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<ri:Resource created="2012-08-01T16:46:09Z" 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>M dwarf flares from SDSS spectra</title><shortName>J/AJ/140/1402</shortName><identifier>ivo://CDS.VizieR/J/AJ/140/1402</identifier><altIdentifier>doi:10.26093/cds/vizier.51401402</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Hilton E.J.</name></creator><creator><name>West A.A.</name></creator><creator><name>Hawley S.L.</name></creator><creator><name>Kowalski A.F.</name></creator><date role="Updated">2017-11-29T11:49:14Z</date><date role="Created">2012-08-01T16:46:09Z</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>late-type-stars</subject><subject>stellar-flares</subject><description>We have identified 63 flares on M dwarfs from the individual component spectra in the Sloan Digital Sky Survey (SDSS) using a novel measurement of emission-line strength called the Flare Line Index. Each of the ~38000M dwarfs in the SDSS low-mass star spectroscopic sample of West et al. (2008, Cat. J/AJ/135/785) was observed several times (usually 3-5) in exposures that were typically 9-25 minutes in duration. Our criteria allowed us to identify flares that exhibit very strong H{alpha} and H{beta} emission-line strength and/or significant variability in those lines throughout the course of the exposures. 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