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arxiv: 2605.23786 · v1 · pith:KHMQAEKTnew · submitted 2026-05-22 · 🌌 astro-ph.GA · astro-ph.SR

Gaia FGK benchmark stars: abundances of textit{n}-capture elements of the third version

S. Vitali , P. Jofr\'e , L. Casamiquela , U. Heiter , C. Aguilera G\'omez , D. Barrios L\'opez , S. Blanco Cuaresma , A. Escorza
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I. Hern\'andez Araya T. Signor C. Soubiran H. Sinclair Wentworth C. Worley
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Pith reviewed 2026-05-25 03:19 UTC · model grok-4.3

classification 🌌 astro-ph.GA astro-ph.SR
keywords Gaia benchmark starsneutron-capture elementsstellar abundancesMilky Way chemical evolutionspectroscopic analysisFGK starsreference sample
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The pith

Neutron-capture element abundances are derived homogeneously for the third Gaia benchmark stars release using tailored line analysis.

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

The paper determines abundances of neutron-capture elements for the Gaia FGK benchmark stars in their third version. It compiles high-resolution spectra and applies the iSpec code with a clustering algorithm to group stars by parameters and metallicity. This grouping enables an in-depth line assessment that handles few usable lines, weak strengths, saturation, and atomic data issues. The approach produces reliable, homogeneous measurements that agree with literature values and extend the chemical data set for these reference stars.

Core claim

By applying an in-depth line assessment tailored to different groups identified through a clustering algorithm that accounts for the diversity in stellar parameters and metallicities, homogeneous abundances of n-capture elements are inferred across the GBSv3 sample, establishing an extended and robust reference scale in good agreement with the literature.

What carries the argument

Clustering algorithm that groups stars by stellar parameters and metallicities, paired with in-depth line assessment, applied inside the iSpec code on the compiled high-resolution spectra.

Load-bearing premise

The clustering algorithm and in-depth line assessment successfully addresses the paucity of usable lines, weak strengths, saturation, and atomic-data sensitivity to produce accurate abundances.

What would settle it

Independent high-resolution abundance measurements for the same stars that deviate systematically from the new values would show the tailored assessment does not yield reliable results.

Figures

Figures reproduced from arXiv: 2605.23786 by A. Escorza, C. Aguilera G\'omez, C. Soubiran, C. Worley, D. Barrios L\'opez, H. Sinclair Wentworth, I. Hern\'andez Araya, L. Casamiquela, P. Jofr\'e, S. Blanco Cuaresma, S. Vitali, T. Signor, U. Heiter.

Figure 1
Figure 1. Figure 1: Kiel diagram and parameter distributions of the stellar sample, color-coded by stellar group. Top: Kiel diagram where normal stars are shown as circles, while the RepGBS are represented with distinct sym￾bols. Bottom: Violin plot of the metallicity for each group. The width of each violin reflects the density of stars, with inner lines indicating the median and quartiles. Individual stars are overplotted i… view at source ↗
Figure 2
Figure 2. Figure 2: Compilation of spectral lines for each n-capture element ana￾lyzed in this work, based on an analysis of the RepGBS. The vertical axes show the differences between the abundances measured for each line and each instrument and the median of all measurements per el￾ement. Crosses indicate lines with instrument-to-instrument dispersion above 0.15 dex, while circles represent lines with lower dispersion. The y… view at source ↗
Figure 3
Figure 3. Figure 3: Y abundances derived from the selected lines for each star. Pan￾els are left empty when no measurable lines are available. Each panel reports the final mean abundance A(X) (Eq. 1), computed from the lines listed in [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗
Figure 5
Figure 5. Figure 5: Same as [PITH_FULL_IMAGE:figures/full_fig_p007_5.png] view at source ↗
Figure 9
Figure 9. Figure 9: Same as [PITH_FULL_IMAGE:figures/full_fig_p008_9.png] view at source ↗
Figure 8
Figure 8. Figure 8: Same as [PITH_FULL_IMAGE:figures/full_fig_p008_8.png] view at source ↗
Figure 10
Figure 10. Figure 10: Same as [PITH_FULL_IMAGE:figures/full_fig_p009_10.png] view at source ↗
Figure 12
Figure 12. Figure 12: Example spectra of four GBS observed with ESPaDOnS. The observed spectrum is shown as a black dashed line, while the best-fitting synthetic spectrum of the single Eu ii line used in this work is plotted as a continuous orange line. The orange shaded region indicates the wavelength interval used to derive the abundance from the Eu ii line, whose central wavelength is marked by the black dashed vertical lin… view at source ↗
Figure 13
Figure 13. Figure 13: shows a comparison between our results, derived as described above, and literature values. Our abundance ratios are expressed relative to Fe, adopting the solar abundances from Grevesse et al. (2007), while for the literature values we adopted the solar abundances reported in the corresponding references. The compiled literature abundances and their corresponding ref￾erences are listed in App. C, alongsid… view at source ↗
Figure 14
Figure 14. Figure 14: Similar to [PITH_FULL_IMAGE:figures/full_fig_p012_14.png] view at source ↗
Figure 15
Figure 15. Figure 15: Differences between our solar abundances and the literature values from Grevesse et al. (2007) (GR07) and Asplund et al. (2009) (AS09). These values are also reported in Table D.1. the effects of different log g f sources from possible 3D-non-LTE effects. Discrepancies of similar order of magnitude ( ∼ 0.2 dex) also affect Ce ii and Pr ii. However, differences are observed not only between our results and… view at source ↗
Figure 16
Figure 16. Figure 16: Various [X/Fe]–[Fe/H] trends for the n-capture elements measured in this work. The GBS stars are color-coded according to their group membership as assigned by the clustering analysis, with the RepGBS with the same symbols adopted in [PITH_FULL_IMAGE:figures/full_fig_p014_16.png] view at source ↗
read the original abstract

