J/A+A/699/A32ivo://CDS.VizieR/J/A+A/699/A32doi:10.26093/cds/vizier/bc-nv/ldcCDSKoutsouridou I.Skuladottir A.Salvadori S.2026-08-03T06:55:46Z2025-07-01T10:43:49ZCDS support team

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

cds-question@unistra.frpopulation-ii-starschemically-peculiar-starschemical-abundancesEarly chemical enrichment processes can be unveiled by the careful study of metal-poor stars. In our Local Group, we can obtain spectra of individual stars to measure their precise, but not always accurate, chemical abundances. Unfortunately, stellar abundances are typically estimated under the simplistic assumption of local thermodynamic equilibrium (LTE). This can systematically alter both the abundance patterns of individual stars and the global trends of chemical enrichment. The SAGA database compiles the largest catalogue of metal-poor stars in the Milky Way. For the first time, we provide the community with the SAGA catalogue fully corrected for non-LTE (NLTE) effects, using state-of-the-art publicly available grids. In addition, we present an easy-to-use online tool NLiTE that quickly provides NLTE corrections for large stellar samples. For further scientific exploration, NLiTE facilitates the comparison of different NLTE grids to investigate their intrinsic uncertainties. Finally, we compare the NLTE-SAGA catalogue with our cosmological galaxy formation and chemical evolution model, NEFERTITI. By accounting for NLTE effects, we can solve the long-standing discrepancy between models and observations in the abundance ratio of [C/Fe], which is the best tracer of the first stellar populations. At low [Fe/H]<-3.5, models were unable to reproduce the high measured [C/Fe] in LTE, which are lowered in NLTE, aligning with the simulations. Other elements are a mixed bag, where some show improved agreement with the models (e.g. Na) and other appear even worse (e.g. Co). Few elemental ratios do not change significantly (e.g. [Mg/Fe], [Ca/Fe]). Properly accounting for NLTE effects is fundamental for correctly interpreting the chemical abundances of metal-poor stars. Our new NLiTE tool, thus, enables a meaningful comparison of stellar samples with chemical and stellar evolution models as well as with low-metallicity gaseous environments at higher redshift.2025A&A...699A..32Khttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/699/A32CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/699/A32https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/699/A32http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/699/A32https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/699/A32https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/699/A32http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/699/A32GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/699/A32/table4 (Coordinates and stellar atmospheric parameters of all MP SAGA entries)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/699/A32/table4?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/699/A32/table4?