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Solar and Stellar Astrophysics · arXiv:2609.15386 v1 · submitted 14 Sep 2026 · 145 references

MINCE IV. A detailed analysis of 37 metal-poor and subsolar metallicity stars

L. Sgatti, G. Cescutti, L. Lombardo, C. T. Nguyen, P. Bonifacio, E. Caffau, L. Monaco, R. Lallement

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L. Magrini, M. Franchini, C. J. Hansen, A. Mucciarelli, A. Korn, A. Kucinskas, E. Spitoni, S. Lucatello

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The paper says

“The project called Measuring at Intermediate metallicity Neutron-Capture Elements (MINCE) primarily focuses on the photospheric abundances of several neutron-capture (NC) elements from high-quality spectra of metal-poor stars within the metallicity range of ${\rm -2.5 \leq\![Fe/H]\!\leq -1.5}$, aiming to provide homogeneous information on their chemical compositions.”

more of the abstract

Furthermore, based on the Gaia mission, chemical abundances can now be coupled with kinematic properties, enabling investigations of the constituent substructures of the Milky Way. We analyse the fourth sample of MINCE stars in terms of atmospheric parameters and chemical composition. The results are then compared with the previously analysed MINCE samples. The observations were conducted with HARPS-N (${\rm R \approx 120\,000}$) at the Telescopio Nazionale Galileo (TNG) and FIES (${\rm R \approx 67\,000}$ ) at the Nordic Optical Telescope (NOT), providing optical spectra with a high signal-to-noise ratio (S/N) and high resolution. We then used the methods developed in previous MINCE works and Gaia photometric data to obtain the stellar atmospheric parameters. The chemical abundances were analysed using 1D-LTE model atmospheres. We present the photospheric abundances in 37 stars of up to 26 elements, including α, iron-peak, light-odd, and 10 NC−elements (Sr, Y, Zr, Ba, La, Ce, Pr, Nd, Sm, and Eu). Kinematic properties and membership assessments are provided for all stars. The MINCE catalogue is thus expanded by 13 thin-disc stars, 9 thick-disc stars, 1 star in a transition zone between the thin and thick disc, 9 stars of the halo, and 5 Gaia-Sausage-Enceladus stars. The results agree excellently with previous MINCE works. The comparison with a Gaia Sausage Enceladus GCE model is consistent with the scenario of a major accretion event on the Milky Way from a dwarf galaxy.

from the abstract

Pith says

Machine review · deepseek-v4-flash · 15 Sep 2026 · what was read was not recorded · not checked by a person

It can be wrong. Challenge this review or reply to it.

The passes disagreed. Reader: holds up. Skeptic: holds up only with conditions. Referee: major revision.

Solid incremental data paper; the neutron-capture conclusions are undermined by the authors' own admission that NLTE corrections could shift [Ba/Eu] by >0.3 dex. This line is wrong

2 major objections · 6 minor

How often objections from reviews like this one are right: not yet measured

Are you an author? What you can do.

Not checked: figures, code, what the 145 references say.

The paper says, at Sects. 5.4, 6.4, and 7

The review did not quote this passage.

Pith says: Objection 1 of 2 · major

There is an internal contradiction that undermines the neutron-capture conclusions. Section 7 explicitly states that 'no conclusions on these elements can be drawn until a proper NLTE treatment is applied' with reference to Sr and Zr. Yet Sects. 5.4 and 6.4 use [Ba/Eu] to classify 27 stars as r-I and to compare with the GCE model, despite the authors noting …

more of objection 1

… that Ba II 5853 Å can have 3D-NLTE corrections up to 0.5 dex and that Sr I 4607 Å may have NLTE corrections up to +0.4 dex. A shift of 0.3 dex in [Ba/Eu] could alter the r/s-process classification and the GSE interpretation. The paper must either apply the necessary corrections or explicitly state that the [Ba/Eu]-based conclusions are preliminary and subject to revision once NLTE/3D grids become available. The current text is inconsistent and reduces the evidential basis for the claimed classifications.

The paper says, at Sect. 4.1 (atmospheric parameters)

The review did not quote this passage.

Pith says: Objection 2 of 2 · major

The paper determines Teff and log g via a photometric method using Gaia magnitudes corrected for extinction with dust maps from Schlegel et al. (1998) or Vergely et al. (2022). The authors verify that different maps yield differences up to 100 K in Teff and 0.15 dex in log g.

more of objection 2

However, seven recovered stars from MINCE I use a third dust map (Schlafly & Finkbeiner 2011). Since all derived abundance ratios depend on these parameters, it would be helpful to quantify how the dust-map-induced parameter shifts propagate into the final [X/Fe] ratios, especially for elements with strong sensitivity to Teff or log g (e.g., Ca I, Ti I). A brief propagation estimate would strengthen the robustness claims.

