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<ri:Resource created="2025-10-07T15:01:08Z" status="active" updated="2026-08-03T07:31:54Z" 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>Gd, Dy, and Th abundances in MW-disc stars</title><shortName>J/MNRAS/516/3786</shortName><identifier>ivo://CDS.VizieR/J/MNRAS/516/3786</identifier><altIdentifier>doi:10.26093/cds/vizier/bg-g4-3pa</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Mishenina T.</name></creator><creator><name>Pignatari M.</name></creator><creator><name>Gorbaneva T.</name></creator><creator><name>Cote B.</name></creator><creator><name>Yague Lopez A.,Thielemann F.-K.</name></creator><creator><name>Soubiran C.</name></creator><date role="Updated">2026-08-03T07:31:54Z</date><date role="Created">2025-10-07T15:01:08Z</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>galaxy-planes</subject><subject>milky-way-galaxy</subject><subject>late-type-stars</subject><subject>spectroscopy</subject><subject>visible-astronomy</subject><subject>metallicity</subject><subject>chemically-peculiar-stars</subject><subject>effective-temperature</subject><subject>galaxy-kinematics</subject><description>The study of the origin of heavy elements is one of the main goals of nuclear astrophysics. In this paper, we present new observational data for the heavy r-process elements gadolinium (Gd, Z= 64), dysprosium (Dy, Z= 66), and thorium (Th, Z= 90) in a sample of 276 Galactic disc stars (-1.0 &lt; [Fe/H] &lt; + 0.3). The stellar spectra have a high resolution of 42000 and 75000, and the signal-to- noise ratio higher than 100. The LTE abundances of Gd, Dy, and Th have been determined by comparing the observed and synthetic spectra for three Gd lines (149 stars), four Dy lines (152 stars), and the Th line at 4019.13 {AA} (170 stars). For about 70 per cent of the stars in our sample, Gd and Dy are measured for the first time, and Th for 95 per cent of the stars. Typical errors vary from 0.07 to 0.16 dex. This paper provides the first extended set of Th observations in the Milky Way disc. Together with europium (Eu, Z= 63) data from our previous studies, we have compared these new observations with nucleosynthesis predictions and Galactic Chemical Evolution simulations. We confirm that [Gd/Fe] and [Dy/Fe] show the same behaviour of Eu. We study with GCE simulations the evolution of [Th/Fe] in comparison with [Eu/Fe], showing that unlike Eu, either the Th production is metallicity dependent in case of a unique source of the r-process in the Galaxy, or the frequency of the Th-rich r-process source is decreasing with the increase in [Fe/H].</description><source format="bibcode">2022MNRAS.516.3786M</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/516/3786</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/MNRAS/340/304">J/MNRAS/340/304 : [X/Fe] of Galactic disc F and G dwarfs (Reddy+, 2003)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/MNRAS/474/2580">J/MNRAS/474/2580 : Temporal evolution of neutron-capture elements (Spina+,2018)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/MNRAS/482/1690">J/MNRAS/482/1690 : Thorium in solar twins (Botelho+, 2019)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/MNRAS/489/1697">J/MNRAS/489/1697 : Galactic disc enrichment with Mo and Ru (Mishenina+, 2019)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/411/559">J/A+A/411/559 : Effective temperature for 181 F-K dwarfs (Kovtyukh+, 2003)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/418/551">J/A+A/418/551 : Galactic disk stars abundances and velocities</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/433/185">J/A+A/433/185 : Detailed abundance analysis of 102 F and G dwarfs</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/439/129">J/A+A/439/129 : HERES II. 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Gadolinium heavy r-process element to iron abundance ratio ([Gd/Fe])</description><unit>log(Sun)</unit><ucd>phys.abund;arith.ratio;meta.modelled</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>s_[Gd/Fe]</name><description>? Standard deviation of [Gd/Fe] (Standard_deviation_[Gd/Fe])</description><unit>log(Sun)</unit><ucd>stat.stdev;phys.abund;meta.modelled</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>[Dy/Fe]</name><description>? Dysprosium heavy r-process element to iron abundance ratio ([Dy/Fe])</description><unit>log(Sun)</unit><ucd>phys.abund;arith.ratio;meta.modelled</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>s_[Dy/Fe]</name><description>? Standard deviation of [Dy/Fe] (Standard_deviation_[Dy/Fe])</description><unit>log(Sun)</unit><ucd>stat.stdev;phys.abund;meta.modelled</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>[Th/Fe]</name><description>? 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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>HD/BD star name number (HD/BD)</description><ucd>meta.id;meta.main</ucd><dataType xsi:type="vs:VOTableType" arraysize="8*">char</dataType></column><column><name>Teff</name><description>Effective temperature from Mishenina et al. 2013A&amp;A...552A.128M, Cat. J/A+A/552/A128 (T_eff_)</description><unit>K</unit><ucd>phys.temperature.effective</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>logg</name><description>Logarithm of surface gravity from Mishenina et al. 2013A&amp;A...552A.128M, Cat. J/A+A/552/A128 (logg)</description><unit>log(cm.s**-2)</unit><ucd>phys.gravity</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>[Fe/H]</name><description>Iron to hydrogen abundance ratio from Mishenina et al. 2013A&amp;A...552A.128M, Cat. 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