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Carbon, oxygen, and iron abundances in disk and halo stars. Implications of 3D non-LTE spectral line formation

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Pith's one-line read Corrected abundances show C/O falling steadily in metal-poor stars

desk verdict This paper resets the baseline for C/O trends with the first 3D non-LTE grids for C I and 3D LTE grids for Fe II, and the central conclusion is probably right, but the metal-poor C I corrections rest on UV pumping that is only indirectly validated. read the letter →

arxiv 1908.10319 v2 pith:W7ZH42MC submitted 2019-08-27 astro-ph.SR

A. M. Amarsi , P. E. Nissen , Á. Skúladóttir This is my paper · ORCID
classification astro-ph.SR
keywords 3Dnon-LTEabundancecorrectionscarbonoxygenironGalacticchemicalevolutionFGKdwarfsC/Oratio
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The reading

Standard spectroscopic analyses of late-type stars assume one-dimensional, hydrostatic atmospheres in local thermodynamic equilibrium (1D LTE), and this paper argues that those assumptions bias carbon and oxygen abundances in ways that change the story of the Milky Way. Using 3D hydrodynamic model atmospheres and non-LTE line formation, the authors compute abundance corrections that reach $-0.3$ dex for C I in low-metallicity F dwarfs and $-0.6$ dex for O I in high-metallicity F dwarfs. Applied to 187 disk and halo dwarfs, the corrections reduce scatter and replace the 1D LTE turnover in $[C/O]$ at $[O/H]\approx -1$ with a monotonic decline to a plateau near $[C/O]\approx -0.6$. The result matters because C and O abundances are used as nucleosynthesis tracers and as inputs to exoplanet host-star characterisation; the paper also finds that thin-disk stars with confirmed planets show higher C/O at fixed $[O/H]$, a signature invisible before correction.

What carries the argument

The departure coefficients $\beta = n_{NLTE}/n_{LTE}$ computed for the levels of C I and O I in 3D model atmospheres. Two competing mechanisms set them: at high metallicity, photon losses in strong permitted lines drain level populations and strengthen the lines; at low metallicity, UV photons between 160 and 250 nm pump C I low-excitation levels into intermediate levels, overpopulating them and again strengthening lines. The abundance correction $\Delta = \log\epsilon_{3D,NLTE} - \log\epsilon_{1D,LTE}$ for each line carries these effects into abundance space.

What would settle it

Measure abundances of a metal-poor F dwarf ($T_{\rm eff}\approx 6000$ K, $[Fe/H]\approx -2$) from the permitted C I 940.6 nm and O I 777 nm lines and from the forbidden $[C I]$ 872.7 nm and $[O I]$ 630.0 nm lines; the 3D non-LTE corrections predict that both sets agree after correction, whereas 1D LTE predicts offsets of several tenths of a dex. A direct test is also possible from solar observations: compare predicted and observed center-to-limb behaviour of the UV C I lines around 160-250 nm.

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Extended reading notes

Core claim

Using 3D hydrodynamic model atmospheres and non-LTE statistical equilibrium for C I and O I, the paper computes line-by-line abundance corrections relative to the standard 1D LTE approximation. The corrections are negative almost everywhere: up to $-0.3$ dex for C I in low-metallicity F dwarfs and $-0.6$ dex for O I in high-metallicity F dwarfs, with Fe II corrections below $+0.15$ dex. Applied to 187 F and G dwarfs, they reduce scatter in $[C/Fe]$, $[O/Fe]$, and $[C/O]$, and change the mean trends: the 1D LTE turnover in $[C/O]$ at $[O/H]\approx -1$ disappears, replaced by a monotonic decrease to a plateau of $[C/O]\approx -0.6$ below $[O/H]\approx -1$. The paper concludes that the previously reported minimum is a line-formation artifact, not a nucleosynthesis signature, and that thin-disk stars with confirmed planets have higher C/O at fixed $[O/H]$.

Load-bearing premise

The correction grids are only as good as the atomic data, specifically the ab initio inelastic hydrogen and electron collision cross-sections and the UV line opacities in the atomic models, and these are validated only against solar disk-centre-to-limb measurements, not against metal-poor stars.

