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<ri:Resource created="2025-03-19T07:41:34Z" status="active" updated="2025-05-21T20:02:37Z" 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>RVs of binaries black hole/Sun-like stars</title><shortName>J/A+A/695/A210</shortName><identifier>ivo://CDS.VizieR/J/A+A/695/A210</identifier><altIdentifier>doi:10.26093/cds/vizier.36950210</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Green M.J.</name></creator><creator><name>Ziv Y.</name></creator><creator><name>Rix H.-W.</name></creator><creator><name>Maoz D.</name></creator><creator><name>Hamoudy I.</name></creator><creator><name>Mazeh T.</name></creator><creator><name>Faigler S.,Lam M.C.</name></creator><creator><name>El-Badry K.</name></creator><creator><name>Hume G.</name></creator><creator><name>Munday J.</name></creator><creator><name>Yarker P.</name></creator><date role="Updated">2025-05-21T20:02:37Z</date><date role="Created">2025-03-19T07:41:34Z</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><subject>g-stars</subject><subject>black-holes</subject><subject>orbits</subject><subject>radial-velocity</subject><description>Stellar-mass black holes descend from high-mass stars, most of which had stellar binary companions. However, the number of those binary systems that survive the binary evolution and black hole formation is uncertain by multiple orders of magnitude. The survival rate is particularly uncertain for massive stars with low-mass companions, which are thought to be the progenitors of most black hole X-ray binaries. We present a search for close black hole companions (orbital period &lt;~3 days, equivalent to separation &lt;~20R_{sun}_) to AFGK-type stars in TESS, i.e. the non-accreting counterparts to and progenitors of low-mass X-ray binaries. Such black holes can be detected by the tidally induced ellipsoidal deformation of the visible star, and the ensuing photometric light-curve variations. From an initial sample of 4.7x10^6^ TESS stars, we have selected 457 candidates for such variations. However, spectroscopic followup of 251 of them shows that none are consistent with a close black hole companion. On the basis of this non-detection, we determine (2{sigma} confidence) that fewer than one in 10^5^ Solar-type stars in the Solar neighbourhood host a short-period black hole companion. This upper limit is in tension with a number of "optimistic" population models in the literature that predict short-period black hole companions around one in ~10^4-5^ stars. Our limits are still consistent with other models that predict only a few in ~10^7-8^.</description><source format="bibcode">2025A&amp;A...695A.210G</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/695/A210</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/IV/39">IV/39 : TESS Input Catalog version 8.2 (TIC v8.2) (Paegert+, 2021)</relatedResource></relationship></content><rights>https://cds.unistra.fr/vizier-org/licences_vizier.html</rights><capability><interface xsi:type="vr:WebBrowser"><accessURL 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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>VC</name><description>Show the Radial Velocity curves</description><ucd>meta.ref.url</ucd><dataType xsi:type="vs:VOTableType" arraysize="*">char</dataType></column><column><name>TIC</name><description>ID number of the target in TESS input catalog</description><ucd>meta.id;meta.main</ucd><dataType xsi:type="vs:VOTableType">long</dataType></column><column><name>Tel</name><description>Telescope was used for the observations (1)</description><ucd>instr.setup</ucd><dataType xsi:type="vs:VOTableType" arraysize="8*">char</dataType></column><column><name>Nepochs</name><description>Number of epochs of observation</description><ucd>meta.number</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>Porb</name><description>? Orbital period</description><unit>d</unit><ucd>time.period</ucd><dataType xsi:type="vs:VOTableType">double</dataType><flag>nullable</flag></column><column><name>e_Porb</name><description>? Orbital period uncertainty</description><unit>d</unit><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">double</dataType><flag>nullable</flag></column><column><name>K</name><description>Orbital velocity semi-amplitude</description><unit>km/s</unit><ucd>phys.veloc.orbital</ucd><dataType xsi:type="vs:VOTableType">double</dataType></column><column><name>e_K</name><description>? Orbital velocity semi-amplitude uncertainty</description><unit>km/s</unit><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">double</dataType><flag>nullable</flag></column><column><name>MinM2</name><description>? Spectroscopic lower limit on companion mass</description><unit>solMass</unit><ucd>phys.mass</ucd><dataType xsi:type="vs:VOTableType">double</dataType><flag>nullable</flag></column><column><name>e_MinM2</name><description>? Spectroscopic lower limit on companion mass uncertainty</description><unit>solMass</unit><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">double</dataType><flag>nullable</flag></column><column><name>Minq</name><description>? Spectroscopic lower limit on mass ratio</description><ucd>phys.mass;arith.ratio</ucd><dataType xsi:type="vs:VOTableType">double</dataType><flag>nullable</flag></column><column><name>e_Minq</name><description>? Spectroscopic lower limit on mass ratio uncertainty</description><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">double</dataType><flag>nullable</flag></column><column><name>SB2?</name><description>[0/1] True if the target spectra showed two spectral components</description><ucd>meta.code</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>_RA</name><description>Positions from TIC (Cat. IV/39) (right ascension part)</description><unit>deg</unit><ucd>pos.eq.ra;meta.main</ucd></column><column><name>_DE</name><description>Positions from TIC (Cat. IV/39) (declination part)</description><unit>deg</unit><ucd>pos.eq.dec;meta.main</ucd></column></table><table><name>J/A+A/695/A210/table4</name><description>Radial velocities measured from individual exposures on the targets listed in Table 3</description><column><name>recno</name><description>Record number assigned by the VizieR team. 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