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<ri:Resource created="2006-02-02T13:35:22Z" 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>M31 Long Period Variables : Photometry</title><shortName>J/ApJS/154/623</shortName><identifier>ivo://CDS.VizieR/J/ApJS/154/623</identifier><altIdentifier>doi:10.26093/cds/vizier.21540623</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Mould J.</name></creator><creator><name>Saha A.</name></creator><creator><name>Hughes S.</name></creator><date role="Updated">2006-02-02T12:35:34Z</date><date role="Created">2006-02-02T13:35:22Z</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><subject>visible-astronomy</subject><subject>kron-cousins-photometry</subject><subject>infrared-photometry</subject><description>A significant fraction of the disk of M31 has been surveyed for long-period variable stars. We report the results, including near-infrared photometry of almost 2000 variables, and light curves in the i band. The period-luminosity relation suggests that most of the variables are asymptotic giant branch stars, and their luminosity function can be understood in terms of mass-loss rates, which increase with increasing luminosity on the giant branch, and star formation rates, which were a few times higher a billion years ago in M31 than they are today. We see some supergiant long-period variables, but somewhat fewer than expected based on their frequency in M33, and confined to the ring of star formation in M31 seen in the IRAS and 2MASS surveys.</description><source format="bibcode">2004ApJS..154..623M</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJS/154/623</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/J/A+A/402/113">J/A+A/402/113 : (RI)c photometry of variables in M31 (Joshi+, 2003)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/421/509">J/A+A/421/509 : AGAPE catalogue of M31 variables (Ansari+, 2004)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/MNRAS/351/1071">J/MNRAS/351/1071 : POINT-AGAPE Survey. 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