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<ri:Resource created="2022-02-03T08:21:40Z" 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>J-PLUS white dwarf atmospheric parameters</title><shortName>J/A+A/658/A79</shortName><identifier>ivo://CDS.VizieR/J/A+A/658/A79</identifier><altIdentifier>doi:10.26093/cds/vizier.36580079</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Lopez-Sanjuan C.</name></creator><creator><name>Tremblay P.-E.</name></creator><creator><name>Ederoclite A.</name></creator><creator><name>Vazquez Ramio H.,Carrasco J.M.</name></creator><creator><name>Varela J.</name></creator><creator><name>Cenarro A.J.</name></creator><creator><name>Marin-Franch A.</name></creator><creator><name>Civera T.,Daflon S.</name></creator><creator><name>Gaensicke B.T.</name></creator><creator><name>Gentile Fusillo N.P.</name></creator><creator><name>Jimenez-Esteban F.M.,Alcaniz J.</name></creator><creator><name>Angulo R.E.</name></creator><creator><name>Cristobal-Hornillos D.</name></creator><creator><name>Dupke R.A.,Hernandez-Monteagudo</name></creator><creator><name>C.</name></creator><creator><name>Moles M.</name></creator><creator><name>Sodre Jr.L.</name></creator><date role="Updated">2024-08-13T20:01:20Z</date><date role="Created">2022-02-03T08:21:40Z</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>effective-temperature</subject><subject>stellar-masses</subject><subject>visible-astronomy</subject><description>We estimated the spectral evolution of white dwarfs with effective temperature using the Javalambre Photometric Local Universe Survey (J-PLUS) second data release (DR2), which provides 12 photometric optical passbands over 2176deg^2^. We analyzed 5926 white dwarfs with r&lt;19.5mag in common between a white dwarf catalog defined from Gaia EDR3 and J-PLUS DR2. We performed a Bayesian analysis by comparing the observed J-PLUS photometry with theoretical models of hydrogen- and helium-dominated atmospheres. We estimated the probability distribution functions for effective temperature (Teff), surface gravity, parallax, and composition; and the probability of having a H-dominated atmosphere (p_H_) for each source. We applied a prior in parallax, using Gaia EDR3 measurements as a reference, and derived a self-consistent prior for the atmospheric composition as a function of Teff. We described the fraction of white dwarfs with a He-dominated atmosphere (f_He_) with a linear function of the effective temperature at 5000&lt;Teff&lt;30000K. We find f_He_=0.24+/-0.01 at Teff=10000K, a change rate along the cooling sequence of 0.14+/-0.02 per 10kK, and a minimum He-dominated fraction of 0.08+/-0.02 at the high-temperature end. We tested the obtained p_H_ by comparison with spectroscopic classifications, finding that it is reliable. We estimated the mass distribution for the 351 sources with distance d&lt;100pc, mass M&gt;0.45M_{sun}_, and Teff&gt;6000K. The result for H-dominated white dwarfs agrees with previous studies, with a dominant M=0.59M_{sun}_ peak and the presence of an excess at M~0.8M_{sun}_. This high-mass excess is absent in the He-dominated distribution, which presents a single peak. The J-PLUS optical data provide a reliable statistical classification of white dwarfs into H- and He-dominated atmospheres. We find a 21+/-3% increase in the fraction of He-dominated white dwarfs from Teff=20000K to Teff=5000K.</description><source format="bibcode">2022A&amp;A...658A..79L</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/658/A79</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>http://archive.cefca.es/catalogues/jplus-dr2 : J-PLUS DR2 Home Page</relatedResource></relationship></content><rights>https://cds.unistra.fr/vizier-org/licences_vizier.html</rights><capability><interface xsi:type="vr:WebBrowser"><accessURL 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