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<ri:Resource created="2013-07-09T13:52:25Z" 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>Inner rings in disc galaxies from UV + H{alpha}</title><shortName>J/A+A/555/L4</shortName><identifier>ivo://CDS.VizieR/J/A+A/555/L4</identifier><altIdentifier>doi:10.26093/cds/vizier.35559004</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Comeron S.</name></creator><date role="Updated">2017-09-22T16:15:52Z</date><date role="Created">2013-07-09T13:52:25Z</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>ring-galaxies</subject><description>In this Letter, I distinguish "passive" inner rings to be those with no current star formation, as distinct from "active" inner rings which have undergone recent star formation. I built a sample of nearby galaxies with inner rings observed in the near- and mid-infrared by the NIRS0S and the S^4^G surveys. I used archival far-ultraviolet (FUV) and H{alpha} imaging of 319 galaxies to diagnose whether their inner rings are passive or active. I found that passive rings are found only in early-type disc galaxies (-3&lt;=T&lt;=2). In this range of stages, 21+/-3% and 28+/-5% of rings are passive according to the FUV and H{alpha} indicators, respectively. A ring which is passive according to FUV is always passive according to H{alpha}, but the reverse is not always true. Ring-lenses form 30-40% of passive rings, which is four times more than the fraction of ring-lenses found in active rings in the stage range -3&lt;=T&lt;=2. This is consistent with both a resonance and a manifold origin for the rings because both models predict purely stellar rings to be wider than their star-forming counterparts. In the case of resonance rings, the widening may be at least partly due to the dissolution of rings. If most inner rings have a resonance origin, I estimate 200Myr to be a lower bound for their dissolution time-scale. This time-scale is on the order of one orbital period at the radius of inner rings.</description><source format="bibcode">2013A&amp;A...555L...4C</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/555/L4</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>http://galex.stsci.edu/GR6/ : GALEX CR6/7 data release</relatedResource></relationship></content><rights>https://cds.unistra.fr/vizier-org/licences_vizier.html</rights><capability><interface xsi:type="vr:WebBrowser"><accessURL use="full">https://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/555/L4</accessURL><mirrorURL 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