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<ri:Resource created="2025-04-25T15:35:37Z" status="active" updated="2026-07-03T06:36:52Z" 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>Cu abundances</title><shortName>J/A+A/696/A210</shortName><identifier>ivo://CDS.VizieR/J/A+A/696/A210</identifier><altIdentifier>doi:10.26093/cds/vizier/bc-nr/lcba</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Caliskan S.</name></creator><creator><name>Amarsi A.M.</name></creator><creator><name>Racca M.</name></creator><creator><name>Koutsouridou I.</name></creator><creator><name>Barklem P.S.</name></creator><creator><name>Lind K.,Salvadori S.</name></creator><date role="Updated">2026-07-03T06:36:52Z</date><date role="Created">2025-04-25T15:35:37Z</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>atomic-physics</subject><subject>chemical-abundances</subject><description>The Galactic evolution of copper remains poorly understood, partly due to the strong departures from local thermodynamic equilibrium (LTE) affecting CuI lines. A key source of uncertainty in non-LTE modelling is the treatment of inelastic Cu+H collisions. We present new rate coefficients based on a combined asymptotic LCAO (linear combination of atomic orbitals) and free electron model approach, which show significant differences from previous calculations. Applying these updated rates to non-LTE stellar modelling, we find reduced line-to-line scatter and improved consistency between metal-poor dwarfs and giants. Our non-LTE analysis reveals a strong upturn in the [Cu/Fe] trend towards lower [Fe/H]&lt;-1.7. We show that this may reflect the interplay between external enrichment of Cu-rich material of the Milky Way halo at low metallicities, and metallicity-dependent Cu yields from rapidly rotating massive stars. 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