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<ri:Resource created="2026-09-08T07:53:07Z" status="active" updated="2026-09-08T06:54:07Z" 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>[Y/Mg] chemical clock from asteroseismic ages</title><shortName>J/A+A/713/A48</shortName><identifier>ivo://CDS.VizieR/J/A+A/713/A48</identifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Mikolaitis S.</name></creator><creator><name>Tautvaisiene G.</name></creator><creator><name>Pakstiene E.</name></creator><creator><name>Drazdauskas A.</name></creator><creator><name>Bagdonas V.,Viscasillas Vazquez C.</name></creator><creator><name>Ambrosch M.</name></creator><creator><name>Chorniy Y.</name></creator><creator><name>Minkeviciute R.,Stonkute E.</name></creator><creator><name>Bale B.</name></creator><creator><name>Curjuric B.</name></creator><creator><name>Sharma A.</name></creator><creator><name>Diktanaite K.</name></creator><date role="Updated">2026-09-08T06:54:07Z</date><date role="Created">2026-09-08T07:53:07Z</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>chemical-abundances</subject><subject>stellar-ages</subject><subject>astronomical-models</subject><description>Building on our previous study, which demonstrated the necessity of accounting for departures from the local thermodynamic equilibrium while determining elemental abundances, and the importance of asteroseismic ages, we aim to characterise the spatial variations of the empirical [Y/Mg]-age relation across the Galactic disc with a significantly larger sample of stars. We observed high-resolution stellar spectra and determined Mg and Y abundances via spectral synthesis of multiple spectral features, rigorously accounting for non-local thermodynamic equilibrium (NLTE) effects. To anchor the time scale, we determined asteroseismic ages for stars showing solar-type pulsations, while employing cross-checked isochrone-based methods for the remaining stars. We determined the main atmospheric parameters and abundances of Mg and Y for a sample of 528 Galactic field stars, as well as asteroseismic ages for 307 stars and cross-checked isochronal ages for 221 stars. We identified two new triple-lined and nine double-lined spectroscopic stellar systems. Based on a total sample of 736 stars, with data from this and our previous study, we have explored the [Y/Mg] versus age relations across the Galactic disc. The [Y/Mg] versus age relations exhibit systematic variations across the Galactic discs, reflecting differences in star formation and enrichment histories. There is a tendency for [Y/Mg] to increase with increasing metallicity across the age range. 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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>Simbad</name><description>Simbad column added by the CDS</description><ucd>meta.ref.url</ucd><dataType xsi:type="vs:VOTableType" arraysize="*">char</dataType></column><column><name>ID</name><description>Tycho-2 catalogue identification</description><ucd>meta.id;meta.main</ucd><dataType xsi:type="vs:VOTableType" arraysize="14*">char</dataType></column><column><name>Teff</name><description>Effective temperature</description><unit>K</unit><ucd>phys.temperature.effective</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>e_Teff</name><description>Uncertainty in effective temperature</description><unit>K</unit><ucd>stat.error;phys.temperature.effective</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>logg</name><description>Surface gravity</description><unit>log(cm.s**-2)</unit><ucd>phys.gravity</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>e_logg</name><description>Uncertainty in surface gravity</description><unit>log(cm.s**-2)</unit><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>[Fe/H]</name><description>Metallicity</description><ucd>phys.abund.Z</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>e_[Fe/H]</name><description>Uncertainty in metallicity</description><ucd>stat.error;phys.abund.Fe</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>Vt</name><description>Microturbulence velocity</description><unit>km/s</unit><ucd>phys.veloc.microTurb</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>e_Vt</name><description>Uncertainty in microturbulence velocity</description><unit>km/s</unit><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>[Mg/H]</name><description>? 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