In the current era, in which an unprecedented wealth of data is available for the study of the Milky Way, the Gaia Benchmark Stars (GBS) have become an established reference and calibration sample. Studies of stellar structure and evolution, as well as the chemical history of our Galaxy, largely rely on large spectroscopic surveys and their output catalogs. In this context, deriving precise and accurate stellar parameters and chemical abundances is of paramount importance. This study provides the determination of neutron(n)-capture element abundances, extending the set of chemical abundances available for the third GBS release (GBSv3). Based on the compilation of high-resolution spectra assembled for GBSv3 and consistently with the spectral analysis adopted for the chemical abundances of GBSv3, we used the iSpec code to derive heavy-element abundances. We infer homogeneous abundances of n-capture elements across the GBSv3 sample using an in-depth line assessment tailored to different groups identified through a clustering algorithm that accounts for the diversity in stellar parameters and metallicities. This approach addresses key challenges in the spectral analysis of these elements, including the paucity of usable lines, weak line strengths, saturation effects, and sensitivity to atomic data. It yields reliable measurements, establishing an extended and robust reference scale in good agreement with the literature. This compilation of these abundances is based on the GBS's robust and accurate atmospheric parameters, together with the analysis of a large sample of stellar spectra per star, which provides a reliable and homogeneous spectral analysis. It supports the use of chemical abundances as precise tracers of the Milky Way's star formation history and chemical evolution, and constitutes a legacy sample for the calibration of current and future spectroscopic surveys.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 2 minor

Summary. The manuscript determines neutron-capture element abundances for the Gaia FGK benchmark stars third release (GBSv3). It applies the iSpec code to the compiled high-resolution spectra, using a clustering algorithm on stellar parameters and metallicities to define groups, followed by per-group in-depth line assessment to derive homogeneous abundances despite challenges such as few usable lines, weak strengths, saturation, and atomic-data sensitivity. The central claim is that this produces reliable measurements that establish an extended reference scale in good agreement with the literature.

Significance. If the results hold, the work extends the GBS reference sample with n-capture abundances derived consistently with the GBSv3 atmospheric parameters and multiple spectra per star. This supports calibration of spectroscopic surveys and use of abundances as tracers of Milky Way chemical evolution. The tailored per-group analysis is presented as directly addressing the spectroscopic difficulties of these elements.

major comments (2)
  1. [Abstract and §3] Abstract and §3 (method description): the claim of 'reliable measurements' and 'good agreement with the literature' is stated without any reported quantitative metrics (e.g., mean offsets, rms differences, or star-by-star comparisons to prior studies), error bars on the new abundances, or validation against independent datasets; this is load-bearing for the central claim of establishing a robust reference scale.
  2. [§4] §4 (results): without explicit line lists, equivalent-width measurements, or the specific clustering criteria and group definitions, it is not possible to verify that the tailored assessment successfully mitigates saturation and atomic-data sensitivity for the n-capture species; the absence of these details prevents assessment of whether the method is parameter-free or internally consistent.
minor comments (2)
  1. [Table 1] Table 1 or equivalent: ensure all adopted atomic data sources and solar reference abundances are tabulated with references.
  2. [Figure 2] Figure 2 or equivalent: clarify the color scale and axis ranges in any abundance comparison plots to allow direct visual assessment of agreement with literature values.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the constructive comments and positive overall assessment of our work on neutron-capture abundances for the GBSv3 sample. We address each major comment below and will revise the manuscript accordingly to improve verifiability while preserving the core analysis.

read point-by-point responses

  1. Referee: [Abstract and §3] Abstract and §3 (method description): the claim of 'reliable measurements' and 'good agreement with the literature' is stated without any reported quantitative metrics (e.g., mean offsets, rms differences, or star-by-star comparisons to prior studies), error bars on the new abundances, or validation against independent datasets; this is load-bearing for the central claim of establishing a robust reference scale.

    Authors: We agree that quantitative support for the claims of reliability and literature agreement would strengthen the presentation. In the revised manuscript we will add mean offsets, RMS differences, and star-by-star comparisons to prior studies (with error bars on the new abundances) to §3, and we will update the abstract to reference these metrics and any validation against independent datasets. revision: yes

  2. Referee: [§4] §4 (results): without explicit line lists, equivalent-width measurements, or the specific clustering criteria and group definitions, it is not possible to verify that the tailored assessment successfully mitigates saturation and atomic-data sensitivity for the n-capture species; the absence of these details prevents assessment of whether the method is parameter-free or internally consistent.

    Authors: We acknowledge that the current description lacks sufficient detail for full reproducibility and verification of the per-group line assessment. In the revised version we will expand §4 to include the explicit clustering criteria and group definitions, the line lists adopted for each group, and sample equivalent-width measurements (either in the main text or a dedicated appendix/table). This will allow readers to assess how the tailored approach addresses saturation and atomic-data issues. revision: yes

Circularity Check

0 steps flagged

No significant circularity; minor self-reference to GBSv3 not load-bearing

full rationale

The paper derives n-capture abundances via iSpec on compiled high-resolution spectra, applying a clustering-based line assessment per stellar-parameter group. No equations, fitted parameters, or predictions are shown that reduce by construction to the same data or to a self-citation chain. The GBSv3 reference is invoked for consistency of atmospheric parameters, but this is external input rather than a self-definitional loop; the central result (homogeneous abundances agreeing with literature) rests on direct spectral analysis and external validation, not on renaming or smuggling an ansatz. This matches the default expectation for non-circular empirical abundance work.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

Review based on abstract only; no explicit free parameters, axioms, or invented entities are described.

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