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<ri:Resource created="2020-08-25T08:36:59Z" 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>Cepheids flux weighted gravity-luminosity</title><shortName>J/A+A/640/A113</shortName><identifier>ivo://CDS.VizieR/J/A+A/640/A113</identifier><altIdentifier>doi:10.26093/cds/vizier.36400113</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Groenewegen M.A.T</name></creator><date role="Updated">2021-09-07T13:39:40Z</date><date role="Created">2020-08-25T08:36:59Z</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>stellar-distance</subject><description>The flux-weighted gravity-luminosity relation (FWGLR) is investigated for a sample of 477 classical Cepheids (CCs), including stars that have been classified in the literature as such but are probably not. The luminosities are taken from the literature, based on the fitting of the spectral energy distributions (SEDs) assuming a certain distance and reddening. The flux-weighted gravity (FWG) is taken from gravity and effective temperature determinations in the literature based on high-resolution spectroscopy. There is a very good agreement between the theoretically predicted and observed FWG versus pulsation period relation that could serve in estimating the FWG (and logg) in spectroscopic studies with a precision of 0.1dex. As was known in the literature, the theoretically predicted FWGLR relation for CCs is very tight and not very sensitive to metallicity (at least for LMC and Solar values), rotation rate and crossing of the instability strip. The observed relation has a slightly different slope and shows more scatter (0.54dex). This is due both to uncertainties in the distances and the pulsation phase averaged FWG values. Data from future Gaia data releases should reduce these errors, and then the FWGLR could serve as a powerful tool in Cepheid studies.</description><source format="bibcode">2020A&amp;A...640A.113G</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/640/A113</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/635/A33">J/A+A/635/A33 : Galactic classical Cepheids Per-Lbol-Rad (Groenewegen, 2020)</relatedResource></relationship></content><rights>https://cds.unistra.fr/vizier-org/licences_vizier.html</rights><capability><interface 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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>Name</name><description>The variable star name</description><ucd>meta.id;meta.main</ucd><dataType xsi:type="vs:VOTableType" arraysize="14*">char</dataType></column><column><name>Type</name><description>The classification of the variability (1)</description><ucd>meta.code.class;src.var</ucd><dataType xsi:type="vs:VOTableType" arraysize="8*">char</dataType></column><column><name>Per</name><description>The pulsation period (1)</description><unit>d</unit><ucd>time.period</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>d</name><description>The distance (1)</description><unit>kpc</unit><ucd>pos.distance</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>e_d</name><description>The error in the distance (1)</description><unit>kpc</unit><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>Lum</name><description>The stellar luminosity (1)</description><unit>solLum</unit><ucd>phys.luminosity</ucd><dataType xsi:type="vs:VOTableType">double</dataType></column><column><name>e_Lum</name><description>The error in the stellar luminosity (1)</description><unit>solLum</unit><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>Nspec</name><description>Number of available stellar spectra</description><ucd>meta.number</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>FWG</name><description>The average of the available flux weighted gravity (FWG) values</description><ucd>phys.gravity</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>e_FWG</name><description>The error in the FWG values</description><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>DeltaFWG</name><description>The difference between largest and smallest FWG value</description><ucd>phys.gravity</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>Ref</name><description>References for logg and Teff values used to calculate the FWG (2)</description><ucd>meta.ref</ucd><dataType xsi:type="vs:VOTableType" arraysize="8*">char</dataType></column><column><name>PapI</name><description>Display Paper I data (Groenewegen, 2020, Cat. 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