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<ri:Resource created="2020-08-14T07:27:29Z" status="active" updated="2026-02-10T20:07:41Z" 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>Blue-core galaxies properties</title><shortName>J/other/RAA/19.8</shortName><identifier>ivo://CDS.VizieR/J/other/RAA/19.81</identifier><altIdentifier>doi:10.26093/cds/vizier/dx/bjkib</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Chen Y.-Y.</name></creator><creator><name>Chen Y.-M.</name></creator><creator><name>Gu Q.-S.</name></creator><creator><name>Shi Y.</name></creator><creator><name>Bing L.-J.</name></creator><creator><name>Yu X.-L.</name></creator><date role="Updated">2026-02-10T20:07:41Z</date><date role="Created">2020-08-14T07:27:29Z</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>galaxy-classification-systems</subject><description>We select 107 blue-core galaxies from the MaNGA survey, studying their morphology, kinematics as well as the gas-phase metallicity. Our results are as follows: (i) In our sample, 26% of blue-core galaxies have decoupled gas-star kinematics, indicating external gas accretion; 15% have bar-like structure and 8% show post-merger features, such as tidal tails and irregular gas/star velocity field. All these processes/features, such as accreting external misaligned gas, interaction and bar, can trigger gas inflow. Thus the central star-forming activities lead to bluer colors in their centers (blue-core galaxies). (ii) By comparing with the SDSS DR7 star-forming galaxy sample, we find that the blue-core galaxies have higher central gas-phase metallicity than what is predicted by the local mass-metallicity relation. We explore the origin of the higher metallicity, finding that not only the blue-core galaxies, but also the flat-gradient and red-core galaxies all have higher metallicity. 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