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<ri:Resource created="1998-06-05T15:01:07Z" 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>Upper Scorpius OB association Lithium survey</title><shortName>J/A+A/333/619</shortName><identifier>ivo://CDS.VizieR/J/A+A/333/619</identifier><altIdentifier>doi:10.26093/cds/vizier.33330619</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Preibisch T.</name></creator><creator><name>Guenther E.</name></creator><creator><name>Zinnecker H.</name></creator><creator><name>Sterzik M.</name></creator><creator><name>Frink S.</name></creator><creator><name>Roeser S.</name></creator><date role="Updated">1998-06-05T15:01:10Z</date><date role="Created">1998-06-05T15:01:07Z</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>pre-main-sequence-stars</subject><subject>line-intensities</subject><subject>proper-motions</subject><subject>stellar-associations</subject><description>We present the results of an intermediate resolution spectroscopic survey for pre-main sequence (PMS) stars in the Upper Scorpius OB association. In a 160 square-degree area we were able to identify 39 new PMS stars by follow up observations of X-ray selected stars with the multi object spectrograph FLAIR at the UK Schmidt Telescope. We also investigated the completeness of our X-ray selected sample by observing more than 100 stars that were not detected as X-ray sources, but have proper motions indicating membership to Upper Sco. While the new X-ray selected PMS stars with known proper motions have kinematics consistent with membership, none of the X-ray quiet proper motion candidates is a PMS star. We conclude that our X-ray selected sample of PMS stars seems to be rather complete. 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