Editorial extensions

If this is right

  • Galactic chemical evolution conclusions for C and O in FGK dwarfs shift: plateau values of $[O/Fe]\approx 0.6$ and the monotonic $[C/O]$ trend supersede the 1D LTE picture.
  • The public correction grids make it cheap to upgrade abundances in large surveys, including planned and ongoing surveys of more than $10^6$ stars, from 1D LTE values.
  • For permitted C I and O I lines, 1D non-LTE modelling should replace 1D LTE when 3D non-LTE is unavailable, since 3D effects mostly enhance non-LTE effects.
  • The apparent C/O-planet connection is only visible after the corrections; this motivates using corrected abundances in exoplanet host-star characterisation.
  • Stellar ages based on isochrones are expected to change, since C and O influence CNO burning and interior opacity.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • If CH-line 3D LTE corrections are as severe as $-1$ dex, as the paper notes, the reported fraction of carbon-enhanced metal-poor stars in the Galaxy may be substantially overestimated by 1D LTE analyses.
  • The same correction logic should apply to oxygen in dwarf satellite galaxies; applying it to those stellar populations would make the comparison with the low-$\alpha$ halo more direct.
  • Because differential O I corrections relative to the Sun become positive at low metallicity, $[O/Fe]$ and $[C/O]$ trends from any survey that uses 1D LTE with a solar reference will be systematically tilted; this paper's grids quantify that tilt.
  • One could test the mechanism's extrapolation by checking whether ultraviolet pumping of C I is similarly strong in hotter subgiants, where the corrections are predicted to grow.
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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

2 major / 6 minor

Summary. The manuscript presents 3D non-LTE abundance correction grids for C I and O I lines and 3D LTE grids for Fe II lines, computed on the STAGGER grid of hydrodynamic model atmospheres, and applies these corrections to 1D LTE literature abundances of 187 F and G dwarfs in the Milky Way disk and halo. The corrections reach about -0.3 dex for C I lines in low-metallicity F dwarfs and about -0.6 dex for O I lines in high-metallicity F dwarfs. After correction, the authors report reduced scatter in abundance trends, a monotonic decrease of [C/O] with [O/H] down to a plateau near [C/O] ≈ -0.6, and a tentative enhancement of C/O among planet-hosting thin-disk stars. The correction grids are made publicly available.

Significance. If the corrections are accurate, this is a valuable contribution: it provides a reusable grid of line-by-line abundance corrections for late-type stars, demonstrates the impact of 3D non-LTE effects on Galactic chemical evolution trends, and offers a falsifiable prediction that removes the need for exotic nucleosynthesis to explain the [C/O] turnover at [O/H] ≈ -1. Strengths include the use of ab initio inelastic collision data, solar centre-to-limb validation of the atomic models, public release of the correction grids, and a careful re-analysis of a homogeneous literature sample. The central risk is that the low-metallicity C I corrections, which set the [C/O] plateau, rest on a UV pumping mechanism not directly validated outside the solar photon-loss regime.

