J/A+A/652/A25ivo://CDS.VizieR/J/A+A/652/A25doi:10.26093/cds/vizier.36520025CDSCasamiquela L.Soubiran C.Jofre P.Chiappini C.Lagarde N.,Tarricq Y.Carrera R.Jordi C.Balaguer-Nunez L.Carbajo-Hijarrubia J.,Blanco-Cuaresma S.2022-12-31T09:44:41Z2021-08-05T08:59:12ZCDS support team

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

cds-question@unistra.frmilky-way-galaxyopen-star-clusterschemical-abundancesPrecise chemical abundances coupled with reliable ages are key ingredients to understand the chemical history of our Galaxy. Open Clusters (OCs) are useful for this purpose because they provide ages with good precision. The aim of this work is to investigate the relations of different chemical abundance ratios vs age traced by red clump (RC) stars in OCs. We analyze a large sample of "NGoodstars" reliable members in "NClusters" OCs with available high-resolution spectroscopy. We applied a differential line-by-line analysis to provide a comprehensive chemical study of "NElements" chemical species. This sample is among the largest samples of OCs homogeneously characterized in terms of atmospheric parameters, detailed chemistry, and ages. In our metallicity range (-0.2<[M/H]<+0.2) we find that while most Fe-peak and {alpha} elements have flat dependence with age, the s-process elements show decreasing trends with increasing age with a remarkable knee at 1Gyr. For Ba, Ce, Y, Mo and Zr we find a plateau at young ages (<1Gyr). We investigate the relations of all possible combinations among the computed chemical species with age. We find 19 combinations with significant slopes, including [Y/Mg] and [Y/Al]. The ratio [Ba/{alpha}] is the one with the most significant correlations found. We find that the [Y/Mg] relation found in the literature using Solar twins is compatible with the one found here in the Solar neighbourhood. The age-abundance relations show larger scatter for clusters at large distances (d>1kpc) than for the Solar neighbourhood, particularly in the outer disk. We conclude that these relations need to be understood also in terms of the complexity of the chemical space introduced by the Galactic dynamics, on top of pure nucleosynthetic arguments, especially out of the local bubble.2021A&A...652A..25Chttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/652/A25CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toI/345 : Gaia DR2 (Gaia Collaboration, 2018)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/652/A25https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/652/A25http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/652/A25https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/652/A25https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/652/A25http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/652/A25GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/652/A25/tablea2 (Mean cluster abundances)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/652/A25/tablea2?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/652/A25/tablea2?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/652/A25/tablea2?GETtext/xml+votable180.050000true283.77212.34280560.0055555555555555566/1302 1509 2436 3063 3242 4078 4298 4698 6149 6760 13198 14134 14175 14246 14363 14575 14730 14752 15121 15369 15396 15497 15595 15709 15759 21602 22053 22499 23410 23538 24057 24121 24361 24522 28711 29109 29154 29728 29868 30215 30439 31812 32016 37933 39912 40696 42464https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/652/A25?format=asciidefaultJ/A+A/652/A25/tablea2Mean cluster abundancesRgcGalactocentric radiuspcphys.size.radius;pos.galactocentricfloatrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordinte_[Al/H]rms uncertainty on abundance [Al/H]stat.error;phys.abundfloat[Mo/H]? Mean value of cluster the abundance [Mo/H]phys.abundfloatnullableSimbadNameSimbad column added by the CDSmeta.idcharnullable_RAfrom Simbad (right ascension part)degpos.eq.ra;meta.mainDistHeliocentric distancepcpos.distancefloatZHeight above the planepcpos.cartesian.z;pos.galacticfloatageCluster ageGyrtime.agefloate_ageCluster age uncertaintyGyrstat.error;time.agefloatNstarsNumber of stars analysed for the clustermeta.numberfloat[Na/H]Mean value of cluster the sodium abundance [Na/H]phys.abundfloate_[Na/H]rms uncertainty in the cluster sodium abundance [Na/H]stat.error;phys.abundfloato_[Na/H]Number of stars used to derive the mean abundance [Na/H]meta.numberfloat[Al/H]Mean value of cluster the abundance [Al/H]phys.abundfloato_[Al/H]Number of stars used to derive the mean abundance [Al/H]meta.numberfloat[Mg/H]Mean value of cluster the abundance [Mg/H]phys.abundfloate_[Mg/H]rms uncertainty