Large databases of metal-poor stars corrected for three-dimensional and/or non-local thermodynamic equilibrium effects

TL;DR

This paper provides a comprehensive correction of metal-poor star abundances for non-LTE effects, improving the accuracy of chemical evolution studies and enabling better comparisons with galaxy formation models.

Contribution

It introduces the fully corrected NLTE SAGA catalogue and the NLiTE online tool for rapid NLTE abundance corrections, advancing stellar chemical analysis.

Findings

NLTE corrections reconcile observed [C/Fe] with models at low metallicity.

Some elemental abundance ratios are significantly affected by NLTE corrections.

NLTE effects are crucial for accurate interpretation of metal-poor star abundances.

Abstract

Early chemical enrichment processes can be revealed 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 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], the best tracer of the first stellar populations. At low [Fe/H]<-3.5, models are unable to reproduce the high measured [C/Fe] in LTE, which are lowered in NLTE, aligning with simulations. Other elements are a mixed bag: some show improved agreement with models (e.g. Na) and others 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 interpreting the chemical abundances of metal-poor stars. Our NLiTE tool thus enables a meaningful comparison of stellar samples with stellar and chemical evolution models and low-metallicity gaseous environments at higher redshift.