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<ri:Resource created="1997-12-09T20:17:16Z" 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>JHK photometry of the OMC2 region</title><shortName>J/AJ/107/2120</shortName><identifier>ivo://CDS.VizieR/J/AJ/107/2120</identifier><altIdentifier>doi:10.26093/cds/vizier.51072120</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Jones T.J.</name></creator><creator><name>Mergen J.</name></creator><creator><name>Odewahn S.</name></creator><creator><name>Gehrz R.D.</name></creator><creator><name>Gatley I.,Merrill K.M.</name></creator><creator><name>Probst R.</name></creator><creator><name>Woodward C.E.</name></creator><date role="Updated">2023-04-06T16:50:07Z</date><date role="Created">1997-12-09T20:17:16Z</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>infrared-photometry</subject><description>We present an unbiased survey at 1.25-2.2um of a 0.025sq.deg. region surrounding the core of Orion Molecular Cloud 2 (OMC-2). Analysis of the source counts and colors indicates that the majority of the sources brighter than K=+13 are not field stars. They must be members of a young association or associations within the survey area. The K band luminosity function (corrected for field star contamination using model calculations) exhibits a drop in counts at magnitudes fainter than K=+13 (~0.15L_{sun}_). This is most easily explained by assuming that the association(s) are young. The lowest mass stars simply have not yet reached the main sequence. The distribution of colors across the region shows moderate correlation with molecular gas, but both reddened and unreddened stars are present along most lines of sight. Considerable reflection nebulosity is present in the region of the core cluster of OMC2 itself. 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