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<ri:Resource created="2018-06-27T09:15:04Z" 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>NLTE spectroscopy. II. Galactic metal-poor stars</title><shortName>J/ApJ/847/16</shortName><identifier>ivo://CDS.VizieR/J/ApJ/847/16</identifier><altIdentifier>doi:10.26093/cds/vizier.18470016</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Bergemann M.</name></creator><creator><name>Collet R.</name></creator><creator><name>Schonrich R.</name></creator><creator><name>Andrae R.</name></creator><creator><name>Kovalev M.</name></creator><creator><name>Ruchti G.,Hansen C.J.</name></creator><creator><name>Magic Z.</name></creator><date role="Updated">2018-09-25T13:12:59Z</date><date role="Created">2018-06-27T09:15:04Z</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>chemically-peculiar-stars</subject><subject>chemical-abundances</subject><subject>line-intensities</subject><description>From exploratory studies and theoretical expectations it is known that simplifying approximations in spectroscopic analysis (local thermodynamic equilibrium (LTE), 1D) lead to systematic biases of stellar parameters and abundances. These biases depend strongly on surface gravity, temperature and, in particular, for LTE versus non-LTE (NLTE), on metallicity of the stars. Here we analyze the [Mg/Fe] and [Fe/H] plane of a sample of 326 stars, comparing LTE and NLTE results obtained using 1D hydrostatic models and averaged &lt;3D&gt; models. We show that compared to the &lt;3D&gt; NLTE benchmark, the other three methods display increasing biases toward lower metallicities, resulting in false trends of [Mg/Fe] against [Fe/H], which have profound implications for interpretations by chemical evolution models. In our best &lt;3D&gt; NLTE model, the halo and disk stars show a clearer behavior in the [Mg/Fe]-[Fe/H] plane, from the knee in abundance space down to the lowest metallicities. Our sample has a large fraction of thick disk stars and this population extends down to at least [Fe/H]~-1.6dex, further than previously proven. The thick disk stars display a constant [Mg/Fe]~0.3dex, with a small intrinsic dispersion in [Mg/Fe] that suggests that a fast SN Ia channel is not relevant for the disk formation. The halo stars reach higher [Mg/Fe] ratios and display a net trend of [Mg/Fe] at low metallicities, paired with a large dispersion in [Mg/Fe]. These indicate the diverse origin of halo stars from accreted low-mass systems to stochastic/inhomogeneous chemical evolution in the Galactic halo.</description><source format="bibcode">2017ApJ...847...16B</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/847/16</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/III/257">III/257 : RAVE second data release (Zwitter+, 2008)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/III/279">III/279 : RAVE 5th data release (Kunder+, 2017)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/I/337">I/337 : Gaia DR1 (Gaia Collaboration, 2016)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/I/345">I/345 : Gaia DR2 (Gaia Collaboration, 2018)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/128/1177">J/AJ/128/1177 : Galactic stellar abundances (Venn+, 2004)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/511/L10">J/A+A/511/L10 : Abundances and space velocities of 94 stars (Nissen+, 2010)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/530/A138">J/A+A/530/A138 : Geneva-Copenhagen survey re-analysis (Casagrande+, 2011)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/530/A54">J/A+A/530/A54 : Abundances of 650 bulge red giants (Gonzalez+, 2011)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/737/9">J/ApJ/737/9 : RAVE data of stars in the thick disk (Ruchti+, 2011)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/546/A90">J/A+A/546/A90 : NLTE analysis of Sr lines (Bergemann+, 2012)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/557/A26">J/A+A/557/A26 : STAGGER-grid of 3D stellar models. 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Should Not be used for identification.</description><ucd>meta.record</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>Name</name><description>Simbad data-base identifier</description><ucd>meta.id;meta.dataset</ucd><dataType xsi:type="vs:VOTableType" arraysize="21*">char</dataType></column><column><name>Teff1</name><description>[4004/6531] LTE-Fe effective temperature</description><unit>K</unit><ucd>phys.temperature.effective</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>log(g)1</name><description>[0.5/4.4] LTE-Fe surface gravity</description><unit>log(cm.s**-2)</unit><ucd>phys.gravity</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>[Fe/H]1</name><description>[-3.2/-0.3] LTE-Fe metallicity</description><unit>log(Sun)</unit><ucd>phys.abund.Z</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>V1</name><description>[0.5/3] LTE-Fe microturbulence</description><unit>km/s</unit><ucd>phys.veloc.microTurb</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>Teff2</name><description>[4043/6519] NLTE-Opt effective temperature</description><unit>K</unit><ucd>phys.temperature.effective</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>log(g)2</name><description>[0.5/4.6] NLTE-Opt surface gravity</description><unit>log(cm.s**-2)</unit><ucd>phys.gravity</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>[Fe/H]2</name><description>[-2.8/-0.4] NLTE-Opt metallicity</description><unit>log(Sun)</unit><ucd>phys.abund.Z</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>V2</name><description>[0.5/3.3] NLTE-Opt microturbulence</description><unit>km/s</unit><ucd>phys.veloc.microTurb</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>[Mg]1</name><description>[-0.03/0.7]? 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