6 minor objections

The paper says, at Sect. 4.3

Pith says: minor objection 1 of 6

The description of the 'single-model' approach in MyGIsFOS could be clearer. Currently it states that 'all the synthetic spectra in the grid are computed with the same model atmosphere, therefore with fixed stellar parameters, while the abundances are varying in an interval of ±1 dex in steps of 0.2 dex.' It would help to explain how the pivot values are chosen and whether the grid covers the full metallicity range of the sample.

The paper says, at Sect. 5.4 (Fig. 10)

Pith says: minor objection 2 of 6

The caption of Fig. 10 does not mention that the [Ba/Eu] thresholds for r-process dominance (< -0.7) and s-process dominance (> +1.5) are from Arlandini et al. (1999) and Bisterzo et al. (2014). Please add the references to the caption.

show 4 more

The paper says, at Sect. 6.4, Fig. 11

Pith says: minor objection 3 of 6

The GCE model presented in Fig. 11 is from Nguyen et al. (2026), which shares co-authors with the present paper. While the comparison is a posteriori, the paper should note this overlap explicitly in the caption or text to allow readers to assess independence.

The paper says, at Sect. 4.5

Pith says: minor objection 4 of 6

The NLTE discussion for Na I states that 'the Na D lines... tend to be hugely overestimated in LTE analysis, leading to corrections up to -0.5 dex.' However, the paper excludes Na D lines and uses other lines. It would be useful to explicitly state that the lines actually used for Na are believed to be minimally affected by NLTE, or to provide a reference justifying that choice.

The paper says, at Sect. 5.1, Fig. 4

Pith says: minor objection 5 of 6

The RMSE values quoted for alpha elements (e.g., O 0.14 dex, Mg 0.12 dex) are derived from a quadratic fit to the data. The functional form of the fit is not described; please add a brief note (e.g., second-order polynomial in [Fe/H]) to the text.

The paper says, at Sect. 5.3 (Zinc)

Pith says: minor objection 6 of 6

The discussion of the Zn dip at solar metallicity notes that no gradient with apocentric distance is found, ruling out the radial gradient hypothesis. The pericentric gradient seen is attributed to selection bias. This interpretation is reasonable, but the pericentric panel (Fig. E.3, bottom) shows a trend; the paper should specify the range of pericentric distances to clarify the contrast.

What would settle it

Apply publicly available 3D-NLTE corrections for Ba II (ChETEC-INFRA database, 2024) and NLTE corrections for Sr I (Bergemann et al. 2012) to all 37 stars. Recompute [Ba/Eu] for each star and recount stars in r-process dominated ([Ba/Eu] <= -0.7), r-I (-0.7 < [Ba/Eu] <= 0), and s-process (>0) categories. Check whether the GSE model overlap in Fig. 11 changes by more than 0.2 dex in [Ba/Eu] for the GSE subsample. If the number of r-I stars changes by more than 10% or the GSE comparison shifts materially, the abundance-derived conclusions require revision.

from the skeptic's reading

How the review went

4 readings by deepseek-v4-flash · 15 Sep 2026

  1. Reader holds up confidence high
  2. Skeptic partly agrees: says it holds up only with conditions 46 s · 30,051 tokens read, 1,218 written NLTE corrections for Ba and Sr could shift [Ba/Eu] classifications by more than 0.3 dex, undermining r-process and GSE conclusions.
  3. Editor wrote the verdict above 12 s · 30,267 tokens read, 977 written
  4. Referee major revision: 2 major objections, 6 minor 25 s · 29,733 tokens read, 2,703 written

Not run on this paper: the simulated authors' defence.

Pith did not check this review's objections against the paper.

The review in full

The review in brief, machine-written

This paper adds 37 stars with homogeneous chemical abundances (up to 26 elements, including 10 neutron-capture) to the MINCE catalogue. The data are carefully obtained, the 1D-LTE analysis is standard for the field, and the kinematic classifications are well-done. The comparison with a GSE chemical evolution model is a nice touch. The paper is a genuine incremental contribution—useful for anyone doing Galactic chemical evolution or studying the GSE accretion event.

The main soft spot is real and sits at the center of the neutron-capture discussion. The authors state clearly (Sect. 4.5) that Ba II 5853 can have 3D-NLTE corrections up to 0.5 dex, Sr I 4607 has NLTE corrections up to +0.4 dex, and in Sect. 7 they write 'no conclusions on these elements can be drawn until a proper NLTE treatment is applied.' Yet in Sects. 5.4 and 6.4 they use the LTE [Ba/Eu] ratio to classify stars as r-I, r-process-dominated, and s-process-mixed, and to compare with the GCE model. The stress-test concern is right: if corrections are even half the quoted maximum, several stars' [Ba/Eu] would cross classification boundaries, and the GSE model comparison in Fig. 11 would rest on shaky ground. The authors acknowledge this tension but do not resolve it.

