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<ri:Resource created="2004-07-21T15:18:05Z" 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>Infrared photometry in the Arches Cluster</title><shortName>J/ApJ/581/258</shortName><identifier>ivo://CDS.VizieR/J/ApJ/581/258</identifier><altIdentifier>doi:10.26093/cds/vizier.15810258</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Figer D.F.</name></creator><creator><name>Najarro F.</name></creator><creator><name>Gilmore D.</name></creator><creator><name>Morris M.</name></creator><creator><name>Kim S.S.</name></creator><creator><name>Serabyn E.,McLean I.S.</name></creator><creator><name>Gilbert A.M.</name></creator><creator><name>Graham J.R.</name></creator><creator><name>Larkin J.E.</name></creator><creator><name>Levenson N.A.,Teplitz H.I.</name></creator><date role="Updated">2004-07-21T15:19:34Z</date><date role="Created">2004-07-21T15:18:05Z</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>emission-line-stars</subject><subject>infrared-photometry</subject><description>We present and use new spectra and narrowband images, along with previously published broadband images, of stars in the Arches cluster to extract photometry, astrometry, equivalent width, and velocity information. The data are interpreted with a wind/atmosphere code to determine stellar temperatures, luminosities, mass-loss rates, and abundances. 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