J/A+A/682/A116ivo://CDS.VizieR/J/A+A/682/A116doi:10.26093/cds/vizier.36820116CDSNissen P.E.Amarsi A.M.Skuladottir A.Schuster W.J.2024-11-28T20:06:09Z2024-02-08T08:56:32ZCDS support team

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

cds-question@unistra.frmilky-way-galaxystellar-populationschemical-abundancesStudies of the element abundances and kinematics of stars belonging to the Galactic halo have revealed the existence of two distinct populations: accreted stars with a low [alpha/Fe] ratio and in situ born stars with a higher ratio. Previous work on the abundances of C, O, Na, Mg, Si, Ca, Ti, Cr, Mn, Fe, Ni, Cu, and Zn in high-alpha and low-alpha halo stars is extended to include the abundances of Sc, V, and Co, enabling us to study the nucleosynthesis of all iron-peak elements along with the lighter elements. The Sc, V, and Co abundances were determined from a 1D MARCS model-atmosphere analysis of equivalent widths of atomic lines in high signal-to-noise, high resolution spectra assuming local thermodynamic equilibrium (LTE). In addition, new 3D and/or non-LTE calculations were used to correct the 1D LTE abundances for several elements including consistent 3D non-LTE calculations for Mg. The two populations of accreted and in situ born stars are well separated in diagrams showing [Sc/Fe], [V/Fe], and [Co/Fe] as a function of [Fe/H]. The [X/Mg] versus [Mg/H] trends for high-alpha and low-alpha stars were used to determine the yields of core-collapse and Type Ia supernovae. The largest Type Ia contribution occurs for Cr, Mn, and Fe, whereas Cu is a pure core-collapse element. Sc, Ti, V, Co, Ni, and Zn represent intermediate cases. A comparison with yields calculated for supernova models shows poor agreement for the core-collapse yields. The Ia yields suggest that sub-Chandrasekhar-mass Type Ia supernovae provide a dominant contribution to the chemical evolution of the host galaxies of the low-alpha stars. A substructure in the abundances and kinematics of the low-alpha stars suggests that they arise from at least two different satellite accretion events, Gaia-Sausage-Enceladus and Thamnos.2024A&A...682A.116Nhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/682/A116CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/A+A/568/A25 : C and O abundances in stellar populations (Nissen+, 2014)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/682/A116https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/682/A116http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/682/A116https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/682/A116https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/682/A116http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/682/A116GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/682/A116/tablea1 (Stellar parameters and abundances)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/682/A116/tablea1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/682/A116/tablea1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/682/A116/tablea1?GETtext/xml+votable180.050000true178.8685756-22.38703470.0055555555555555566/200 208 373 436 488 953 1053 1425 1614 4603 5413 5622 6681 7286 7334 8235 9537 9831 10313 12451 12793 13162 13348 17136 17245 17332 17726 17782 18053 19347 19385 21926 22118 22754 22909 23015 23096 23978 24442 24775 24824 24827 24942 25444 27162 27323 27394 27826 27975 27991 28258 28265 28459 29490 29596 29765 30196 30233 30296 30359 31470 31503 31874 32100 32335 33273 33508 37232 38072 38288 38986 39157 39647 39692 40716 40924 41721 43310 43641 44281 44653 46053 48394 48736https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/682/A116?format=asciidefaultJ/A+A/682/A116/tablea1Stellar parameters and abundancesSimbadNameSimbad column added by the CDSmeta.idcharnullablerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintStarName of starmeta.id;meta.maincharTeffEffective temperatureKphys.temperature.effectiveintloggLogarithm of surface gravitylog(cm.s**-2)phys.gravityfloat[Fe/H]1D1D LTE iron abundancelog(Sun)phys.abund.FefloatVturbMicroturbulence velocitykm/sphys.veloc.microTurbfloat[C/H]? 3D non-LTE carbon abundance (1)log(Sun)phys.abundfloatnullable[O/H]? 3D non-LTE oxygen abundance (1)log(Sun)phys.abundfloatnullable[Na/H]1D non-LTE sodium abundancelog(Sun)phys.abundfloat[Na/H]cor1D non-LTE sodium abundance correctionlog(Sun)phys.abund;arith.difffloat[Mg/H]3D non-LTE magnesium abundancelog(Sun)phys.abundfloat[Mg/H]cor3D non-LTE magnesium abundance correctionlog(Sun)phys.abund;arith.difffloat[Si/H]1D non-LTE silicon abundancelog(Sun)phys.abundfloat[Si/H]cor1D non-LTE silicon abundance correctionlog(Sun)phys.abund;arith.difffloat[Ca/H]1D non-LTE calcium abundancelog(Sun)phys.abundfloat[Ca/H]cor1D non-LTE calcium abundance correctionlog(Sun)phys.abund;arith.difffloat[Sc/H]1D LTE scandium abundancelog(Sun)phys.abundfloat[Ti/H]1D LTE titanium abundancelog(Sun)phys.abundfloat[V/H]? 1D LTE vanadium abundance (1)log(Sun)phys.abundfloatnullable[Cr/H]1D LTE chromium abundancelog(Sun)phys.abundfloat[Mn/H]1D non-LTE manganese abundancelog(Sun)phys.abundfloat[Mn/H]cor1D non-LTE manganese abundance correctionlog(Sun)phys.abund;arith.difffloat[Fe/H]3D3D LTE iron abundancelog(Sun)phys.abund.Fefloat[Co/H]? 1D LTE cobalt abundance (1)log(Sun)phys.abundfloatnullable[Ni/H]1D LTE nickel abundancelog(Sun)phys.abundfloat[Cu/H]? 1D non-LTE copper abundance (1)log(Sun)phys.abundfloatnullable[Zn/H]1D LTE zinc abundancelog(Sun)phys.abundfloatPop[1/3] Population assigned in the paper (2)meta.codeintBinInformation on binarity (3)meta.code.classchar_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