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<ri:Resource created="2005-03-04T16:07:37Z" 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>Period of Cepheids in M 83</title><shortName>J/ApJ/591/L111</shortName><identifier>ivo://CDS.VizieR/J/ApJ/591/L111</identifier><altIdentifier>doi:10.26093/cds/vizier.15919111</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Bonanos A.Z.</name></creator><creator><name>Stanek K.Z.</name></creator><date role="Updated">2005-03-04T15:08:07Z</date><date role="Created">2005-03-04T16:07:37Z</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>variable-stars</subject><description>We apply the image-subtraction method in order to reanalyze the ESO Very Large Telescope data on M83 (NGC 5236), obtained and analyzed by Thim et al. (2003ApJ...590..256T). Whereas Thim et al. (2003ApJ...590..256T) found 12 Cepheids with periods between 12 and 55 days, we find 112 Cepheids with periods ranging from 7 to 91 days as well as 60 other variables. These include two candidate eclipsing binaries, which, if confirmed, would be the first optically discovered outside the Local Group. We thus demonstrate that the image-subtraction method is much more powerful for detecting variability, especially in crowded fields. However, Hubble Space Telescope observations are necessary to obtain a Cepheid period-luminosity distance not dominated by blending and crowding. 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Should Not be used for identification.</description><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>RAJ2000</name><description>Hour of Right Ascension (J2000)</description><ucd>pos.eq.ra;meta.main</ucd></column><column><name>DEJ2000</name><description>Degree of Declination (J2000)</description><ucd>pos.eq.dec;meta.main</ucd></column><column><name>Per</name><description>Period</description><unit>d</unit><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>Xpix</name><description>The X pixel coordinate on the reference image</description><unit>pix</unit><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>Ypix</name><description>The Y pixel coordinate on the reference image</description><unit>pix</unit><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>Comm</name><description>Additional comments (1)</description><dataType xsi:type="vs:VOTableType" arraysize="15*">char</dataType></column></table></schema></tableset></ri:Resource>