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<ri:Resource created="2009-04-07T17:36:14Z" 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>Fundamental parameters of M dwarfs</title><shortName>J/MNRAS/389/585</shortName><identifier>ivo://CDS.VizieR/J/MNRAS/389/585</identifier><altIdentifier>doi:10.26093/cds/vizier.73890585</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Casagrande L.</name></creator><creator><name>Flynn C.</name></creator><creator><name>Bessell M.</name></creator><date role="Updated">2024-07-07T20:16:53Z</date><date role="Created">2009-04-07T17:36:14Z</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>dwarf-stars</subject><subject>m-stars</subject><subject>infrared-photometry</subject><subject>visible-astronomy</subject><subject>broad-band-photometry</subject><subject>effective-temperature</subject><description>We empirically determine effective temperatures and bolometric luminosities for a large sample of nearby M dwarfs, for which high accuracy optical and infrared photometry is available. We introduce a new technique which exploits the flux ratio in different bands as a proxy of both effective temperature and metallicity. Our temperature scale for late-type dwarfs extends well below 3000K (almost to the brown dwarf limit) and is supported by interferometric angular diameter measurements above 3000K. Our metallicities are in excellent agreement (usually within 0.2dex) with recent determinations via independent techniques. A subsample of cool M dwarfs with metallicity estimates based on hotter Hipparcos common proper motion companions indicates our metallicities are also reliable below 3000K, a temperature range unexplored until now. The high quality of our data allows us to identify a striking feature in the bolometric luminosity versus temperature plane, around the transition from K to M dwarfs. We have compared our sample of stars with theoretical models and conclude that this transition is due to an increase in the radii of the M dwarfs, a feature which is not reproduced by theoretical models.</description><source format="bibcode">2008MNRAS.389..585C</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/389/585</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/MNRAS/334/20">J/MNRAS/334/20 : UBV(RI)_c_ photometry of HIP red stars (Koen+, 2002)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/123/2822">J/AJ/123/2822 : Photometry of southern NLTT stars (Reid+, 2002)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/126/3007">J/AJ/126/3007 : Spectroscopy of faint red NLTT dwarfs (Reid+, 2003)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/128/463">J/AJ/128/463 : A preliminary 20pc census from NLTT catalogue (Reid+, 2004)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/MNRAS/373/13">J/MNRAS/373/13 : Lower main-sequence stars fund. param. 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