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<ri:Resource created="2014-03-13T08:50:49Z" 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>UVES/VLT spectroscopy of white dwarfs</title><shortName>J/A+A/470/1079</shortName><identifier>ivo://CDS.VizieR/J/A+A/470/1079</identifier><altIdentifier>doi:10.26093/cds/vizier.34701079</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Voss B.</name></creator><creator><name>Koester D.</name></creator><creator><name>Napiwotzki R.</name></creator><creator><name>Christlieb N.</name></creator><creator><name>Reimers D.</name></creator><date role="Updated">2018-01-08T06:37:59Z</date><date role="Created">2014-03-13T08:50:49Z</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>white-dwarf-stars</subject><subject>apparent-magnitude</subject><subject>effective-temperature</subject><description>We present a detailed spectroscopic analysis of the stars with helium-dominated spectra in the ESO Supernova Ia Progenitor Survey (SPY). Atmospheric parameters, masses, and abundances of trace hydrogen are determined and discussed in the context of spectral evolution of white dwarfs. The spectra are compared with theoretical model atmospheres using a {chi}^2^ fitting technique, leading to determinations of effective temperature, surface gravity, and hydrogen abundance. Our final sample contains 71 objects, of which 6 are new detections and 14 are reclassified from DB to DBA because of the presence of H lines. One is a cool DO with weak HeII lines, 2 are composite DB+dM. 55% of the DB sample show hydrogen and are thus DBA, a significantly higher fraction than found before.</description><source format="bibcode">2007A&amp;A...470.1079V</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/470/1079</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/III/235">III/235 : Spectroscopically Identified White Dwarfs (McCook+, 2008)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/378/556">J/A+A/378/556 : UVES/VLT spectra of white dwarfs (Koester+, 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