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<ri:Resource created="2013-04-23T10:25:15Z" 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>Candidate Be stars in the Magellanic Clouds</title><shortName>J/MNRAS/421/3622</shortName><identifier>ivo://CDS.VizieR/J/MNRAS/421/3622</identifier><altIdentifier>doi:10.26093/cds/vizier.74213622</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Paul K.T.</name></creator><creator><name>Subramaniam A.</name></creator><creator><name>Mathew B.</name></creator><creator><name>Mennickent R.E.</name></creator><creator><name>Sabogal B.</name></creator><date role="Updated">2024-07-17T20:15:28Z</date><date role="Created">2013-04-23T10:25:15Z</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>be-stars</subject><subject>line-intensities</subject><description>Mennickent et al. (2002A&amp;A...393..887M) and Sabogal et al. (2005, Cat. J/MNRAS/361/1055) identified a large number of classical Be (CBe) candidates (~3500) in the Large and Small Magellanic Clouds (LMC and SMC) based on their photometric variability using the OGLE II data base (Udalski et al., 1998, Cat. J/AcA/48/147; 2000, Cat. J/AcA/50/307). They classified these stars into four different groups based on the appearance of their variability. In order to refine and understand the nature of this large number of stars, we studied the infrared properties of the sample and the spectroscopic properties of a subsample. We cross-correlated the optical sample with the IRSF-MCPS catalogue to obtain the J, H, Ks magnitudes of all the four types of stars (~2500) in the LMC and SMC. Spectra of 120 stars belonging to the types 1, 2 and 3 were analysed to study their spectral properties.</description><source format="bibcode">2012MNRAS.421.3622P</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/421/3622</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/II/288">II/288 : IRSF Magellanic Clouds Point Source Catalog (Kato+ 2007)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AcA/48/147">J/AcA/48/147 : OGLE SMC BVI photometry (Udalski+ 1998)</relatedResource><relatedResource 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Dereddened B-V colour index</description><unit>mag</unit><ucd>phot.color;em.opt.B;em.opt.V</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>V0mag</name><description>? Dereddened V magnitude</description><unit>mag</unit><ucd>phot.mag.reddFree;em.opt.V</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>(H-K)0</name><description>? Dereddened H-K colour index</description><unit>mag</unit><ucd>phot.color;em.IR.H;em.IR.K</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>(J-H)0</name><description>? 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