J/A+A/660/A135ivo://CDS.VizieR/J/A+A/660/A135doi:10.26093/cds/vizier.36600135CDSViscasillas Vazquez C.Magrini L.Casali G.Tautvaisiene G.Spina L.,Van der Swaelmen M.Randich S.Bensby T.Bragaglia A.Friel E.,Feltzing S.Sacco G.G.Turchi A.Jimenez-Esteban F.D'Orazi V.,Delgado-Mena E.Mikolaitis S.Drazdauskas A.Minkeviciute R.,Stonkute E.Bagdonas V.Montes D.Guiglion G.Baratella M.,Tabernero H.M.Gilmore G.Alfaro E.Francois P.Korn A.Smiljanic R.,Bergemann M.Franciosini E.Gonneau A.Hourihane A.Worley C.C.,Zaggia S.2023-01-30T11:33:06Z2022-12-30T08:37:14ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frmilky-way-galaxyopen-star-clusterschemical-abundancesvisible-astronomyThe last decade has seen a revolution in our knowledge of the Galaxy thanks to the Gaia and asteroseismic space missions and the ground-based spectroscopic surveys. To complete this picture, it is necessary to map the ages of its stellar populations. During recent years, the dependence on time of abundance ratios involving slow (s) neutron-capture and {alpha} elements (called chemical-clocks) has been used to provide estimates of stellar ages, usually in a limited volume close to the Sun. We aim to analyse the relations of chemical clocks in the Galactic disc extending the range to Rgc~6-20kpc. Using the sixth internal data release of the Gaia-ESO survey, we calibrated several relations between stellar ages and abundance ratios[s/{alpha}] using a sample of open clusters, the largest one so far used with this aim (62 clusters). Thanks to their wide galactocentric coverage, we investigated the radial variations of the shape of these relations, confirming their non-universality. The multi-variate relations allowed us to infer stellar ages for field stars. We estimated our accuracy (ranging from 0.0 to -0.9Gyr) and precision (from 0.4 to 2.3Gyr) in recovering the global ages of open clusters, and the ages of their individual members. We applied the relations with the highest correlation coefficients to the field star population, finding an older population at lower metallicity and higher [{alpha}/Fe] in the thin disc, and a younger one at higher [Fe/H] and low [{alpha}/Fe], as expected. We confirm that there is no single age-chemical clock relationship valid for the whole disc, but that there is a dependence on the galactocentric position, which is related to the radial variation of the star formation history combined with the non-monotonic dependence on metallicity of the yields of the s-process elements from low- and intermediate-mass stars. Finally, the abundance ratios [Ba/{alpha}] are more sensitive to age than those with [Y/{alpha}] for young disc stars, and their slopes vary less with galactocentric distance. We remind the reader that the application of such relationships to field stars is only of statistical value.2022A&A...660A.135Vhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/660/A135CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/A+A/640/A1 : Portrait Galactic disc (Cantat-Gaudin+, 2020)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/660/A135https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/660/A135http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/660/A135https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/660/A135https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/660/A135http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/660/A135GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/660/A135/tablea1 (Metallicity of each cluster, galactocentric distance, age and abundance ratios (average ratios [s/H] and [s/Fe] of open clusters))https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/660/A135/tablea1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/660/A135/tablea1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/660/A135/tablea1?GETtext/xml+votable180.050000true0.853-29.9580.0055555555555555566/4298 6149 14336 14575 16490 20562 20763 20814 20939 20957 20989 21372 21519 21529 21550 21557 21567 21586 21719 22130 22216 22224 22239 22433 22499 22887 23612 23638 23745 23861 24322 24330 24344 28806 28823 29066 29728 30215 30308 30635 31812 32089 37279 37592 37867 37933 37971 38441 39356 41466 41613 41649 41678 41834 42153 42177 42374 42402 42464 42496 43034 43140https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/660/A135?format=asciiOpticaldefaultJ/A+A/660/A135/tablea1Metallicity of each cluster, galactocentric distance, age and abundance ratios (average ratios [s/H] and [s/Fe] of open clusters)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintGESFieldGaia ESO Field (cluster Name in the Gaia ESO catalogue)meta.id;meta.mainchar[Fe/H]Metallicity of each cluster from Randich et al. (2022, A&A, in prep.)phys.abundfloatAgeCluster age from Cantat-Gaudin et al. (2020, Cat. J/A+A/640/A1)Gyrtime.agefloatRgcCluster galactocentric distance from Cantat-Gaudin et al. (2020, Cat. J/A+A/640/A1)kpcpos.distance;pos.galactocentricfloat[YII/H]Solar scaled abundance [YII/H]phys.abundfloat[ZrI/H]? Solar scaled abundance [ZrI/H]phys.abundfloatnullable[BaII/H]? Solar scaled abundance [BaII/H]phys.abundfloatnullableSimbadNameSimbad column added by the CDSmeta.idcharnullable[LaII/H]? Solar scaled abundance [LaII/H]phys.abundfloatnullable[CeII/H]? Solar scaled abundance [CeII/H]phys.abundfloatnullable[YII/Fe]? Solar scaled abundance ratio [YII/Fe]phys.abund;arith.ratiofloatnullable[ZrI/Fe]? Solar scaled abundance ratio [ZrI/Fe]phys.abund;arith.ratiofloatnullable[BaII/Fe]? Solar scaled abundance ratio [BaII/Fe]phys.abund;arith.ratiofloatnullable[LaII/Fe]? Solar scaled abundance ratio [LaII/Fe]phys.abund;arith.ratiofloatnullable[CeII/Fe]? Solar scaled abundance ratio [CeII/Fe]phys.abund;arith.ratiofloatnullable_RARight Ascension (J2000) from SIMBAD (not part of the original data)degpos.eq.ra;meta.main_DEDeclination (J2000) from SIMBAD (not part of the original data)degpos.eq.dec;meta.main