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<ri:Resource created="2021-03-24T10:12:36Z" 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>PA &amp; angular separation measurements of 80 Tau</title><shortName>J/ApJ/883/105</shortName><identifier>ivo://CDS.VizieR/J/ApJ/883/105</identifier><altIdentifier>doi:10.26093/cds/vizier.18830105</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Torres G.</name></creator><date role="Updated">2021-05-03T09:00:00Z</date><date role="Created">2021-03-24T10:12:36Z</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>multiple-stars</subject><description>The empirical mass-luminosity relation in the Hyades cluster rests on dynamical mass determinations for five binary systems, of which one is eclipsing and the other four are visual or interferometric binaries. The last one was identified and first measured more than 20yr ago. Here we present dynamical mass measurements for a new binary system in the cluster, 80 Tau, which is also a visual pair with a much longer orbital period of about 170yr. Although we lack the radial-velocity information that has enabled the individual mass determinations in all of the previous binaries, we show that it is still possible to derive the component masses for 80 Tau using only astrometric observations. This is enabled by the accurate proper motion measurements from the Hipparcos and Gaia missions, which constrain the orbital acceleration in the plane of the sky. Separate proper motion values from Gaia for the primary and secondary provide a direct constraint on the mass ratio. Our mass measurements, M_A_=1.63_-0.13_^+0.30^M_{sun}_ and M_B_=1.11_-0.14_^+0.21^M_{sun}_, are consistent with the mass-luminosity relation defined by the five previously known systems, which in turn is in good agreement with current models of stellar evolution.</description><source format="bibcode">2019ApJ...883..105T</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/883/105</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/B/wds">B/wds : The Washington Visual Double Star Catalog (Mason+ 2001-2020)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/I/259">I/259 : The Tycho-2 Catalogue (Hog+ 2000)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/I/345">I/345 : Gaia DR2 (Gaia Collaboration, 2018)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+AS/101/551">J/A+AS/101/551 : Optical polarization of 1000 stars (Leroy 1993)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/331/81">J/A+A/331/81 : Hyades membership (Perryman+ 1998)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/341/121">J/A+A/341/121 : Visual binary orbits and masses (Soederhjelm 1999)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/120/2638">J/AJ/120/2638 : CCD speckle obs. of binary stars. 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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>Year</name><description>[1831.18/2015.846] Year of observation in Julian years</description><unit>yr</unit><ucd>time.epoch</ucd><dataType xsi:type="vs:VOTableType">double</dataType></column><column><name>PA</name><description>[1.7/78.2]? Position angle {theta} (1)</description><unit>deg</unit><ucd>pos.posAng</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>e_PA</name><description>[0.012/0.15]? Position angle uncertainty along tangential direction {sigma}_t_ (2)</description><unit>arcsec</unit><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>(O-C)t</name><description>[-8.4/22.2]? Position angle (O-C)_{theta}_ value</description><unit>deg</unit><ucd>pos.posAng</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>(O-C)t/sig</name><description>[-2.7/3.1]? Position angle (O-C)_{theta}_ value divided by uncertainty in theta {sigma}_{theta}_</description><ucd>stat.error;pos.posAng</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>rho</name><description>[0.4/1.9]? Angular separation {rho}</description><unit>arcsec</unit><ucd>pos.angDistance</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>e_rho</name><description>[0.012/0.2]? Uncertainty in rho {sigma}_{rho}_ (2)</description><unit>arcsec</unit><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>(O-C)rho</name><description>[-0.4/0.4]? Angular separation (O-C)_{rho}_ value</description><unit>arcsec</unit><ucd>pos.angDistance</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>(O-C)rho/sig</name><description>[-2.2/2.7]? Angular separation (O-C)_{rho}_ divided by uncertainty in rho {sigma}_{rho}_</description><ucd>stat.error;pos.angDistance</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column></table></schema></tableset></ri:Resource>