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/699/A32/table4?GETtext/xml+votable180.050000true104.36237555.71989170.0055555555555555565/11676 6/0 24-25 30-31 51 98 118 143-144 146 154 207-208 232 241 253 337 368 373 377 382 428 488 524 643 697 712 763 783 796 798 800 815 822 872 893 971 1141 1147 1210 1224 1236 1285 1319 1435 1441 1468 1519 1533 1556 1642 1644 1701 1911 1971 2064 2067 2083 2087 2110 2133 2148 2180 2190 2249 2381 2398 2404 2426 2437 2463 2506 2513 2515 2545 2579 2599 2602 2638 2675 2707 2736-2737 2806 2838-2839 2850 2882 2921 2988-2989 2997 3005 3095 3099 3120 3267 3350 3494 3588 3654 3663 3712 3751 3825 3970 4057 4101 4103 4111 4129 4170 4184 4240 4253 4269 4282 4324 4376 4413 4421 4526 4598 4639 4694 4702 4705-4706 4714 4734 4750 4776 4783 4799 4821 4846 4854 4884 4901 4905 4909 4934 4948 4968 4974 5009 5012 5015 5036 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47476 47478 47483 47500 47502 47512 47518-47519 47530 47538 47540-47541 47544 47556 47558 47564 47589 47596 47608 47610 47625 47627 47630 47634 47636 47646 47649-47650 47654-47655 47659-47660 47666 47672 47674 47676 47698-47699 47749 47756 47776 47780-47781 47792 47799 47806 47819 47840 47851-47852 47869 47876 47940 47943 47954-47955 47987 48087 48129 48138 48142 48145 48153 48160 48162-48163 48173 48186 48221 48223 48234 48240 48246 48249 48256 48265 48281 48286 48289 48292 48358 48363 48375 48387-48388 48392 48394 48400 48436 48451 48481 48484-48485 48488 48501 48508-48509 48511 48514 48517-48518 48526 48534 48544 48555 48557 48577-48578 48588 48591 48603 48609 48613-48614 48625 48628 48631 48636 48641 48645 48648 48660 48666 48672 48674 48677 48695 48708 48711 48719-48720 48722 48728 48731 48734 48736 48744 48750 48752 48762 48764 48766 48798 48824 48848 48861-48862 48894 48916 48937 48946 48982 48998 49001 49004 49009 49011-49012 49019 49027 49063 49078 49081 49093 49103 49105 49124 49136 49149https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/699/A32?format=asciidefaultJ/A+A/699/A32/table1Spectral lines most commonly used in observations of MP stars, for which NLTE corrections are available in the literaturerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIonSpecies identifierphys.atmol.ionStagecharlambdaWavelength {lambda}; in {AA}0.1nmem.wlfloatJ/A+A/699/A32/table2NLTE-corrected abundances of all individual MP SAGA starsNameStar identifiermeta.id;meta.mainchar[Ti/Fe]? NLTE [Ti/Fe] abundance ratiophys.abundfloatnullablee_[Ti/Fe]? Uncertainty on [Ti/Fe]stat.error;phys.abundfloatnullablel_[TiI/Fe]? Limit flag for [TiI/Fe]meta.code.error;phys.abundchar[TiI/Fe]? NLTE [TiI/Fe] abundance ratiophys.abundfloatnullablel_[Mn/Fe]? Limit flag for [Mn/Fe]meta.code.error;phys.abundcharl_[Cu/Fe]? Limit flag for [Cu/Fe]meta.code.error;phys.abundcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintRefReference of the source papermeta.bibcharA(Li)? NLTE absolute Li abundancephys.abundfloatnullablee_A(Li)? Uncertainty on A(Li)stat.errorfloatnullablel_[C/Fe]? Limit flag for [C/Fe]meta.code.error;phys.abundchar[C/Fe]? NLTE [C/Fe] abundance ratio (1)phys.abundfloatnullablee_[C/Fe]? Uncertainty on [C/Fe]stat.error;phys.abundfloatnullablel_[CH/Fe]? Limit flag for [CH/Fe]meta.code.error;phys.abundchar[CH/Fe]? NLTE [CH/Fe] abundance ratio (1)phys.abundfloatnullablee_[CH/Fe]? Uncertainty on [CH/Fe]stat.error;phys.abundfloatnullablel_[CI/Fe]? Limit flag for [CI/Fe]meta.code.error;phys.abundchar[CI/Fe]? NLTE [CI/Fe] abundance ratio (1)phys.abundfloatnullablee_[CI/Fe]? Uncertainty