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<ri:Resource created="2024-01-12T06:38:56Z" status="active" updated="2026-08-27T08:07:52Z" 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>THYME. IX. MELANGE-4 association members</title><shortName>J/AJ/165/85</shortName><identifier>ivo://CDS.VizieR/J/AJ/165/85</identifier><altIdentifier>doi:10.26093/cds/vizier/be-55-2n</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Wood M.L.</name></creator><creator><name>Mann A.W.</name></creator><creator><name>Barber M.G.</name></creator><creator><name>Bush J.L.</name></creator><creator><name>Kraus A.L.</name></creator><creator><name>Tofflemire B.M.,Vanderburg A.</name></creator><creator><name>Newton E.R.</name></creator><creator><name>Feiden G.A.</name></creator><creator><name>Zhou G.</name></creator><creator><name>Bouma L.G.</name></creator><creator><name>Quinn S.N.,Armstrong D.J.</name></creator><creator><name>Osborn A.</name></creator><creator><name>Adibekyan V.</name></creator><creator><name>Mena E.D.</name></creator><creator><name>Sousa S.G.</name></creator><creator><name>Gagne J.,Fields M.J.</name></creator><creator><name>Milburn R.P.</name></creator><creator><name>Thao Pa C.</name></creator><creator><name>Schmidt S.P.</name></creator><creator><name>Gnilka C.L.,Howell S.B.</name></creator><creator><name>Law N.M.</name></creator><creator><name>Ziegler C.</name></creator><creator><name>Briceno C.</name></creator><creator><name>Ricker G.R.</name></creator><creator><name>Vanderspek R.,Latham D.W.</name></creator><creator><name>Seager S.</name></creator><creator><name>Winn J.N.</name></creator><creator><name>Jenkins J.M.</name></creator><creator><name>Schlieder J.E.,Osborn H.P.</name></creator><creator><name>Twicken J.D.</name></creator><creator><name>Ciardi D.R.</name></creator><creator><name>Huang C.X.</name></creator><date role="Updated">2026-08-27T08:07:52Z</date><date role="Created">2024-01-12T06:38:56Z</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>stellar-associations</subject><subject>visible-astronomy</subject><subject>spectroscopy</subject><subject>radial-velocity</subject><description>We report the discovery and characterization of a nearby (~85pc), older (27{+/-}3Myr), distributed stellar population near Lower Centaurus Crux (LCC), initially identified by searching for stars comoving with a candidate transiting planet from TESS (HD109833; TOI1097). We determine the association membership using Gaia kinematics, color-magnitude information, and rotation periods of candidate members. We measure its age using isochrones, gyrochronology, and Li depletion. While the association is near known populations of LCC, we find that it is older than any previously found LCC subgroup (10-16Myr), and distinct in both position and velocity. In addition to the candidate planets around HD109833, the association contains four directly imaged planetary-mass companions around three stars, YSES-1, YSES-2, and HD95086, all of which were previously assigned membership in the younger LCC. Using the Notch pipeline, we identify a second candidate transiting planet around HD109833. We use a suite of ground-based follow-up observations to validate the two transit signals as planetary in nature. HD109833 b and c join the small but growing population of &lt;100Myr transiting planets from TESS. HD109833 has a rotation period and Li abundance indicative of a young age (&lt;~100Myr), but a position and velocity on the outskirts of the new population, lower Li levels than similar members, and a color-magnitude diagram position below model predictions for 27Myr. So, we cannot reject the possibility that HD109833 is a young field star coincidentally nearby the population.</description><source format="bibcode">2023AJ....165...85W</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/AJ/165/85</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/259">I/259 : The Tycho-2 Catalogue (Hog+ 2000)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/I/337">I/337 : Gaia DR1 (Gaia Collaboration, 2016)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/VII/233">VII/233 : The 2MASS Extended sources (IPAC/UMass, 2003-2006)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/117/354">J/AJ/117/354 : OB associations from Hipparcos (de Zeeuw+, 1999)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/381/446">J/A+A/381/446 : Astrometric Radial Velocities. 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