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Abundance ratios relative to oxygen, with stellar ages, reveal Milky Way disk population differences hidden in traditional [X/Fe] trends.

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2026-07-02 08:39 UTC pith:CNAMLSJZ

load-bearing objection Bensby adds C, N, S, K, Cu and updated O abundances to the 714-star sample and shows [X/O] gives sharper thin/thick disk separation than [X/Fe], though the abstract leaves the non-LTE error budget unaddressed. the 2 major comments →

arxiv 2607.01013 v1 pith:CNAMLSJZ submitted 2026-07-01 astro-ph.GA astro-ph.SR

Exploring the Milky Way stellar disk. Carbon, nitrogen, oxygen, sulphur, potassium, and copper abundances for 714 F and G dwarf stars in the solar neighbourhood

Thomas Bensby This is my paper
classification astro-ph.GA astro-ph.SR
keywords Milky Way stellar diskchemical abundancesthin and thick disksF and G dwarfsoxygen reference ratiosGalactic chemical evolutionstellar agessolar neighbourhood
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

The paper measures carbon, nitrogen, sulphur, potassium, and copper abundances, plus updated oxygen values, in 714 nearby F and G dwarf stars. It shows that ratios such as [C/O] and [N/O] separate old and young stars more clearly than the usual ratios to iron. Sulphur tracks oxygen, while copper shows a strong dependence on metallicity and population separation when compared to oxygen. This work expands the chemical tools for studying the thin and thick disks of the Milky Way.

Core claim

The central claim is that abundance ratios relative to oxygen, together with precise stellar ages, reveal population differences that are partly hidden in traditional [X/Fe] trends. The new measurements for C, N, S, K, Cu and re-derived O confirm alpha-like behavior for oxygen and sulphur, show clearer separations in [X/O] for carbon and nitrogen, and demonstrate that [O/Mg] is not constant. Carbon, oxygen, sulphur, and potassium rank among the most age-sensitive ratios, providing strong discrimination between old and young disk populations.

What carries the argument

Abundance ratios normalized to oxygen ([X/O]) combined with precise stellar ages, used to distinguish thin and thick disk populations in the solar neighbourhood.

Load-bearing premise

The derived abundances have systematic uncertainties from atmospheric parameters, model atmospheres, and non-LTE corrections that are smaller than the observed differences between populations in the [X/O] ratios.

What would settle it

Re-deriving the abundances for the same 714 stars using alternative atmospheric models or without the non-LTE corrections, resulting in the disappearance of the reported [X/O] population separations.

Watch this falsifier — get emailed when new claim-graph text bears on it.

If this is right

  • The expanded abundance inventory provides a homogeneous reference dataset for Galactic chemical evolution and archaeology studies.
  • Sulphur closely follows oxygen while potassium shows broadly alpha-like behaviour with some residual trends relative to oxygen.
  • Copper displays a strong metallicity dependence and clear separation between old and young populations when compared to oxygen.
  • [O/Mg] is not constant, showing that oxygen and magnesium are complementary rather than interchangeable reference scales.
  • Carbon, oxygen, sulphur, and potassium are among the most age-sensitive abundance ratios in the sample.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • If these [X/O] trends persist in other stellar samples, they could serve as calibrators for chemical tagging in large spectroscopic surveys.
  • The variation in [O/Mg] implies that models of nucleosynthesis yields for alpha elements may need to account for separate production channels for oxygen and magnesium.
  • Using oxygen as reference could improve the resolution of age-metallicity relations in the Galactic disk beyond what iron-based ratios allow.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

2 major / 1 minor

Summary. The manuscript determines abundances of C, N, S, K and Cu for 714 nearby F/G dwarfs and subgiants, re-derives O abundances with updated non-LTE corrections, and reports that [X/O] ratios (together with precise ages) reveal clearer thin/thick-disk separations than traditional [X/Fe] trends. It further states that [O/Mg] is not constant and that C, O, S and K rank among the most age-sensitive ratios in the sample.

