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<ri:Resource created="2023-01-03T15:18:33Z" 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>Havlen-Moffat No. 1 UBVRI photometry</title><shortName>J/A+A/371/908</shortName><identifier>ivo://CDS.VizieR/J/A+A/371/908</identifier><altIdentifier>doi:10.26093/cds/vizier.33710908</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Vazquez R.A.</name></creator><creator><name>Baume G.</name></creator><date role="Updated">2023-01-03T14:18:49Z</date><date role="Created">2023-01-03T15:18:33Z</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>infrared-photometry</subject><subject>visible-astronomy</subject><subject>broad-band-photometry</subject><subject>morgan-keenan-classification</subject><description>A deep CCD UBVRI photometric survey combined with UBVRI polarimetric observations of 21 bright stars was carried out in the region of the open cluster Havlen-Moffat No. 1. Our data reveal that the extinction law in this cluster es variable and that six cluster stars show very high polarisation values (&gt;4%), probably because of the presence of a nearby small dust cloud. The cluster is at a distance of d=3300pc, it is 2-4Myr old and the initial mass function of its most massive stars (M&gt;3M_{sun}_) has a flat slope of x about of 0.7. 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