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<ri:Resource created="2023-04-04T07:54:56Z" 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>Galactic Cepheid luminosity scale</title><shortName>J/A+A/672/A85</shortName><identifier>ivo://CDS.VizieR/J/A+A/672/A85</identifier><altIdentifier>doi:10.26093/cds/vizier.36720085</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Cruz Reyes M.</name></creator><creator><name>Anderson R.I.</name></creator><date role="Updated">2024-11-28T20:03:07Z</date><date role="Created">2023-04-04T07:54:56Z</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>variable-stars</subject><subject>radial-velocity</subject><subject>visible-astronomy</subject><subject>trigonometric-parallax</subject><description>We have conducted a search for open clusters in the vicinity of Galactic classical Cepheids based on high-quality astrometry from the ESA mission Gaia's third data release (DR3) to improve the calibration of the Leavitt law. Our approach requires no prior knowledge of existing clusters, allowing us to both detect new host clusters and cross-check previously reported associations. Our Gold sample consists of 34 Cepheids residing in 28 open clusters, including 27 fundamental mode and 7 overtone Cepheids. Three new bona fide cluster Cepheids are reported (V0378 Cen, ST Tau and GH Lup) and the host cluster identifications for three others (VW Cru, IQ Nor, SX Vel) is corrected. The fraction of Cepheids occurring in open clusters within 2 kpc of the Sun is f_CC,2kpc_=0.092+/-0.009. Non-variable cluster members allow us to determine cluster parallaxes to 7 as in the range 12.5&lt;G&lt;17mag where recent studies found that parallax corrections by Lindegren et al. (2021A&amp;A...649A...4L) are accurate and require no further offset corrections. Comparing MW cluster Cepheids to Cepheids in the LMC, we confirm these independent results and the adequacy of the L21 corrections for the cluster members in this range. Combining cluster and field Cepheids, we calibrate the Galactic Cepheid Leavitt law for a variety of individual optical and near-infrared passbands, as well as using reddening-free Wesenheit magnitudes based on Gaia and HST photometry, while solving for the residual offset applicable to Cepheid parallaxes, {Delta}{varpi}_Cep_. The most direct comparison of our results with the SH0ES distance ladder yields excellent (0.3{sigma}) agreement for both the absolute magnitude of a 10d Solar metallicity Cepheid in the _IR HST Wesenheit magnitudes, M^W^_H_=-5.915+/-0.017mag, and the residual parallax offset, {varpi}_Cl_=-13+/-5uas. Despite the use of a common set of photometry, this is an important cross-check of the recent Hubble constant measurement by Riess et al. based on independently determined cluster membership and average parallaxes. Allowing the LL slope to vary yields results consistent to within 1 and a slightly larger residual parallax offsets {Delta}{varpi}_Cep_=-17+/-5uas. Using the larger sample of 26 Gold cluster Cepheids and 225 MW Cepheids with recent Gaia DR3 astrometry and photometry, we determine the absolute magnitude of a 10d fundamental mode Cepheid in the optical Gaia Wesenheit magnitude at the sample average iron abundance of &lt;[Fe=H]&gt;=0.069, M^W^_G_=-6.051+/-0.020mag, and {Delta}{varpi}_Cep_=-22+/-3uas. Correcting to Solar metallicity yields M^W^_G_=-5.996+/-0.019mag and {Delta}{varpi}_Cep_=-19+/-3uas. These results mark the currently most accurate absolute calibrations of the Cepheid luminosity scale based purely on observations of MW Cepheids, as well as the most precise determination of the residual Cepheid parallax offset at a significance of 6-7{sigma}.</description><source format="bibcode">2023A&amp;A...672A..85C</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/672/A85</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/I/355">I/355 : Gaia DR3 Part 1. 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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>Cepheid</name><description>Cepheid name</description><ucd>meta.id;meta.main</ucd><dataType xsi:type="vs:VOTableType" arraysize="9*">char</dataType></column><column><name>Per</name><description>Cepheid pulsation period</description><unit>d</unit><ucd>time.period</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>plx</name><description>Host cluster parallax</description><unit>uarcsec</unit><ucd>pos.parallax.trig</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>sigmastat</name><description>Statistical uncertainty in cluster parallax</description><unit>uarcsec</unit><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>sigmacov</name><description>Angular covariance in cluster parallax</description><unit>uarcsec</unit><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>sigmatot</name><description>Sum in quadrature of sigma_stat and sigma_cov</description><unit>uarcsec</unit><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>WG</name><description>? Wesenheit WG magnitude, WD=G-1.921(Bp-Rp)</description><unit>mag</unit><ucd>phot.mag</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>e_[Fe/H]</name><description>? Uncertainty in iron abundance</description><ucd>stat.error;phys.abund.Fe</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>r_[Fe/H]</name><description>Reference of the iron abundance (1)</description><ucd>meta.ref</ucd><dataType xsi:type="vs:VOTableType" arraysize="4*">char</dataType></column><column><name>E(B-V)</name><description>? Color excess value</description><unit>mag</unit><ucd>phot.color.excess</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>e_E(B-V)</name><description>? Uncertainty in the color excess</description><unit>mag</unit><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>_RA</name><description>Right Ascension (J2000) from SIMBAD (not part of the original data)</description><unit>deg</unit><ucd>pos.eq.ra;meta.main</ucd></column><column><name>_DE</name><description>Declination (J2000) from SIMBAD (not part of the original data)</description><unit>deg</unit><ucd>pos.eq.dec;meta.main</ucd></column></table><table><name>J/A+A/672/A85/tablea1</name><description>Cluster members of the Gold, Silver and Bronze</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>Cluster</name><description>Cluster name</description><ucd>meta.id.parent</ucd><dataType xsi:type="vs:VOTableType" arraysize="17*">char</dataType></column><column><name>GaiaDR3</name><description>Gaia EDR3 source id</description><ucd>meta.id;meta.main</ucd></column><column><name>plx</name><description>Gaia EDR3 parallax</description><unit>mas</unit><ucd>pos.parallax.trig</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>Corr</name><description>Lindegren et al. (2021A&amp;A...649A...4L) parallax offset correction</description><unit>mas</unit><ucd>arith.factor</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column></table></schema></tableset></ri:Resource>