major comments (2)
  1. [Sect. 3.1.1 and Sect. 5.5] The low-metallicity C I corrections that drive the claimed [C/O] plateau rely on non-thermal UV photon pumping through C I lines near 160-250 nm, as described in Sect. 3.1.1. The only external test cited (Sect. 1; Amarsi et al. 2019a) is solar centre-to-limb variation, which probes the high-metallicity photon-loss regime rather than the metal-poor pumping regime. The pumping rate depends on background UV opacities and on inelastic H-collision rates that are not directly benchmarked at [Fe/H] ≈ -2 to -3. A systematic error of order 0.1-0.2 dex in these corrections would alter the slope and plateau level of [C/O] versus [O/H] and could restore the 1D LTE turnover at [O/H] ≈ -1. The authors should present a sensitivity test (for example, varying the inelastic H-collision rates or the UV background opacities within plausible bounds) and report the resulting spread in the final abundance trends.
  2. [Sect. 4.2 and Sect. 5.5] The stellar parameters used to apply the correction grids are adopted from 1D LTE analyses (Sect. 4.2) and are not re-derived self-consistently under the 3D non-LTE line formation models. For the UVES-FIES sample, Teff and log g come from differential 1D LTE analyses of Fe I and Fe II lines; Sect. 4.3 discusses only the surface-gravity side and shows that 0.1 dex uncertainties in log g have a small effect. However, the effective temperature also enters the interpolated corrections, and given that Fe I lines are subject to 3D non-LTE effects (as argued in Sect. 4.3), a Teff bias of order 100 K is not excluded. Such a bias changes the low-metallicity C I corrections by a few hundredths of a dex (Fig. 5) and, more importantly, changes the differential correction between the Sun and metal-poor stars. The authors should quantify the sensitivity of the final [C/O] versus [O/H] trend to correlated shifts in Teff, log g, and [Fe/H], or re-derive parameters for a subset of stars using 3D non-LTE Fe II and C I lines.
minor comments (6)
  1. [Sect. 3.2.4] The text states that the 3D LTE versus 1D LTE abundance corrections for Fe II lines are 'positive' but then gives a typical range that includes -0.05 dex for lines of intermediate excitation potential; please reconcile these statements.
  2. [Sect. 3.1.1] The sentence beginning 'Non-thermal UV photons pump...' is a run-on after the preceding clause and should be broken into a separate sentence.
  3. [Sect. 5.4] In the text 'C /O2 versus [O/H]' should read 'C/O versus [O/H]'.
  4. [Fig. 2 caption and Sect. 2.1.3] The parameter written as '3conv' appears to be a typo for the mixing-length parameter (likely αconv); please correct it in the figure caption and text.
  5. [Throughout] The formatting of chemical species is inconsistent, with 'Ci', 'Oi', and 'Feii' appearing in several places; please use 'C I', 'O I', and 'Fe II' consistently.
  6. [Sect. 6] The citation 'Amarsi et al. 2019b' in the final paragraph should include a comma after 'al.'.

Circularity Check

0 steps flagged · score 0.0 of 10

No circularity: the abundance corrections are forward model predictions benchmarked externally, and the stellar abundance trends are outputs rather than fitted inputs.

full rationale

The paper's core claim is the set of 3D non-LTE versus 1D LTE abundance corrections defined in Eq. 1 and the resulting C, O, Fe abundance trends in Sect. 5. These corrections are computed from radiative transfer on STAGGER-grid model atmospheres using C I and O I atomic models with ab initio collisional data cited from prior work (Amarsi et al. 2018a, 2019a); they are not fitted to the 187-star sample or to any adopted [C/Fe], [O/Fe], or [C/O] trend. The re-analysis in Sect. 4 simply interpolates these precomputed correction grids and applies them to literature 1D LTE abundances, with no feedback from the resulting abundances into the models. The claimed monotonic decrease of [C/O] to a plateau near -0.6 (Sect. 5.5 and Conclusion) is a consequence of the differential corrections, not an input to them. The self-citations that provide the atomic models are supported by independent solar center-to-limb variation measurements, which are an external benchmark and do not depend on the stellar sample or the derived Galactic chemical evolution trends. The skeptic's concern that low-metallicity C I corrections are driven by UV pumping that is not directly validated outside the Sun is a legitimate accuracy/robustness limitation, but it is not circularity: the magnitude and metallicity dependence of the corrections are not tuned to reproduce the observed stellar abundance patterns. Therefore no step in the derivation chain reduces to its own inputs by construction.

Assumptions & free parameters 1 free parameters · 4 assumptions · 0 invented entities

The central contribution is model-based: abundance corrections are computed from 3D non-LTE radiative transfer with no new particles or forces. The load-bearing assumptions are the fidelity of the STAGGER 3D atmospheres, the accuracy of the inelastic collision data and atomic models, and the inherited Fe II LTE approximation. The only explicit hand-chosen numerical parameter is the Unsöld broadening enhancement factor.

