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<ri:Resource created="2019-12-16T09:19:44Z" 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>Radial velocity changes for 439 white dwarfs</title><shortName>J/MNRAS/467/1414</shortName><identifier>ivo://CDS.VizieR/J/MNRAS/467/1414</identifier><altIdentifier>doi:10.26093/cds/vizier.74671414</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Maoz D.</name></creator><creator><name>Hallakoun N.</name></creator><date role="Updated">2024-08-17T20:18:09Z</date><date role="Created">2019-12-16T09:19:44Z</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>multiple-stars</subject><subject>radial-velocity</subject><description>From a sample of spectra of 439 white dwarfs (WDs) from the ESO-VLT Supernova-Ia Progenitor Survey (SPY), we measure the maximal changes in radial velocity ({Delta}RVmax) between epochs (generally two epochs, separated by up to 470d), and model the observed {Delta}RVmax statistics via Monte Carlo simulations, to constrain the population characteristics of double WDs (DWDs). The DWD fraction among WDs is f_bin_=0.10+/-0.02 (1{sigma}, random) +0.02 (systematic), in the separation range &lt;~4au within which the data are sensitive to binarity. Assuming the distribution of binary separation, a, is a power law, dN/da{prop.to}a^alpha^, at the end of the last common-envelope phase and the start of solely gravitational-wave-driven binary evolution, the constraint by the data is alpha=-1.3+/-0.2(1{sigma}) +/-0.2 (systematic). If these parameters extend to small separations, the implied Galactic WD merger rate per unit stellar mass is R_merge_=(1-80)x10^-13^yr^-1^M_[sun}_^-1^ (2{sigma}), with a likelihood-weighted mean of R_merge_=(7+/-2)x10^-13^yr^-1^M_{sun}_^-1^ (1{sigma}). The Milky Way's specific Type Ia supernova (SN Ia) rate is likely R_Ia_~=1.1x10^-13^yr^-1^M_{sun}_^-1^ and therefore, in terms of rates, a possibly small fraction of all merging DWDs (e.g. those with massive-enough primary WDs) could suffice to produce most or all SNe Ia.</description><source format="bibcode">2017MNRAS.467.1414M</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/467/1414</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></content><rights>https://cds.unistra.fr/vizier-org/licences_vizier.html</rights><capability><interface xsi:type="vr:WebBrowser"><accessURL 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arraysize="12*">char</dataType></column><column><name>recno</name><description>Record number assigned by the VizieR team. Should Not be used for identification.</description><ucd>meta.record</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>Note</name><description>[*] Note (1)</description><ucd>meta.note</ucd><dataType xsi:type="vs:VOTableType" arraysize="1*">char</dataType></column><column><name>Name</name><description>WD name</description><ucd>meta.id;meta.main</ucd><dataType xsi:type="vs:VOTableType" arraysize="13*">char</dataType></column><column><name>RAJ2000</name><description>Right ascension (J2000)</description><ucd>pos.eq.ra;meta.main</ucd></column><column><name>DEJ2000</name><description>Declination (J2000)</description><ucd>pos.eq.dec;meta.main</ucd></column><column><name>Deltat</name><description>Epoch separation</description><unit>d</unit><ucd>time.epoch</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>DeltaRVmax</name><description>Maximum velocity difference between epochs</description><unit>km/s</unit><ucd>spect.dopplerVeloc;arith.diff;stat.max</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>sigma</name><description>Root of the summed squares of the RV errors of the two individual RV measurements forming each difference</description><unit>km/s</unit><ucd>stat.stdev</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>Nsigma</name><description>DeltaRVmax/sigma ratio</description><ucd>stat.fit.omc</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>M1</name><description>Derived mass for the photometric-primary WD</description><unit>solMass</unit><ucd>phys.mass</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>Com</name><description>Comments (2)</description><ucd>meta.note</ucd><dataType xsi:type="vs:VOTableType" arraysize="4*">char</dataType></column></table></schema></tableset></ri:Resource>