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<ri:Resource created="2022-08-17T06:54:43Z" status="active" updated="2025-06-13T15:25:00Z" 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>Large-scale expansion of OB stars in Cygnus</title><shortName>J/MNRAS/515/687</shortName><identifier>ivo://CDS.VizieR/J/MNRAS/515/687</identifier><altIdentifier>doi:10.26093/cds/vizier.75150687</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Quintana A.L.</name></creator><creator><name>Wright N.J.</name></creator><date role="Updated">2024-08-22T20:16:14Z</date><date role="Created">2022-08-17T06:54:43Z</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>ob-stars</subject><subject>visible-astronomy</subject><subject>trigonometric-parallax</subject><subject>proper-motions</subject><subject>stellar-ages</subject><subject>stellar-distance</subject><description>The proper motions (PMs) of OB stars in Cygnus have recently been found to exhibit two large-scale kinematic patterns suggestive of expansion. We perform a 3D traceback on these OB stars, the newly identified OB associations and related open clusters in the region. We find that there are two groups of stars, associations and clusters and that they were each more compact in the past, reaching their closest approach 7.9^+3.0^_-1.8_ and 8.5^+0.8^_-2.8_Myr ago. We consider two main scenarios for the driver of these large-scale expansion patterns: feedback-driven expansion from a previous generation of massive stars, and expansion as a result of the turbulent velocity field in the primordial molecular cloud. While it is tempting to attribute such large-scale expansion patterns to feedback processes, we find that the observed kinematics are fully consistent with the turbulent origin, and therefore that the injection of further energy or momentum from feedback is not required. Similar conclusions may be drawn for other star forming regions with large-scale expansion patterns.</description><source format="bibcode">2022MNRAS.515..687Q</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/515/687</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/350">I/350 : Gaia EDR3 (Gaia Collaboration, 2020)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/811/85">J/ApJ/811/85 : RVs + V-band LCs of probable members of Cyg OB2 (Kiminki+, 2015)</relatedResource></relationship></content><rights>https://cds.unistra.fr/vizier-org/licences_vizier.html</rights><capability><interface xsi:type="vr:WebBrowser"><accessURL use="full">https://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/515/687</accessURL><mirrorURL title="VizieR at IUCAA: Pune, India">https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/515/687</mirrorURL><mirrorURL title="VizieR at SAAO: SAAO, South Africa">http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/515/687</mirrorURL></interface></capability><capability><interface xsi:type="vs:ParamHTTP"><accessURL use="base">https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/515/687</accessURL><mirrorURL title="VizieR at IUCAA: Pune, India">https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/515/687</mirrorURL><mirrorURL title="VizieR at SAAO: SAAO, South Africa">http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/515/687</mirrorURL><queryType>GET</queryType><resultType>text/xml+votable</resultType></interface></capability><capability standardID="ivo://ivoa.net/std/TAP#aux"><interface xsi:type="vs:ParamHTTP" role="std"><accessURL use="base">https://tapvizier.cds.unistra.fr/TAPVizieR/tap</accessURL></interface></capability><capability xsi:type="cs:ConeSearch" standardID="ivo://ivoa.net/std/ConeSearch"><description>Cone search capability for table J/MNRAS/515/687/asscyg2 (Position, proper motions and SED-fitted distance of the association members)</description><interface xsi:type="vs:ParamHTTP" role="std"><accessURL use="base">https://vizier.cds.unistra.fr/viz-bin/conesearch/J/MNRAS/515/687/asscyg2?</accessURL><mirrorURL title="VizieR at IUCAA: Pune, India">https://vizier.iucaa.in/viz-bin/conesearch/J/MNRAS/515/687/asscyg2?</mirrorURL><mirrorURL title="VizieR at SAAO: SAAO, South Africa">http://vizieridia.saao.ac.za/viz-bin/conesearch/J/MNRAS/515/687/asscyg2?</mirrorURL><queryType>GET</queryType><resultType>text/xml+votable</resultType></interface><maxSR>180.0</maxSR><maxRecords>50000</maxRecords><verbosity>true</verbosity><testQuery><ra>305.93594694</ra><dec>37.257825</dec><sr>0.005555555555555556</sr></testQuery></capability><coverage><spatial>5/3657 3660 6/14622 14627 14633 14636-14637 14644-14646 14653 14655 14670-14671 14689 14691-14694 14696 14698-14699 14741 14784-14785</spatial><footprint ivo-id="ivo://ivoa.net/std/moc">https://cdsarc.cds.unistra.fr/viz-bin/moc/J/MNRAS/515/687?format=ascii</footprint><waveband>Optical</waveband></coverage><tableset><schema><name>default</name><table><name>J/MNRAS/515/687/asscyg2</name><description>Position, proper motions and SED-fitted distance of the association members</description><column><name>recno</name><description>Record number assigned by the VizieR team. 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