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<ri:Resource created="2019-04-23T08:59:24Z" 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>Coma Berenices neighbor moving group</title><shortName>J/A+A/624/L11</shortName><identifier>ivo://CDS.VizieR/J/A+A/624/L11</identifier><altIdentifier>doi:10.26093/cds/vizier.36249011</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Fuernkranz V.</name></creator><creator><name>Meingast S.</name></creator><creator><name>Alves J.</name></creator><date role="Updated">2020-02-21T09:00:44Z</date><date role="Created">2019-04-23T08:59:24Z</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>astrometry</subject><description>We report the discovery of a kinematically cold group of stars, located in the immediate neighborhood of the well-known star cluster Coma Berenices (Mel 111). The new group identified in tangential velocity space as measured by Gaia contains at least 177 coeval members distributed in two subgroups, and appears as a flattened structure parallel to the plane, stretching for about 50pc. More remarkably, the new group, which appears to have formed about 300Myr later than Mel 111 in a different part of the Galaxy, will share essentially the same volume with the older cluster when the centers of both groups will be at their closest in 13 Myr. This will result in the mixing of two unrelated populations with different metallicities. The phase of cohabitation for these two groups is about 20-30Myr, after which the two populations will drift apart. We estimate that temporal cohabitation of such populations is not a rare event in the disk of the Milky Way, and of the order of once per Galactic revolution. Our study also unveils the tidal tails of the Mel 111 cluster.</description><source format="bibcode">2019A&amp;A...624L..11F</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/624/L11</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/345">I/345 : Gaia DR2 (Gaia Collaboration, 2018)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/621/L3">J/A+A/621/L3 : Hyades tidal tails with Gaia DR2 (Meingast+, 2019)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/622/L13">J/A+A/622/L13 : Stellar stream in Gaia DR2 discovery 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