free parameters (1)
  • Unsöld broadening enhancement factor = 2.0 for C I and O I; 1.5 for Fe II
    Hand-chosen multiplicative factor applied to Unsöld (1955) pressure broadening for lines outside the ABO tables (Sect. 2.3). Affects line wings and hence abundance corrections; not derived or fitted here.
assumptions (4)
  • domain assumption 3D hydrodynamic STAGGER-grid model atmospheres represent the real atmospheres of late-type stars more accurately than 1D hydrostatic models.
    Used throughout; the entire correction scheme contrasts 3D with 1D (Sects 1 and 2.1).
  • domain assumption Fe II lines have negligible non-LTE effects in 3D atmospheres for the considered parameter range, based on 1D non-LTE calculations of Lind et al. 2012.
    Adopted in Sects 1 and 2.2; motivates computing Fe II in 3D LTE rather than 3D non-LTE.
  • domain assumption The C I 'No-FS' and O I 'reduced' atomic models with ab initio hydrogen collision data are accurate across the parameter grid.
    Adopted from Amarsi et al. 2019a and 2018a; validated by solar center-to-limb variation (Sect. 1), not by independent data for the metal-poor UV-pumping regime (Sect. 3.1).
  • domain assumption The mixing-length theory parameters in the 1D models (alpha_MLT = 1.5, y = 0.076, conv = 8.0) reproduce the 3D grid's mean stratification sufficiently well.
    Stated in Sect. 2.1.3 and used to produce the 1D ATMO and MARCS model atmospheres that define the 1D LTE baseline.

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Cite this review

Pith. "Pith review of Carbon, oxygen, and iron abundances in disk and halo stars. Implications of 3D non-LTE spectral line formation." pith.science (2026). https://pith.science/paper/W7ZH42MC

@misc{pith2026190810319,
  author       = {Pith},
  title        = {Pith review of: Carbon, oxygen, and iron abundances in disk and halo stars. Implications of 3D non-LTE spectral line formation},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/W7ZH42MC}},
  note         = {Machine review of arXiv:1908.10319}
}
abstract

The abundances of carbon, oxygen, and iron in late-type stars are important parameters in exoplanetary and stellar physics, as well as key tracers of stellar populations and Galactic chemical evolution. We carried out three-dimensional (3D) non-LTE radiative transfer calculations for CI and OI, and 3D LTE radiative transfer calculations for FeII, across the STAGGER-grid of 3D hydrodynamic model atmospheres. The absolute 3D non-LTE versus 1D LTE abundance corrections can be as severe as $-0.3$ dex for CI lines in low-metallicity F dwarfs, and $-0.6$ dex for OI lines in high-metallicity F dwarfs. The 3D LTE versus 1D LTE abundance corrections for FeII lines are less severe, typically less than $+0.15$ dex. We used the corrections in a re-analysis of carbon, oxygen, and iron in $187$ F and G dwarfs in the Galactic disk and halo. Applying the differential 3D non-LTE corrections to 1D LTE abundances visibly reduces the scatter in the abundance plots. The thick disk and high-$\alpha$ halo population rise in carbon and oxygen with decreasing metallicity, and reach a maximum of [C/Fe]$\approx0.2$ and a plateau of [O/Fe]$\approx0.6$ at [Fe/H]$\approx-1.0$. The low-$\alpha$ halo population is qualitatively similar, albeit offset towards lower metallicities and with larger scatter. Nevertheless, these populations overlap in the [C/O] versus [O/H] plane, decreasing to a plateau of [C/O]$\approx-0.6$ below [O/H]$\approx-1.0$. In the thin-disk, stars having confirmed planet detections tend to have higher values of C/O at given [O/H]; this potential signature of planet formation is only apparent after applying the abundance corrections to the 1D LTE results. Our grids of line-by-line abundance corrections are publicly available and can be readily used to improve the accuracy of spectroscopic analyses of late-type stars.

Figures

Figures reproduced from arXiv: 1908.10319 by the authors.

