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<ri:Resource created="2015-04-16T14:14:23Z" 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>SIM2D parameters of SDSS-DR7 galaxies</title><shortName>J/MNRAS/440/843</shortName><identifier>ivo://CDS.VizieR/J/MNRAS/440/843</identifier><altIdentifier>doi:10.26093/cds/vizier.74400843</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Omand C.M.B.</name></creator><creator><name>Balogh M.L.</name></creator><creator><name>Poggianti B.M.</name></creator><date role="Updated">2024-08-09T20:14:46Z</date><date role="Created">2015-04-16T14:14:23Z</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>galaxy-classification-systems</subject><description>Using data from the Sloan Digital Sky Survey (SDSS)-DR7, including structural measurements from 2D surface brightness fits with gim2d, we show how the fraction of quiescent galaxies depends on galaxy stellar mass M*, effective radius Re, fraction of r-band light in the bulge, B/T, and their status as a central or satellite galaxy at 0.01&lt;z&lt;0.2. For central galaxies we confirm that the quiescent fraction depends not only on stellar mass, but also on Re. The dependence is particularly strong as a function of M*/Re^{alpha}^, with {alpha}~1.5. This appears to be driven by a simple dependence on B/T over the mass range 9&lt;log(M*/M_{sun}_)&lt;11.5, and is qualitatively similar even if galaxies with B/T&gt;0.3 are excluded. For satellite galaxies, the quiescent fraction is always larger than that of central galaxies, for any combination of M*, Re and B/T. The quenching efficiency is not constant, but reaches a maximum of ~0.7 for galaxies with 9&lt;log(M*/M_{sun}_)&lt;9.5 and Re&lt;1kpc. This is the same region of parameter space in which the satellite fraction itself reaches its maximum value, suggesting that the transformation from an active central galaxy to a quiescent satellite is associated with a reduction in Re due to an increase in dominance of a bulge component.</description><source format="bibcode">2014MNRAS.440..843O</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/440/843</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/J/ApJS/196/11">J/ApJS/196/11 : Bulge+disk decompositions of SDSS galaxies (Simard+, 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