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<ri:Resource created="2001-05-04T22:13:47Z" 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>Orion Trapezium cluster</title><shortName>J/AJ/117/1375</shortName><identifier>ivo://CDS.VizieR/J/AJ/117/1375</identifier><altIdentifier>doi:10.26093/cds/vizier.51171375</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Simon M.</name></creator><creator><name>Close L.M.</name></creator><creator><name>Beck T.L.</name></creator><date role="Updated">2023-04-06T16:50:32Z</date><date role="Created">2001-05-04T22:13:47Z</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>multiple-stars</subject><subject>photometry</subject><description>We have imaged an area ~5arcmin^2^ at the center of the Trapezium cluster in Orion in the K band using the University of Hawaii (UH) adaptive optics system at the UH 2.2 m telescope. Our survey detects 292 stars brighter than K=18.2mag and resolves pairs to the 0.23" diffraction limit of the telescope. The binary fraction in the angular separation range 0.3"-0.6", corresponding to 132-264AU at 440pc, is indistinguishable from that of the solar-like stars in the solar neighborhood. Proplyds are associated with both single stars and visual binaries. About half the stars in our sample have also been measured at V and I by Prosser et al. (1994ApJ...421..517P); most of these seem to be about 10^6^yr old, observed through moderate extinction, and having some excess emission at K. 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