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<ri:Resource created="2011-11-06T18:30:09Z" 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>SAGA extremely metal-poor stars</title><shortName>J/MNRAS/412/843</shortName><identifier>ivo://CDS.VizieR/J/MNRAS/412/843</identifier><altIdentifier>doi:10.26093/cds/vizier.74120843</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Suda T.</name></creator><creator><name>Yamada S.</name></creator><creator><name>Katsuta Y.</name></creator><creator><name>Komiya Y.</name></creator><creator><name>Ishizuka C.</name></creator><creator><name>Aoki W.,Fujimoto M.Y.</name></creator><date role="Updated">2024-07-13T20:15:05Z</date><date role="Created">2011-11-06T18:30:09Z</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>population-ii-stars</subject><subject>chemically-peculiar-stars</subject><subject>chemical-abundances</subject><description>We discuss the characteristics of known extremely metal-poor (EMP) stars in the Galaxy using the Stellar Abundances for Galactic Archaeology (SAGA) data base. We find the transition of the initial mass function to be at [Fe/H]~-2 from the viewpoint of the distribution of carbon abundance and the frequency of carbon-enhanced stars. Analyses of carbon-enhanced stars in our sample suggest that nucleosynthesis in asymptotic giant branch (AGB) stars can contribute to carbon enrichment in a different way depending on whether the metallicity is above or below [Fe/H]~-2.5, which is consistent with the current models of stellar evolution at low metallicity.</description><source format="bibcode">2011MNRAS.412..843S</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/412/843</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/A+A/403/1105">J/A+A/403/1105 : Extremely metal-poor giants equivalent widths (Francois+ 2003)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/128/2402">J/AJ/128/2402 : Extremely metal-poor star candidates abundances (Lai+, 2004)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/132/137">J/AJ/132/137 : Abundances of extremely metal-poor carbon stars (Cohen+, 2006)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/490/769">J/A+A/490/769 : Yields from extremely metal-poor stars (Campbell+, 2008)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/501/519">J/A+A/501/519 : Extremely metal-poor turnoff stars abund. 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