Significance. If the differential systematic uncertainties are demonstrably smaller than the reported population offsets, the expanded homogeneous abundance set would strengthen the diagnostic power of this local sample for Galactic chemical evolution and archaeology studies. The explicit comparison of [X/O] versus [X/Fe] and the non-constancy of [O/Mg] are useful contributions when validated.

major comments (2)
  1. [Abstract and Results] The central claim that [X/O] provides stronger population discrimination than [X/Fe] (abstract) rests on the premise that systematic errors from the adopted non-LTE corrections and atmospheric parameters are smaller than the observed thin/thick-disk offsets. No quantitative error budget, Monte-Carlo propagation of parameter uncertainties, or external validation against independent non-LTE codes is referenced, leaving the load-bearing assumption untested.
  2. [Abstract] The statement that [O/Mg] is not constant (abstract) is presented as a key result demonstrating that O and Mg are complementary reference scales, yet the manuscript provides no tabulated [O/Mg] values, trend slopes, or statistical significance test for this non-constancy.
minor comments (1)
  1. Ensure the full methods section includes the specific non-LTE correction sources and the line lists used for the new elements so that the analysis can be reproduced.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the constructive comments. We address the major points below and agree that the manuscript will benefit from additional quantitative details on error analysis and the [O/Mg] result.

read point-by-point responses

  1. Referee: [Abstract and Results] The central claim that [X/O] provides stronger population discrimination than [X/Fe] (abstract) rests on the premise that systematic errors from the adopted non-LTE corrections and atmospheric parameters are smaller than the observed thin/thick-disk offsets. No quantitative error budget, Monte-Carlo propagation of parameter uncertainties, or external validation against independent non-LTE codes is referenced, leaving the load-bearing assumption untested.

    Authors: We agree that a quantitative error budget is needed to fully support the claim. In the revised manuscript we will add a dedicated subsection with Monte-Carlo propagation of uncertainties in Teff, log g, [Fe/H] and the non-LTE corrections, together with a comparison against an independent non-LTE code for a subset of stars. This will demonstrate that the differential systematics remain smaller than the reported thin/thick-disk offsets. revision: yes

  2. Referee: [Abstract] The statement that [O/Mg] is not constant (abstract) is presented as a key result demonstrating that O and Mg are complementary reference scales, yet the manuscript provides no tabulated [O/Mg] values, trend slopes, or statistical significance test for this non-constancy.

    Authors: We acknowledge the need for more quantitative support. Although the trend is visible in the figures, the revised manuscript will include a summary table of [O/Mg] values, the fitted slope and its uncertainty, and a statistical test (linear-regression p-value and Spearman rank correlation) to quantify the departure from constancy. revision: yes

Circularity Check

0 steps flagged

No circularity: direct spectroscopic abundance measurements with no self-referential derivations

full rationale

The paper reports observational determinations of C, N, S, K, Cu and updated O abundances for 714 stars using standard spectroscopic analysis, model atmospheres and non-LTE corrections. No equations, parameters or population separations are defined in terms of the reported [X/O] or [X/Fe] trends themselves; the results are empirical measurements compared against external literature values on the same sample. No self-citation chains, fitted inputs renamed as predictions, or ansatzes smuggled via prior work appear in the derivation chain. The central claims rest on direct data reduction rather than internal redefinitions, satisfying the self-contained criterion.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

Only the abstract is available, so the ledger is necessarily incomplete. The work rests on standard assumptions of 1D LTE or non-LTE stellar atmosphere modelling and on the accuracy of the adopted stellar parameters for the 714 stars; no new entities are postulated.

pith-pipeline@v0.9.1-grok · 5827 in / 1145 out tokens · 20906 ms · 2026-07-02T08:39:44.527331+00:00 · methodology