on abundance [Mg/H]stat.error;phys.abundfloato_[Mg/H]Number of stars used to derive the mean abundance [Mg/H]meta.numberfloat[Si/H]Mean value of cluster the abundance [Si/H]phys.abundfloate_[Si/H]rms uncertainty on abundance [Si/H]stat.error;phys.abundfloato_[Si/H]Number of stars used to derive the mean abundance [Si/H]meta.numberfloat[Ca/H]Mean value of cluster the abundance [Ca/H]phys.abundfloate_[Ca/H]rms uncertainty on abundance [Ca/H]stat.error;phys.abundfloato_[Ca/H]Number of stars used to derive the mean abundance [Ca/H]meta.numberfloat[Sc/H]Mean value of cluster the abundance [Sc/H]phys.abundfloate_[Sc/H]rms uncertainty on abundance [Sc/H]stat.error;phys.abundfloato_[Sc/H]Number of stars used to derive the mean abundance [Sc/H]meta.numberfloat[Ti/H]Mean value of cluster the abundance [Ti/H]phys.abundfloate_[Ti/H]rms uncertainty on abundance [Ti/H]stat.error;phys.abundfloato_[Ti/H]Number of stars used to derive the mean abundance [Ti/H]meta.numberfloat[V/H]Mean value of cluster the abundance [V/H]phys.abundfloate_[V/H]rms uncertainty on abundance [V/H]stat.error;phys.abundfloato_[V/H]Number of stars used to derive the mean abundance [V/H]meta.numberfloat[Cr/H]Mean value of cluster the abundance [Cr/H]phys.abundfloate_[Cr/H]rms uncertainty on abundance [Cr/H]stat.error;phys.abundfloato_[Cr/H]Number of stars used to derive the mean abundance [Cr/H]meta.numberfloat[Mn/H]Mean value of cluster the abundance [Mn/H]phys.abundfloate_[Mn/H]rms uncertainty on abundance [Mn/H]stat.error;phys.abundfloato_[Mn/H]Number of stars used to derive the mean abundance [Mn/H]meta.numberfloat[Fe/H]Mean value of cluster the abundance [Fe/H]phys.abund.Fefloate_[Fe/H]rms uncertainty on abundance [Fe/H]stat.error;phys.abund.Fefloato_[Fe/H]Number of stars used to derive the mean abundance [Fe/H]meta.numberfloat[Co/H]Mean value of cluster the abundance [Co/H]phys.abundfloate_[Co/H]rms uncertainty on abundance [Co/H]stat.error;phys.abundfloato_[Co/H]Number of stars used to derive the mean abundance [Co/H]meta.numberfloat[Ni/H]Mean value of cluster the abundance [Ni/H]phys.abundfloate_[Ni/H]rms uncertainty on abundance [Ni/H]stat.error;phys.abundfloato_[Ni/H]Number of stars used to derive the mean abundance [Ni/H]meta.numberfloat[Cu/H]Mean value of cluster the abundance [Cu/H]phys.abundfloate_[Cu/H]rms uncertainty on abundance [Cu/H]stat.error;phys.abundfloato_[Cu/H]Number of stars used to derive the mean abundance [Cu/H]meta.numberfloat[Zn/H]? Mean value of cluster the abundance [Zn/H]phys.abundfloatnullablee_[Zn/H]? rms uncertainty on abundance [Zn/H]stat.error;phys.abundfloatnullableo_[Zn/H]? Number of stars used to derive the mean abundance [Zn/H]meta.numberfloatnullable[Y/H]Mean value of cluster the abundance [Y/H]phys.abundfloate_[Y/H]rms uncertainty on abundance [Y/H]stat.error;phys.abundfloato_[Y/H]Number of stars used to derive the mean abundance [Y/H]meta.numberfloat[Zr/H]? Mean value of cluster the abundance [Zr/H]phys.abundfloatnullablee_[Zr/H]? rms uncertainty on abundance [Zr/H]stat.error;phys.abundfloatnullableo_[Zr/H]? Number of stars used to derive the mean abundance [Zr/H]meta.numberfloatnullablee_[Mo/H]? rms uncertainty on abundance [Mo/H]stat.error;phys.abundfloatnullableo_[Mo/H]? Number of stars used to derive the mean abundance [Mo/H]meta.numberfloatnullable[Ba/H]Mean value of cluster the abundance [Ba/H]phys.abundfloate_[Ba/H]rms uncertainty on abundance [Ba/H]stat.error;phys.abundfloato_[Ba/H]Number of stars used to derive the mean abundance [Ba/H]meta.numberfloat[Ce/H]Mean value of cluster the abundance [Ce/H]phys.abundfloate_[Ce/H]rms uncertainty on abundance [Ce/H]stat.error;phys.abundfloato_[Ce/H]Number of stars used to derive the mean abundance [Ce/H]meta.numberfloat[Pr/H]? Mean value of cluster the abundance [Pr/H]phys.abundfloatnullablee_[Pr/H]? rms uncertainty on abundance [Pr/H]stat.error;phys.abundfloatnullableo_[Pr/H]? Number of stars used to derive the mean abundance [Pr/H]meta.numberfloatnullable[Nd/H]? Mean value of cluster the abundance [Nd/H]phys.abundfloatnullablee_[Nd/H]? rms uncertainty on abundance [Nd//Hstat.error;phys.abundfloatnullableo_[Nd/H]? Number of stars used to derive the mean abundance [Nd/H]meta.numberfloatnullable_DEfrom Simbad (declination part)degpos.eq.dec;meta.mainClusterCluster namemeta.id;meta.maincharJ/A+A/652/A25/tablea1Details of the used spectrarecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintClusterCluster namemeta.id;meta.maincharGaiaDR2Gaia DR2 source ID of the starmeta.idInstInstrument usedinstr.setupcharoriginOrigin of the spectrum (archive/own observations)meta.ref;obscharsnrSignal-to-noise ratio of the spectrumstat.snrfloat