on [CI/Fe]stat.error;phys.abundfloatnullablel_[N/Fe]LTE? Limit flag for [N/Fe]meta.code.error;phys.abundchar[N/Fe]LTE? LTE [N/Fe] abundance ratio (2)phys.abundfloatnullablee_[N/Fe]LTE? Uncertainty on [N/Fe]stat.error;phys.abundfloatnullable[O/Fe]? NLTE [O/Fe] abundance ratiophys.abundfloatnullablee_[O/Fe]? Uncertainty on [O/Fe]stat.error;phys.abundfloatnullablel_[Na/Fe]? Limit flag for [Na/Fe]meta.code.error;phys.abundchar[Na/Fe]? NLTE [Na/Fe] abundance ratiophys.abundfloatnullablee_[Na/Fe]? Uncertainty on [Na/Fe]stat.error;phys.abundfloatnullablel_[Mg/Fe]? Limit flag for [Mg/Fe]meta.code.error;phys.abundchar[Mg/Fe]? NLTE [Mg/Fe] abundance ratiophys.abundfloatnullablee_[Mg/Fe]? Uncertainty on [Mg/Fe]stat.error;phys.abundfloatnullablel_[Al/Fe]? Limit flag for [Al/Fe]meta.code.error;phys.abundchar[Al/Fe]? NLTE [Al/Fe] abundance ratiophys.abundfloatnullablee_[Al/Fe]? Uncertainty on [Al/Fe]stat.error;phys.abundfloatnullablel_[Si/Fe]? Limit flag for [Si/Fe]meta.code.error;phys.abundchar[Si/Fe]? NLTE [Si/Fe] abundance ratiophys.abundfloatnullablee_[Si/Fe]? Uncertainty on [Si/Fe]stat.error;phys.abundfloatnullable[S/Fe]LTE? LTE [S/Fe] abundance ratio (2)phys.abundfloatnullablee_[S/Fe]LTE? Uncertainty on [S/Fe]stat.error;phys.abundfloatnullablel_[K/Fe]? Limit flag for [K/Fe]meta.code.error;phys.abundchar[K/Fe]? NLTE [K/Fe] abundance ratiophys.abundfloatnullablee_[K/Fe]? Uncertainty on [K/Fe]stat.error;phys.abundfloatnullablel_[Ca/Fe]? Limit flag for [Ca/Fe]meta.code.error;phys.abundchar[Ca/Fe]? NLTE [Ca/Fe] abundance ratiophys.abundfloatnullablee_[Ca/Fe]? Uncertainty on [Ca/Fe]stat.error;phys.abundfloatnullablel_[Sc/Fe]LTE? Limit flag for [Sc/Fe]meta.code.error;phys.abundchar[Sc/Fe]LTE? LTE [Sc/Fe] abundance ratio (2)phys.abundfloatnullablee_[Sc/Fe]LTE? Uncertainty on [Sc/Fe]stat.error;phys.abundfloatnullablel_[Ti/Fe]? Limit flag for [Ti/Fe]meta.code.error;phys.abundchare_[TiI/Fe]? Uncertainty on [TiI/Fe]stat.error;phys.abundfloatnullablel_[TiII/Fe]? Limit flag for [TiII/Fe]meta.code.error;phys.abundchar[TiII/Fe]? NLTE [TiII/Fe] abundance ratiophys.abundfloatnullablee_[TiII/Fe]? Uncertainty on [TiII/Fe]stat.error;phys.abundfloatnullablel_[V/Fe]LTE? Limit flag for [V/Fe]meta.code.error;phys.abundchar[V/Fe]LTE? LTE [V/Fe] abundance ratio (2)phys.abundfloatnullablee_[V/Fe]LTE? Uncertainty on [V/Fe]stat.error;phys.abundfloatnullablel_[Cr/Fe]? Limit flag for [Cr/Fe]meta.code.error;phys.abundchar[Cr/Fe]? NLTE [Cr/Fe] abundance ratiophys.abundfloatnullablee_[Cr/Fe]? Uncertainty on [Cr/Fe]stat.error;phys.abundfloatnullable[Mn/Fe]? NLTE [Mn/Fe] abundance ratiophys.abundfloatnullablee_[Mn/Fe]? Uncertainty on [Mn/Fe]stat.error;phys.abundfloatnullablel_[Fe/H]? Limit flag for [Fe/H]meta.code.error;phys.abund.Fechar[Fe/H]? NLTE [Fe/H] abundance ratiophys.abund.Fe;arith.ratiofloatnullablee_[Fe/H]? Uncertainty on [Fe/H]stat.error;phys.abund.Fefloatnullablel_[FeI/H]? Limit flag for [FeI/H]meta.code.error;phys.abundchar[FeI/H]? NLTE [FeI/H] abundance ratiophys.abund;arith.ratiofloatnullablee_[FeI/H]? Uncertainty on [FeI/H]stat.error;phys.abundfloatnullablel_[FeII/H]? Limit flag for [FeII/H]meta.code.error;phys.abundchar[FeII/H]? NLTE [FeII/H] abundance ratiophys.abund;arith.ratiofloatnullablee_[FeII/H]? Uncertainty on [FeII/H]stat.error;phys.abundfloatnullable[Fe/H]LTE? LTE [Fe/H] abundance ratiophys.abund.Fe;arith.ratiofloatnullablel_[Co/Fe]? Limit flag for [Co/Fe]meta.code.error;phys.abundchar[Co/Fe]? NLTE [Co/Fe] abundance ratiophys.abundfloatnullablee_[Co/Fe]? Uncertainty on [Co/Fe]stat.error;phys.abundfloatnullablel_[Ni/Fe]LTE? Limit flag for [Ni/Fe]meta.code.error;phys.abundchar[Ni/Fe]LTE? LTE [Ni/Fe] abundance ratio (2)phys.abundfloatnullablee_[Ni/Fe]LTE? Uncertainty on [Ni/Fe]stat.error;phys.abundfloatnullable[Cu/Fe]? NLTE [Cu/Fe] abundance ratiophys.abundfloatnullablee_[Cu/Fe]? Uncertainty on [Cu/Fe]stat.error;phys.abundfloatnullablel_[Zn/Fe]? Limit flag for [Zn/Fe]meta.code.error;phys.abundchar[Zn/Fe]? NLTE [Zn/Fe] abundance ratiophys.abundfloatnullablee_[Zn/Fe]? Uncertainty on [Zn/Fe]stat.error;phys.abundfloatnullablel_[Sr/Fe]? Limit flag for [Sr/Fe]meta.code.error;phys.abundchar[Sr/Fe]? NLTE [Sr/Fe] abundance ratiophys.abundfloatnullablee_[Sr/Fe]? Uncertainty on [Sr/Fe]stat.error;phys.abundfloatnullablel_[Ba/Fe]? Limit flag for [Ba/Fe]meta.code.error;phys.abundchar[Ba/Fe]? NLTE [Ba/Fe] abundance ratiophys.abundfloatnullablee_[Ba/Fe]? Uncertainty on [Ba/Fe]stat.error;phys.abundfloatnullablel_[Eu/Fe]? Limit flag for [Eu/Fe]meta.code.error;phys.abundchar[Eu/Fe]? NLTE [Eu/Fe] abundance ratiophys.abundfloatnullablee_[Eu/Fe]? Uncertainty on [Eu/Fe]stat.error;phys.abundfloatnullablel_A(Li)? Limit flag for A(Li)meta.code.errorcharl_[O/Fe]? Limit flag for [O/Fe]meta.code.error;phys.abundcharl_[S/Fe]LTE? Limit flag for [S/Fe]meta.code.error;phys.abundcharJ/A+A/699/A32/table3Full details for our NLTE corrections for all MP entries in SAGA (multiple entries may correspond to the same star)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameStar identifiermeta.id;meta.maincharRefReference of the source papermeta.bibcharIonElement/species identifierphys.atmol.ionStagecharl_[X/H]LTELimit flag for [X/H]meta.code.error;phys.abundchar[X/H]LTE? LTE [X/H] abundance ratio (1)phys.abundfloatnullablee_[X/H]LTE? Uncertainty on [X/H]stat.error;phys.abundfloatnullableOCX[0/1]? Originally Corrected flag (2)meta.codeintnullableOWX[0/1]? Other Wavelengths flag (3)meta.codeintnullabled[X/H]NLTE? NLTE abundance correction (4)arith.factorfloatnullableingrid[X/H][0/1]? In Grid flag (5)meta.codeintnullables_d[X/H]NLTE? Standard deviation of the NLTE correctionarith.factorfloatnullableo_d[X/H]NLTE? Number of spectral lines used to compute NLTE correction (6)meta.numberintnullableLineTypeLine Type flag (7)src.morph.type;spect.linecharPlaccoCor? Placco evolutionary correction for carbon (8)arith.factorfloatnullableJ/A+A/699/A32/table4Coordinates and stellar atmospheric parameters of all MP SAGA entriesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameStar identifier (1)meta.id;meta.maincharRefReference of the source papermeta.bibcharRAJ2000Right Ascension (J2000)pos.eq.ra;meta.mainDEJ2000Declination (J2000)pos.eq.dec;meta.mainTeff? Effective temperatureKphys.temperature.effectivefloatnullablelogg? Surface gravitylog(cm.s**-2)phys.gravityfloatnullablel_[Fe/H]Limit flag for [Fe/H]meta.code.error;phys.abund.Fechar[Fe/H]? [Fe/H] abundance ratio (2)phys.abund.Fe;arith.ratiofloatnullablee_[Fe/H]? Uncertainty on [Fe/H]stat.error;phys.abund.FefloatnullableSAGAnameName of star in SAGA (3)meta.idchar