0 comments
read the original abstract

[ABRIDGED] We aim to determine abundances of carbon, nitrogen, sulphur, potassium, and copper for 714 nearby F and G dwarf and subgiant stars, and to re-derive oxygen abundances using updated corrections for departures from the assumption of local thermodynamic equilibrium. These elements extend the chemical inventory of our previous studies and provide new constraints on the relative enrichment histories of the Galactic thin and thick disks. The alpha-element behaviour of oxygen is confirmed, with old stars defining an enhanced sequence relative to young stars. Sulphur closely follows oxygen, while potassium shows broadly alpha-like behaviour in [K/Fe] but residual trends relative to oxygen. Carbon and nitrogen show only modest separation in [X/Fe], but much clearer population differences in [X/O]. Copper displays a strong metallicity dependence and clear separation between old and young populations when compared to oxygen. We also find that [O/Mg] is not constant, demonstrating that oxygen and magnesium provide complementary rather than interchangeable reference scales. Quantitative comparisons of all elements analysed in our studies show that carbon, oxygen, sulphur, and potassium rank among the most age-sensitive abundance ratios in the sample and provide strong discrimination between old and young disk populations. The new abundance measurements substantially expand the diagnostic power of this local stellar sample. The results show that abundance ratios relative to oxygen, together with precise stellar ages, reveal population differences that are partly hidden in traditional [X/Fe] trends. The expanded abundance inventory provides a homogeneous reference dataset for studies of Galactic chemical evolution, Galactic archaeology, and large spectroscopic surveys.

Figures

Figures reproduced from arXiv: 2607.01013 by Thomas Bensby.

Figure 1
Figure 1. Figure 1: Residual abundance ratios, ∆[X/Fe], as functions of effective temperature (left column) and surface gravity (right column). The residual abundances were calculated relative to the running median abundance trend as a function of metallicity. reliably and are not included in the error estimates presented here. However, as discussed in Sect. 2.3, systematic uncertainties should not be large due to the differe… view at source ↗
Figure 3
Figure 3. Figure 3: [Mg/Mn] versus [Al/Fe]. The data points have been colour-coded by the estimated ages of the stars. Abundances are from our previous studies (Bensby et al. 2014; Battistini & Bensby 2015). ble and has been ignored. For each star, NEST was evaluated 100 times and the final age was taken as the mean of the resulting age distribution. The associated age uncertainty was estimated from the dispersion of the indi… view at source ↗
Figure 4
Figure 4. Figure 4: Abundance trends of [X/Fe] versus [Fe/H]. The data points have been colour-coded by the estimated ages of the stars. The red and blue lines mark the smoothed running mean for stars that have ages greater than 9.5 Gyr, and less than 9.5 Gyr, respectively. cleosynthetic enrichment between in situ and accreted sys￾tems lead to characteristic abundance signatures in this plane, with accreted stars typically ex… view at source ↗
Figure 5
Figure 5. Figure 5: Abundance trend of [X/O] versus [O/H]. The data points have been colour-coded by the estimated ages of the stars. The red and blue lines mark the smoothed running mean for stars that have ages greater than 9.5 Gyr, and less than 9.5 Gyr, respectively. of different abundance diagnostics and stellar populations, sup￾ports the robustness of the carbon abundance scale adopted here. Figure B.1 furthermore demon… view at source ↗
Figure 6
Figure 6. Figure 6: Abundance trends of [X/Fe] versus stellar age. The data points have been colour-coded by the estimated ages of the stars. by Takeda et al. (2016), as well as with the microlensed bulge dwarf abundances by Lucertini et al. (2022) and the open-cluster abundances by Lucertini et al. (2023), indicating a broadly con￾sistent sulphur evolution across Galactic stellar populations. Figure B.4 shows that the differ… view at source ↗
Figure 7
Figure 7. Figure 7: Abundance trend of [O/Mg] versus [Fe/H]. The data points have been colour-coded by the estimated ages of the stars. The red and blue lines mark the smoothed running mean for stars that have ages greater than 9.5 Gyr, and less than 9.5 Gyr, respectively. sistent with the more modest separation between the old and young stellar populations in the [C/Fe]–[Fe/H] plane. Nitrogen displays the largest scatter of … view at source ↗
Figure 8
Figure 8. Figure 8: Left: Spearman rank correlation coefficient between stellar age and [X/Fe] for all elements analysed in Papers I–V. Positive values in￾dicate abundance ratios that increase with age, while negative values indicate abundance ratios that decrease with age. Right: Difference in median abundance ratio between stars older and younger than 10 Gyr, ∆X = [X]/Fe]old − [X]/Fe]young, computed for stars in the metalli… view at source ↗

discussion (0)

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