><altIdentifier>doi:10.26093/cds/vizier.74403809</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Reed M.D.</name></creator><creator><name>Foster H.</name></creator><creator><name>Telting J.H.</name></creator><creator><name>Ostensen R.H.</name></creator><creator><name>Farris L.H.</name></creator><creator><name>Oreiro R.,Baran A.S.</name></creator><date role="Updated">2024-08-09T20:14:38Z</date><date role="Created">2017-06-12T08:54:10Z</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>variable-stars</subject><subject>b-stars</subject><subject>spectroscopy</subject><description>We analyse 2.75yr of Kepler spacecraft observations of the pulsating subdwarf B star KIC 10670103. These 1.4 million measurements have an impressive duty cycle of 93.8 per cent, a frequency resolution of 0.017{mu}Hz, and a 5{sigma} detection limit of 0.1 parts-per-thousand (ppt). We detect 278 periodicities, making KIC 10670103 the richest pulsating subdwarf B star to date. Frequencies range from 23 to 673{mu}Hz (0.4 and 11.8h), with amplitudes from the detection limit up to 14 ppt. Follow-up spectroscopic data were obtained from which it was determined that KIC 10670103 does not show significant radial velocity variations. Updated atmospheric model fits determined T_eff_=21485+/-540K, logg=5.14+/-0.05, and logN(He)/N(H) =-2.60+/-0.04. We identify pulsation modes using asymptotic period spacings and frequency multiplets. The frequency multiplets indicate a spin period of 88+/-8d. Of the 278 periodicities detected in KIC 10670103, 163 (59 per cent) have been associated with low-degree (l&lt;=2) pulsation modes, providing tight constraints for model fitting. While the data are exquisite, amplitudes (and some frequencies) are not stable over the course of the observations, requiring tools which are non-standard for compact pulsators such as sliding Fourier transforms and Lorentzian fitting. Using the 163 identified pulsation modes, it is possible to make detailed examinations of the pulsation structure; including where the pulsation power is concentrated in radial order, over what frequency range mode trapping is inefficient, and how power switches between multiplet members.</description><source format="bibcode">2014MNRAS.440.3809R</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/440/3809</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>related-to</relationshipType><relatedResource ivo-id="ivo://CDS.VizieR/V/133">V/133 : Kepler Input Catalog (Kepler Mission Team, 2009)</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/440/3809</accessURL><mirrorURL title="VizieR at IUCAA: Pune, India">https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/440/3809</mirrorURL><mirrorURL title="VizieR at SAAO: SAAO, South Africa">http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/440/3809</mirrorURL></interface></capability><capability><interface xsi:type="vs:ParamHTTP"><accessURL use="base">https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/440/3809</accessURL><mirrorURL title="VizieR at IUCAA: Pune, India">https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/440/3809</mirrorURL><mirrorURL title="VizieR at SAAO: SAAO, South Africa">http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/440/3809</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"/><waveband>Optical</waveband></coverage><tableset><schema><name>default</name><table><name>J/MNRAS/440/3809/table1</name><description>The frequency list as a result of Lorentzian fitting</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>ID</name><description>Frequency identification</description><ucd>meta.id;em.freq</ucd><dataType xsi:type="vs:VOTableType" arraysize="4*">char</dataType></column><column><name>n_ID</name><description>[abd] Note on ID (1)</description><ucd>meta.note</ucd><dataType xsi:type="vs:VOTableType" arraysize="1*">char</dataType></column><column><name>Freq</name><description>Frequency</description><unit>uHz</unit><ucd>em.freq</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>e_Freq</name><description>rms uncertainty on Freq (2)</description><unit>uHz</unit><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>Per</name><description>Period</description><unit>s</unit><ucd>time.period</ucd><dataType xsi:type="vs:VOTableType">double</dataType></column><column><name>e_Per</name><description>rms uncertainty on Per (2)</description><unit>s</unit><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>Amp</name><description>Amplitude (in ppt = parts-per-thousand)</description><ucd>src.var.amplitude</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>l</name><description>Best estimate of the mode degree l</description><ucd>stat.param</ucd><dataType xsi:type="vs:VOTableType" arraysize="6*">char</dataType></column><column><name>m</name><description>Azimuthal order m</description><ucd>stat.param</ucd><dataType xsi:type="vs:VOTableType" arraysize="7*">char</dataType></column><column><name>n1</name><description>? radial overtone n1 fit to {Pi}_l,n_={Pi}_l,n=0_+n.{Delta}{pi}_l_ (3)</description><ucd>stat.param</ucd><dataType xsi:type="vs:VOTableType">int</dataType><flag>nullable</flag></column><column><name>n2</name><description>? radial overtone n2 fit to {Pi}_l,n_={Pi}_l,n=0_+n.{Delta}{pi}_l_ (3)</description><ucd>stat.param</ucd><dataType xsi:type="vs:VOTableType">int</dataType><flag>nullable</flag></column><column><name>dP/DPi1</name><description>? 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