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<ri:Resource created="2011-05-17T15:12:46Z" 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>HATNet Pleiades Rotation Period Catalogue</title><shortName>J/MNRAS/408/475</shortName><identifier>ivo://CDS.VizieR/J/MNRAS/408/475</identifier><altIdentifier>doi:10.26093/cds/vizier.74080475</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Hartman J.D.</name></creator><creator><name>Bakos G.A.</name></creator><creator><name>Kovacs G.</name></creator><creator><name>Noyes R.W.</name></creator><date role="Updated">2024-07-12T20:14:47Z</date><date role="Created">2011-05-17T15:12:46Z</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>open-star-clusters</subject><subject>variable-stars</subject><subject>visible-astronomy</subject><subject>broad-band-photometry</subject><subject>infrared-photometry</subject><description>Using data from the Hungarian-made Automated Telescope Network (HATNet) survey for transiting exoplanets, we measure photometric rotation periods for 368 Pleiades stars with 0.4~&lt;M~&lt;1.3M_{sun}_. We detect periodic variability for 74 per cent of the cluster members in this mass range that are within our field-of-view, and 93 per cent of the members with 0.7~&lt;M~&lt;1.0M_{sun}_. This increases, by a factor of 5, the number of Pleiades members with measured periods. We compare these data to the rich sample of spectroscopically determined projected equatorial rotation velocities (vsini) available in the literature for this cluster. 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