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<ri:Resource created="2015-01-13T07:31:43Z" 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>Spectroscopy of Damped Ly{alpha} (DLA) systems</title><shortName>J/ApJ/769/54</shortName><identifier>ivo://CDS.VizieR/J/ApJ/769/54</identifier><altIdentifier>doi:10.26093/cds/vizier.17690054</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Neeleman M.</name></creator><creator><name>Wolfe A.M.</name></creator><creator><name>Prochaska J.X.</name></creator><creator><name>Rafelski M.</name></creator><date role="Updated">2017-11-29T11:48:10Z</date><date role="Created">2015-01-13T07:31:43Z</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>line-intensities</subject><subject>quasars</subject><subject>redshifted</subject><subject>chemical-abundances</subject><description>Using a sample of 100 H I-selected damped Ly{alpha} (DLA) systems, observed with the High Resolution Echelle Spectrometer on the Keck I telescope, we present evidence that the scatter in the well-studied correlation between the redshift and metallicity of a DLA is largely due to the existence of a mass-metallicity relationship at each redshift. To describe the fundamental relations that exist between redshift, metallicity, and mass, we use a fundamental plane description, which is described by the following equation: [M/H]=(-1.9+/-0.5)+(0.74+/-0.21)*log{Delta}v_90_-(0.32+/-0.06)*z. Here, we assert that the velocity width, {Delta}v_90_, which is defined as the velocity interval containing 90% of the integrated optical depth, traces the mass of the underlying dark matter halo. This description provides two significant improvements over the individual descriptions of the mass-metallicity correlation and metallicity-redshift correlation. Firstly, the fundamental equation reduces the scatter around both relationships by about 20%, providing a more stringent constraint on numerical simulations modeling DLAs. Secondly, it confirms that the dark matter halos that host DLAs satisfy a mass-metallicity relationship at each redshift between redshifts 2 through 5.</description><source format="bibcode">2013ApJ...769...54N</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/769/54</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/II/294">II/294 : The SDSS Photometric Catalog, Release 7 (Adelman-McCarthy+, 2009)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/MNRAS/435/482">J/MNRAS/435/482 : DLA system from SDSS DR5 (Jorgenson+, 2013)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/755/89">J/ApJ/755/89 : Metallicities of damped Ly{alpha} systems (Rafelski+, 2012)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/547/L1">J/A+A/547/L1 : SDSS-III DR9 DLA catalogue (Noterdaeme+, 2012)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/530/A33">J/A+A/530/A33 : Evolutionary tracks of DLA depletions (Vladilo+, 2011)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/721/1">J/ApJ/721/1 : Keck ESI observations of Ly{alpha} systems (Penprase+, 2010)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/505/1087">J/A+A/505/1087 : DLAs in SDSS-DR7 (Noterdaeme+, 2009)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/683/321">J/ApJ/683/321 : Metallicities of GRB, DLA, &amp; Ly{alpha} gal. (Fynbo+, 2008)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/478/701">J/A+A/478/701 : Color excess of SDSS QSOs with DLA systems (Vladilo+, 2008)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/473/791">J/A+A/473/791 : CIV absorption in DLAs and sub-DLAs systems (Fox+, 2007)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJS/171/29">J/ApJS/171/29 : UCSD/Keck DLA Abundance Database (Prochaska+, 2007)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/PASP/118/1077">J/PASP/118/1077 : Metal-strong damped Ly{alpha} systems (Herbert-Fort+, 2006)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/130/1345">J/AJ/130/1345 : Optical-infrared colors of CORALS QSOs (Ellison+, 2005)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/635/123">J/ApJ/635/123 : The SDSS-DR3 damped Ly{alpha} survey (Prochaska+, 2005)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/MNRAS/354/L31">J/MNRAS/354/L31 : SDSS 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