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<ri:Resource created="2023-08-09T09:35:21Z" 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>Rotation periods and catalogue information</title><shortName>J/A+A/676/A55</shortName><identifier>ivo://CDS.VizieR/J/A+A/676/A55</identifier><altIdentifier>doi:10.26093/cds/vizier.36760055</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Labadie-Bartz J.</name></creator><creator><name>Huemmerich S.</name></creator><creator><name>Bernhard K.</name></creator><creator><name>Paunzen E.</name></creator><creator><name>Shultz M.E.</name></creator><date role="Updated">2024-11-06T20:05:31Z</date><date role="Created">2023-08-09T09:35:21Z</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>eclipsing-binary-stars</subject><subject>ap-stars</subject><subject>chemically-peculiar-stars</subject><subject>variable-stars</subject><description>We analysed space photometry from the TESS mission for a sample of 1002 mCP stars discovered in LAMOST archival spectra. Of the 782 mCP stars with available TESS data, rotation periods were measured for 720 of these. The sample includes 25 stars with additional photometric variability, and 4 eclipsing binaries. With our work, we increase the sample size of mCP stars with known rotation periods and identify prime candidates for detailed follow-up studies. 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Should Not be used for identification.</description><ucd>meta.record</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>TIC</name><description>TESS Input Catalog identifier</description><ucd>meta.id</ucd></column><column><name>LAMOST</name><description>LAMOST identifier (JHHMMSS.ss+DDMMSS.s)</description><ucd>meta.id;meta.main</ucd><dataType xsi:type="vs:VOTableType" arraysize="19*">char</dataType></column><column><name>RAJ2000</name><description>Right Ascension (J2000)</description><ucd>pos.eq.ra;meta.main</ucd></column><column><name>DEJ2000</name><description>Declination (J2000)</description><ucd>pos.eq.dec;meta.main</ucd></column><column><name>Gmag</name><description>Gaia magnitude</description><unit>mag</unit><ucd>phot.mag;em.opt</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>SpType</name><description>Spectral type (1)</description><ucd>src.spType</ucd><dataType xsi:type="vs:VOTableType" arraysize="30*">char</dataType></column><column><name>l_Per</name><description>Limit flag on Per</description><ucd>meta.code.error</ucd><dataType xsi:type="vs:VOTableType" arraysize="1*">char</dataType></column><column><name>Per</name><description>? 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