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<ri:Resource created="2013-07-04T13:25:55Z" 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>X-ray properties of HM1 and IC2944/2948</title><shortName>J/A+A/555/A83</shortName><identifier>ivo://CDS.VizieR/J/A+A/555/A83</identifier><altIdentifier>doi:10.26093/cds/vizier.35550083</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Naze Y.</name></creator><creator><name>Rauw G.</name></creator><creator><name>Sana H.</name></creator><creator><name>Corcoran M.F.</name></creator><date role="Updated">2023-07-24T15:14:09Z</date><date role="Created">2013-07-04T13:25:55Z</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>x-ray-sources</subject><description>Using XMM-Newton data, we study for the first time the X-ray emission of HM1 and IC2944/2948. Low-mass, pre-main sequence objects with an age of a few Myr are detected, as well as a few background or foreground objects. Most massive stars in both clusters display the usual high-energy properties of that kind of objects, though with log(Lx/Lbol) apparently lower in HM1 than in IC2944/2948. Comparing with studies of other clusters, it seems that low S/N at soft energies, due to the high extinction, may the main cause of this difference. In HM1, the two Wolf-Rayet stars show contrasting behaviours: WR89 is extremely bright, but much softer than WR87. It remains to be seen whether wind-wind collisions or magnetically confined winds can explain such emissions. In IC2944/2948, the X-ray sources concentrate around HD101205; a group of massive stars to the north of this object appears rather isolated, suggesting that there exist two subclusters in the field-of-view.</description><source format="bibcode">2013A&amp;A...555A..83N</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/555/A83</referenceURL><type>Catalog</type><contentLevel>Research</contentLevel><relationship><relationshipType>IsServedBy</relationshipType><relatedResource ivo-id="ivo://CDS.VizieR/TAP">TAP VizieR generic service</relatedResource></relationship><relationship><relationshipType>IsServedBy</relationshipType><relatedResource>Conesearch service</relatedResource></relationship><relationship><relationshipType>related-to</relationshipType><relatedResource ivo-id="ivo://CDS.VizieR/B/ocl">B/ocl : Optically visible open clusters and Candidates (Dias+ 2002-2013)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/B/xmm">B/xmm : XMM-Newton Observation Log (XMM-Newton Science Operation Center, 2012)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/VII/239">VII/239 : History and Accurate Positions for the NGC/IC Objects (Corwin, 2004)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/VII/101">VII/101 : Star Clusters/Associations. 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