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<ri:Resource created="2010-03-01T22:31:38Z" 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>Be/X-ray binaries in Small Magellanic Cloud</title><shortName>J/MNRAS/388/1198</shortName><identifier>ivo://CDS.VizieR/J/MNRAS/388/1198</identifier><altIdentifier>doi:10.26093/cds/vizier.73881198</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>McBride V.A.</name></creator><creator><name>Coe M.J.</name></creator><creator><name>Negueruela I.</name></creator><creator><name>Schurch M.P.E.</name></creator><creator><name>McGowan K.E.</name></creator><date role="Updated">2024-07-07T20:16:36Z</date><date role="Created">2010-03-01T22:31:38Z</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>magellanic-clouds</subject><subject>x-ray-binary-stars</subject><subject>photometry</subject><description>The spectral distributions of Be/X-ray binaries in the Large Magellanic Cloud and Galaxy have been shown to differ significantly from the distribution of isolated Be stars in the Galaxy. Population synthesis models can explain this difference in spectral distributions through substantial angular momentum loss from the binary system. In this work, we explore the spectral distribution of Be/X-ray binaries in the Small Magellanic Cloud (SMC) using high signal-to-noise ratio spectroscopy of a sample of 37 optical counterparts to known X-ray pulsars. Our results show that the spectral distribution of Be/X-ray binaries in the SMC is consistent with that of the Galaxy, despite the lower metallicity environment of the SMC. 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