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<ri:Resource created="2013-04-12T10:01:50Z" 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>Gas exchanges between galaxies and IGM</title><shortName>J/MNRAS/421/2888</shortName><identifier>ivo://CDS.VizieR/J/MNRAS/421/2888</identifier><altIdentifier>doi:10.26093/cds/vizier.74212888</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Rodrigues M.</name></creator><creator><name>Puech M.</name></creator><creator><name>Hammer F.</name></creator><creator><name>Rothberg B.</name></creator><creator><name>Flores H.</name></creator><date role="Updated">2024-07-17T20:15:16Z</date><date role="Created">2013-04-12T10:01:50Z</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>galaxies</subject><subject>catalogs</subject><subject>chemical-abundances</subject><description>Using a representative sample of 65 intermediate-mass galaxies at z~0.6, we have investigated the interplay between the main ingredients of chemical evolution: metal abundance, gas mass, stellar mass and star formation rate (SFR). All quantities have been estimated using deep spectroscopy and photometry from ultraviolet to infrared and assuming an inversion of the Kennicutt-Schmitt law for the gas fraction. Six billion years ago, galaxies had a mean gas fraction of 32+/-3 per cent, i.e. twice that of their local counterparts. 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