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<ri:Resource created="2016-11-10T12:31:45Z" 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>SDSS WD-M binary parameters</title><shortName>J/AJ/125/2621</shortName><identifier>ivo://CDS.VizieR/J/AJ/125/2621</identifier><altIdentifier>doi:10.26093/cds/vizier.51252621</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Raymond S.N.</name></creator><creator><name>Szkody P.</name></creator><creator><name>Hawley S.L.</name></creator><creator><name>Anderson S.F.</name></creator><creator><name>Brinkmann J.,Covey K.R.</name></creator><creator><name>Mcgehee P.M.</name></creator><creator><name>Schneider D.P.</name></creator><creator><name>West A.A.</name></creator><creator><name>York D.G.</name></creator><date role="Updated">2023-04-06T16:50:55Z</date><date role="Created">2016-11-10T12:31:45Z</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>spectroscopic-binary-stars</subject><subject>visible-astronomy</subject><subject>sloan-photometry</subject><description>We have identified 109 white dwarf (WD)-M dwarf pairs in the Sloan Digital Sky Survey (SDSS) with g&lt;20th magnitude. For each system we determined the temperature of the WD primary and the spectral type of the M dwarf secondary. Using H{alpha} emission as a proxy for the chromospheric activity level of the M dwarf, we investigated correlations between the activity level and properties of the system. Compared with field M dwarfs previously observed in the Palomar/MSU Survey, we see a slightly higher active fraction of early-type stars, with activity levels similar to the field. We have conducted follow-up observations at the ARC 3.5m telescope to obtain radial velocity information and to search for short-period binaries that may be on the verge of interacting. 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