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<ri:Resource created="2023-09-28T14:37:27Z" 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>Abundances in cool metal-polluted white dwarfs</title><shortName>J/MNRAS/496/1881</shortName><identifier>ivo://CDS.VizieR/J/MNRAS/496/1881</identifier><altIdentifier>doi:10.26093/cds/vizier.74961881</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Blouin S.</name></creator><date role="Updated">2025-02-20T20:15:59Z</date><date role="Created">2023-09-28T14:37:27Z</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>chemically-peculiar-stars</subject><subject>effective-temperature</subject><subject>stellar-masses</subject><subject>stellar-distance</subject><subject>infrared-photometry</subject><subject>visible-astronomy</subject><subject>broad-band-photometry</subject><description>The accretion of rocky material is responsible for the presence of heavy elements in the atmospheres of a large fraction of white dwarf stars. Those objects represent a unique opportunity to infer the bulk composition of exoplanetesimals. This chemical characterization requires the use of detailed atmosphere models to determine the elemental abundances at the photospheres of white dwarfs. In this work, we use a state-of-the-art model atmosphere code to reanalyse the first large survey of metal-polluted white dwarfs for which abundances are found for multiple elements. We show that the improved constitutive physics of our models lead to systematically higher Mg abundances than previous analyses. We find an average logMg/Ca number abundance ratio of 1.5. This value is significantly above the reference abundance for chondrites, which is expected as current diffusion models predict that for the cool helium-atmosphere white dwarfs of our sample, Mg should remain in the atmosphere longer than Ca. This helps resolve a recently identified Mg depletion problem, where the planetesimals accreted by white dwarfs were reported to be Mg-deficient compared to the expected composition of their planetary systems.</description><source format="bibcode">2020MNRAS.496.1881B</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/496/1881</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/I/347">I/347 : Distances to 1.33 billion stars in Gaia DR2</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/MNRAS/467/4970">J/MNRAS/467/4970 : Cool DZ white dwarfs. I. 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Should Not be used for identification.</description><ucd>meta.record</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>Name</name><description>SDSS identifier (JHHMMSS.ss+DDMMSS.s)</description><ucd>meta.id;meta.main</ucd><dataType xsi:type="vs:VOTableType" arraysize="19*">char</dataType></column><column><name>OName</name><description>Montreal White Dwarf Database identifier</description><ucd>meta.id;meta.dataset</ucd><dataType xsi:type="vs:VOTableType" arraysize="25*">char</dataType></column><column><name>umag</name><description>SDSS u-band magnitude</description><unit>mag</unit><ucd>phot.mag;em.opt.U</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>gmag</name><description>SDSS g-band magnitude</description><unit>mag</unit><ucd>phot.mag;em.opt.B</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>rmag</name><description>SDSS r-band magnitude</description><unit>mag</unit><ucd>phot.mag;em.opt.R</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>imag</name><description>SDSS i-band magnitude</description><unit>mag</unit><ucd>phot.mag;em.opt.I</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>zmag</name><description>SDSS z-band magnitude</description><unit>mag</unit><ucd>phot.mag;em.opt.I</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>Dist</name><description>? 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Should Not be used for identification.</description><ucd>meta.record</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>Name</name><description>SDSS identifier (JHHMMSS.ss+DDMMSS.s)</description><ucd>meta.id;meta.main</ucd><dataType xsi:type="vs:VOTableType" arraysize="19*">char</dataType></column><column><name>Teff</name><description>Effective temperature</description><unit>K</unit><ucd>phys.temperature.effective</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>e_Teff</name><description>Error on Teff</description><unit>K</unit><ucd>stat.error;phys.temperature.effective</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>logg</name><description>Surface gravity (1)</description><unit>log(cm.s**-2)</unit><ucd>phys.gravity</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>e_logg</name><description>? 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