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<ri:Resource created="2015-09-03T08:09:42Z" 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>IFU observations of NGC 4191</title><shortName>J/A+A/581/A65</shortName><identifier>ivo://CDS.VizieR/J/A+A/581/A65</identifier><altIdentifier>doi:10.26093/cds/vizier.35810065</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Coccato L.</name></creator><creator><name>Fabricius M.</name></creator><creator><name>Morelli L.</name></creator><creator><name>Corsini E.M.</name></creator><creator><name>Pizzella A.,Erwin P.</name></creator><creator><name>Dalla Bonta E.</name></creator><creator><name>Saglia R.</name></creator><creator><name>Bender R.</name></creator><creator><name>Williams M.</name></creator><date role="Updated">2022-12-20T09:23:11Z</date><date role="Created">2015-09-03T08:09:42Z</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>visible-astronomy</subject><subject>spectroscopy</subject><description>We here distinguish two counter-rotating stellar components in NGC 4191 and characterize their physical properties such as kinematics, size, morphology, age, metallicity. We obtained integral field spectroscopic observations with VIRUS-W and used a spectroscopic decomposition technique to separate the contribution of two stellar components to the observed galaxy spectrum. We also performed a photometric decomposition, modeling the galaxy with a Sersic bulge and two exponential disks of different scale length, with the aim of associating these structural components with the kinematic components. 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