Figure 1
Figure 1. Kiel diagram illustrating model atmospheres in log g— Teff space. The 1807 marcs nodes (grey circles) are regularly spaced in effective temperature, so model atmospheres with the same Teff label and log g label but different [Fe/H] labels overlap in this figure. How￾ever the 164 stagger nodes (blue diamonds) are not regularly space in effective temperature: thus, model atmospheres with different [Fe/H] la￾bels are a… view at source ↗
Figure 2
Figure 2. Gas temperature distributions in four different 3D stagger model atmospheres. The <3D> and 1D atmo model atmospheres are also plotted, as are the 1D marcs model atmospheres after interpolating them onto the same effective temperature. The 1D atmo and marcs model atmospheres were computed using the same fixed set of MLT parameters: αMLT = 1.5, y = 0.076, 3conv = 8.0. peting effects of radiative heating and adiabatic … view at source ↗
Figure 3
Figure 3. Grotrian term diagrams of the atomic models for C i and O i used for the non-LTE iterations. Also shown is a Grotrian term diagram for Fe ii, based on which LTE emergent line fluxes were calculated. Lev￾els for which fine structure has been collapsed are shown in red, and super levels are shown as long horizontal blue lines at the top of the figures. The transitions for which emergent line fluxes and abundance corre… view at source ↗
Figures from the paper (11 more)
Figure 4
Figure 4. Figure 4: Departure coefficients for levels of Ci (left panel), and for levels of O i (right panel), in different <3D> model atmospheres assuming [C/Fe] = [O/Fe] = 0.0 and ξmic = 1.0 km s−1 . The levels of intermediate excitation indicated here are, for Ci, 2p.3s 3P o (7.49 eV),…
Figure 5
Figure 5. Figure 5: Kiel diagram of 3D non-LTE versus 1D LTE abundance corrections for different Ci lines (columns), at different metallicities and carbon abundances (rows). The 1D microturbulence was fixed to ξmic = 1.0 km s−1 . that they turn over once the line is saturated. This signat…
Figure 6
Figure 6. Figure 6: Kiel diagram of 3D non-LTE versus 1D LTE abundance corrections for different O i lines (columns), at different metallicities and oxygen abundances (rows). The 1D microturbulence was fixed to ξmic = 1.0 km s−1 . can be in excess of −0.6 dex for the O i 777 nm multiplet;…
Figure 7
Figure 7. Figure 7: 3D non-LTE versus 1D LTE abundance corrections as functions of 3D non-LTE reduced equivalent widths, Wreduced = W/λ, for different C i and O i lines. The arrows show how the results change by increasing log C and log O respectively, and the curves are for fixed effec…
Figure 8
Figure 8. Figure 8: 3D LTE versus 1D LTE abundance corrections as functions of 3D LTE reduced equivalent widths, Wreduced = W/λ, for different Fe ii lines. The arrows show how the results change by increasing the metallicity [Fe/H] (noting that the iron abundance is always kept consistent…
Figure 9
Figure 9. Figure 9: Toomre diagram for the entire stellar sample, corrected for the peculiar solar motion using Co¸skunoglu et al. ˇ (2011). The kinematic information are primarily from Gaia DR2 (Gaia Collaboration et al. 2018), but for some stars where these data were missing the kinemat…
Figure 10
Figure 10. Figure 10: Differences between the spectroscopic surface gravities adopted here, and photometric surface gravities for 39 stars in the UVES-FIES sample for which the photometry are not significantly af￾fected by interstellar absorption and for which precise parallaxes are availa…
Figure 11
Figure 11. Figure 11: Carbon to iron abundance ratios for the entire stellar sample. The unclassified stars are from the VLT/UVES sample. The panels show results based on different line formation models, the 3D non-LTE model being preferred. −3.5 −3.0 −2.5 −2.0 −1.5 −1.0 −0.5 0.0 0.5 −0.2 …
Figure 12
Figure 12. Figure 12: Oxygen to iron abundance ratios for the entire stellar sample. The unclassified stars are from the VLT/UVES sample. The panels show results based on different line formation models, the 3D non-LTE model being preferred. discuss the results for those stars in the previ…
Figure 13
Figure 13. Figure 13: Carbon to oxygen abundance ratios for the entire stellar sample. The unclassified stars are from the VLT/UVES sample. The panels show results based on different line formation models, the 3D non-LTE model being preferred. −0.4 −0.3 −0.2 −0.1 −0.0 0.1 0.2 0.3 0.4 0.2 0…
Figure 14
Figure 14. Figure 14: Carbon to oxygen abundance ratios, for thin-disk stars without and with confirmed planet detections. The latter are further separated according to the maximum planet mass in the system. The panels show results based on different line formation models, the 3D non-LTE m…

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