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<ri:Resource created="2021-03-04T09:42:25Z" status="active" updated="2025-06-13T15:25:00Z" 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>Passive spiral galaxies quench</title><shortName>J/MNRAS/474/1909</shortName><identifier>ivo://CDS.VizieR/J/MNRAS/474/1909</identifier><altIdentifier>doi:10.26093/cds/vizier.74741909</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Fraser-McKelvie A.</name></creator><creator><name>Brown M.J.I.</name></creator><creator><name>Pimbblet K.</name></creator><creator><name>Dolley T.</name></creator><creator><name>Bonne N.J.</name></creator><date role="Updated">2024-08-18T20:17:09Z</date><date role="Created">2021-03-04T09:42:25Z</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>galaxy-classification-systems</subject><description>We examine the properties of a sample of 35 nearby passive spiral galaxies in order to determine their dominant quenching mechanism(s). All five low-mass (M*&lt;1x10^10^M_{sun}_) passive spiral galaxies are located in the rich Virgo cluster. This is in contrast to low-mass spiral galaxies with star formation, which inhabit a range of environments. We postulate that cluster-scale gas stripping and heating mechanisms operating only in rich clusters are required to quench low-mass passive spirals, and ram-pressure stripping and strangulation are obvious candidates. For higher mass passive spirals, while trends are present, the story is less clear. The passive spiral bar fraction is high: 74+/-15 per cent, compared with 36+/-5 per cent for a mass, redshift and T-type matched comparison sample of star-forming spiral galaxies. The high mass passive spirals occur mostly, but not exclusively, in groups, and can be central or satellite galaxies. The passive spiral group fraction of 74+/-15 per cent is similar to that of the comparison sample of star-forming galaxies at 61+/-7 per cent. We find evidence for both quenching via internal structure and environment in our passive spiral sample, though some galaxies have evidence of neither. 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