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<ri:Resource created="2012-08-29T13:28:34Z" 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>Orbital eccentricities of 31535 G-dwarfs</title><shortName>J/ApJ/725/L186</shortName><identifier>ivo://CDS.VizieR/J/ApJ/725/L186</identifier><altIdentifier>doi:10.26093/cds/vizier.17259186</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Dierickx M.</name></creator><creator><name>Klement R.</name></creator><creator><name>Rix H.-W.</name></creator><creator><name>Liu C.</name></creator><date role="Updated">2017-09-22T16:15:38Z</date><date role="Created">2012-08-29T13:28:34Z</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>milky-way-galaxy</subject><subject>visible-astronomy</subject><subject>sloan-photometry</subject><subject>metallicity</subject><subject>proper-motions</subject><subject>radial-velocity</subject><subject>g-stars</subject><description>We test four competing models that aim to explain the nature of stars in spiral galaxies that are well away (&gt;1kpc) from the midplane, the so-called thick disk: the stars may have gotten there through orbital migration, through satellite mergers and accretion, or through heating of pre-existing thin disk stars. The eccentricity distribution of thick disk stars has recently been proposed as a diagnostic to differentiate between these mechanisms. Drawing on SDSS-DR7, we have assembled a sample of 31535 G-dwarfs with six-dimensional phase-space information and metallicities and have derived the orbital eccentricities for them.</description><source format="bibcode">2010ApJ...725L.186D</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/725/L186</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/II/294">II/294 : The SDSS Photometric Catalog, Release 7 (Adelman-McCarthy+, 2009)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/714/663">J/ApJ/714/663 : Stellar density map of the Milky Way (de Jong+, 2010)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/137/4377">J/AJ/137/4377 : List of SEGUE plate pairs (Yanny+, 2009)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/698/865">J/ApJ/698/865 : Halo streams in the SDSS-DR7 (Klement+, 2009)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/136/2070">J/AJ/136/2070 : SEGUE stellar parameter pipeline. 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