J/A+A/683/A73ivo://CDS.VizieR/J/A+A/683/A73doi:10.26093/cds/vizier.36830073CDSGuiglion G.Bergemann M.Storm N.Lian J.Cescutti G.Serenelli A.2024-11-29T20:01:22Z2024-03-08T12:25:41ZCDS support team

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

cds-question@unistra.frmilky-way-galaxyf-starschemical-abundancesspectroscopyThe chemical evolution history of slow neutron-capture elements in the Milky Way is still a matter of debate, especially in the metal-poor regime ([Fe/H]<-1). Based on Gaia-ESO spectroscopic data, a recent study investigated the chemical evolution of neutron-capture elements in the regime [Fe/H]>-1. Here, we aim to complement this study down to [Fe/H]=-3, and focus on Ba, Y, and Sr, along with the abundance ratios of [Ba/Y] and [Sr/Y], which give comprehensive views on s-process nucleosynthesis channels. We measured the local thermodynamic equilibrium (LTE) and non-local thermodynamic equilibrium (NLTE) abundances of Ba, Y, and Sr in 323 Galactic metal-poor stars using high-resolution optical spectra with high signal-to-noise ratios. We used the spectral fitting code TSFitPy together with 1D model atmospheres, using previously determined LTE and NLTE atmospheric parameters. We find that the NLTE effects are on the order of ~-0.1 to ~0.2dex, depending on the element. We find that stars enhanced(deficient) in [Ba/Fe] and [Y/Fe] are also enhanced(deficient) in [Sr/Fe], suggesting a common evolution channel for these three elements. We find that the ratio between heavy and light s-process elements [Ba/Y] varies weakly with [Fe/H] even in the metal-poor regime, which is consistent with the behaviour in the metal-rich regime. The [Ba/Y] scatter at a given metallicity is larger than the abundance measurement uncertainties. Homogeneous chemical evolution models with different yield prescriptions are not able to accurately reproduce the [Ba/Y] scatter in the low-[Fe/H] regime. Adopting the stochastic chemical evolution model by Cescutti & Chiappini (2014A&A...565A..51C) allows us to reproduce the observed scatter in the abundance pattern of [Ba/Y] and [Ba/Sr]. Based on our observations, we have ruled out the need for an arbitrary scaling of the r-process contribution, as previously suggested by the authors behind the construction of the model. We show how important it is to properly include NLTE effects when measuring chemical abundances, especially in the metal-poor regime. This work demonstrates that the choice of the Galactic chemical evolution model (stochastic versus one-zone) is key when comparing models to observations. Upcoming large-scale spectroscopic surveys such as 4MOST and WEAVE are poised to deliver high-quality data for many thousands of metal-poor stars and this work gives a typical case study of what could be achieved with such surveys in the future.2024A&A...683A..73Ghttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/683/A73CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/A+A/631/A80 : Mn lines 3D NLTE formation in late-type stars (Bergemann+ 2019)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/683/A73https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/683/A73http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/683/A73https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/683/A73https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/683/A73http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/683/A73GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/683/A73/abund (Catalogue of abundances)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/683/A73/abund?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/683/A73/abund?