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<ri:Resource created="2015-06-12T09:04:35Z" 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>Spectra of 12 ON stars</title><shortName>J/A+A/578/A109</shortName><identifier>ivo://CDS.VizieR/J/A+A/578/A109</identifier><altIdentifier>doi:10.26093/cds/vizier.35780109</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Martins F.</name></creator><creator><name>Simon-Diaz S.</name></creator><creator><name>Palacios A.</name></creator><creator><name>Howarth I.</name></creator><creator><name>Georgy C.</name></creator><creator><name>Walborn N.,Bouret J.-C.</name></creator><creator><name>Barba R.</name></creator><date role="Updated">2017-09-27T05:55:39Z</date><date role="Created">2015-06-12T09:04:35Z</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>o-stars</subject><subject>multiple-stars</subject><subject>spectroscopy</subject><description>Massive stars burn hydrogen through the CNO cycle during most of their evolution. When mixing is efficient or when mass transfer in binary systems occurs, chemically processed material is observed at the surface of O and B stars. ON stars show stronger lines of nitrogen than morphologically normal counterparts. Whether this corresponds to the presence of material processed through the CNO cycle is not known. Our goal is to answer this question. We performed a spectroscopic analysis of a sample of ON stars with atmosphere models. We determined the fundamental parameters as well as the He, C, N, and O surface abundances. We also measured the projected rotational velocities. 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