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/683/A73/abund?GETtext/xml+votable180.050000true5.8778306-16.52864420.0055555555555555566/16504 16586 16607 16764 16819 16828 16890 16907 16929 17033 17091 17127 17134 17234 17517 17556 17595 17618 17698 18606 18683 18952 18973 20538 20623 20635 20882 21126 21202 21228-21229 21241 22564 23043 23304 24602 24607 24618 24636 24644 24663 24668 24675 24717 24750 24887 24986 24994 25061 25074 25098 25126 25139 25158 25167 25197 25207 25297 25318 25327 25350 25394 25400 25405 25520 25595 25608 25614 25618 25622 25624 25635 25652 25696 25767 25786 25857 25873 25893 25938 25990 26145 26168 26241 26669 26720 26722 26725 26728 26730 26739 26764 26767 26827 26925 26927 27016 27182 30761 30778 30857 30923 30962 31117 31249 32894 33030 33051 33121 33142 33207 33366 33446 33521 33523 33720 33724 33750 33877 33885 34141 34260 34276 34427 34478 34493 34570 34588 34610 34908 34935 34939 35084 35090 35112 35234 35267 35288 35359 35381 35649 35760 35857 35927 35947 36002 36082 36105 36172 36263 36316 36336 36446 36467 36486 36501 36728 36783 36842 36995 37543 37551 38218 38303 38336 38639 38683 38772 38775 38779-38780 38851 39084 39188 39443 39490 39653 39707 39817 39847 39866 40046 40133 40270 40278 40313 40337 40498 40911 41029 43248 43307 43487 43508 43577 43619 43629 43663 43862 43905 43950 43976 43992 44002 44006 44208 44260 44279 44458 44478 44552 44641 44661 44701 44754 44780 44817 44825 44830 44841 44847 44851-44852 44890 44901 44906 44923 44960 45019 45037 45097 45185 45199 45216 45408 45595 45622 45640 45658 45714 45748 45764 45786 45804 45807 45857 45954 46023 46167 46203 46250 46273 46324 46370 46418 46633 46666 46696 46706 46806 46942 46987 47094 47168 47191 47201 47223 47226 47325 47373 47379 47387 47400 47447 47544 47564 47589 47711 47895 47940 47954 47967 48163 48171 48186 48246 48256 48272 48281 48358 48436 48588 48609 48641 48648 48672 48676-48677 48694 48749-48752 48861 49093 49103 49124https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/683/A73?format=asciidefaultJ/A+A/683/A73/abundCatalogue of abundancesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIDTarget IDmeta.id;meta.mainchar[Fe/H]LTELTE [Fe/H] ratiophys.abund.Fe;arith.ratiofloat[Fe/H]NLTENLTE [Fe/H] ratiophys.abund.Fe;arith.ratiofloat[Ba/Fe]LTE? Abundance ratio [Ba/Fe] in LTEphys.abundfloatnullablee_[Ba/Fe]LTE? Uncertainty on LTE [Ba/Fe]stat.error;phys.abundfloatnullable[Ba/Fe]NLTE? Abundance ratio [Ba/Fe] in NLTEphys.abundfloatnullablee_[Ba/Fe]NLTE? Uncertainty on NLTE [Ba/Fe]stat.error;phys.abundfloatnullable[Sr/Fe]LTE? Abundance ratio [Sr/Fe] in LTEphys.abundfloatnullablee_[Sr/Fe]LTE? Uncertainty on LTE [Sr/Fe]stat.error;phys.abundfloatnullable[Sr/Fe]NLTE? Abundance ratio [Sr/Fe] in NLTEphys.abundfloatnullablee_[Sr/Fe]NLTE? Uncertainty on NLTE [Sr/Fe]stat.error;phys.abundfloatnullable[Y/Fe]LTE? Abundance ratio [Y/Fe] in LTEphys.abundfloatnullablee_[Y/Fe]LTE? Uncertainty on LTE [Y/Fe]stat.error;phys.abundfloatnullable[Y/Fe]NLTE? Abundance ratio [Y/Fe] in NLTEphys.abundfloatnullablee_[Y/Fe]NLTE? Uncertainty on NLTE [Y/Fe]stat.error;phys.abundfloatnullable[Ba/Fe]LTE5853? Abundance ratio [Ba/Fe] in LTE from line at 5853{AA}phys.abundfloatnullable[Ba/Fe]LTE6141? Abundance ratio [Ba/Fe] in LTE from line at 6141{AA}phys.abundfloatnullable[Ba/Fe]LTE6496? Abundance ratio [Ba/Fe] in LTE from line at 6496{AA}phys.abundfloatnullable[Ba/Fe]NLTE5853? Abundance ratio [Ba/Fe] in NLTE from line at 5853{AA}phys.abundfloatnullable[Ba/Fe]NLTE6141? Abundance ratio [Ba/Fe] in NLTE from line at 6141{AA}phys.abundfloatnullable[Ba/Fe]NLTE6496? Abundance ratio [Ba/Fe] in NLTE from line at 6496{AA}phys.abundfloatnullable[Y/Fe]LTE4883? Abundance ratio [Y/Fe] in LTE from line at 4883{AA}phys.abundfloatnullable[Y/Fe]LTE5087? Abundance ratio [Y/Fe] in LTE from line at 5087{AA}phys.abundfloatnullableSimbadNameSimbad column added by the CDSmeta.idcharnullable[Y/Fe]NLTE4883? Abundance ratio [Y/Fe] in NLTE from line at 4883{AA}phys.abundfloatnullable[Y/Fe]NLTE5087? Abundance ratio [Y/Fe] in NLTE from line at 5087{AA}phys.abundfloatnullable_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