This is not a fatal flaw—the paper's core value is the abundance table itself, not the interpretive layer. But the referees should press the authors to either apply approximate corrections (even if just for the diagnostic [Ba/Eu] ratio) or explicitly remove the scientific claims that depend on those ratios and recast the neutron-capture section as purely descriptive. The GCE model comparison (which also involves an author overlap) should be either omitted or moved to a supplementary 'suggestive' section.

Verdict: this paper deserves peer review; it's a serious piece of work with a clear, fixable inconsistency. A reasonable editor sends it to a referee who knows neutron-capture abundance analysis.

The strongest objection

The neutron-capture discussion (Sects. 5.4, 6.4) and GSE model comparison (Fig. 11) rely on Ba and Sr abundances derived in 1D-LTE. The authors note that Sr I 4607 A may have NLTE corrections up to +0.4 dex (Bergemann et al. 2012) and that Ba II 5853 A can have 3D-NLTE corrections up to 0.5 dex (ChETEC-INFRA 2024). For nine metal-rich stars Sr was measured manually; for many stars the Ba 5853 line is the only reliable one. If these corrections are applied, [Ba/Eu]—the primary r/s-process diagnostic—could shift by more than 0.3 dex. In Fig. 10, 30 stars have [Ba/Eu] < 0; after correction some could cross the r-process threshold (<= -0.7) or the s-process threshold (>0). This reclassification would alter the statement that 27 stars are r-I and the interpretation of GSE stars in Fig. 11. The authors state 'no conclusions on these elements can be drawn until a proper NLTE treatment is applied' (Sect. 7), yet use [Ba/Eu] to assess mixing and compare to the GCE model. This internal tension removes the evidential basis for the neutron-capture conclusions.

The paper is well-conducted and provides a valuable homogeneous abundance dataset. However, the neutron-capture analysis draws conclusions about r-process enrichment and GSE comparisons from Ba and Sr abundances that the authors themselves flag as unreliable due to unmodeled NLTE effects. This does not invalidate the raw data—they are correctly published—but it directly weakens the strongest interpretive claims in the paper. A conditional acceptance requiring the authors to either apply and report NLTE corrections for Ba and Sr to the key stars (GSE sample and those defining [Ba/Eu] thresholds) or to explicitly limit neutron-capture conclusions to elements with verified small NLTE effects would resolve this tension and strengthen the final article. The reader's weakest assumption (dust map systematics) is related but less directly tied to the specific conclusions that are at risk.

The referee's report

The work provides a homogeneous, high-quality abundance dataset for metal-poor and subsolar metallicity stars, covering 10 neutron-capture elements. Such datasets are valuable for constraining Galactic chemical evolution models and identifying accreted substructures. The combination of kinematics and detailed chemistry is a strength. The paper extends the MINCE series and offers a resource for the community.

Pith's reading of the paper (a machine's summary, not the authors')

This paper reports the photospheric abundances of up to 26 elements for 37 stars observed with high-resolution spectrographs, adding to the MINCE project's homogeneous dataset. By combining abundances with Gaia-based kinematics, the authors classify the stars into thin disc, thick disc, halo, and Gaia-Sausage-Enceladus (GSE) members. The chemical patterns, especially for α-elements and neutron-capture elements, match previous MINCE results and a dedicated GSE chemical evolution model, supporting the idea that GSE originated from an accreted dwarf galaxy. The data also reveal a decline in [Zn/Fe] at near-solar metallicities that does not correlate with Galactocentric radius, contradicting a previous claim of a radial gradient.

What carries the argument. The analysis uses high-resolution optical spectra (R≈120,000 from HARPS-N and R≈67,000 from FIES), 1D-LTE ATLAS9 model atmospheres with the MyGIsFOS code for abundance determination via spectral synthesis, and equivalent-width measurements with the sbundance code for atmospheric parameters and microturbulence. Kinematic membership is based on Gaia DR3 astrometry and the galpy potential, using criteria from Bensby et al. (2014) for disc components and Feuillet et al. (2021) for halo substructures. The chemical evolution model for GSE (Nguyen et al. 2026) employs a Gaussian infall rate and Schmidt-type star formation with an outflow wind.

Core claim. This paper presents a homogeneous chemical abundance analysis of 37 metal-poor and subsolar-metallicity stars, determining abundances for up to 26 elements including 10 neutron-capture species, and classifying them into Galactic substructures. The results are in excellent agreement with earlier MINCE papers and with a chemical evolution model of Gaia-Sausage-Enceladus, which assumes a lower star-formation efficiency compared to the Milky Way's thick disc. A notable finding is that the [Zn/Fe] ratio declines toward solar metallicity without a radial gradient, ruling out a previously proposed explanation for this trend in giants.

The premise it rests on. The atmospheric parameters (Teff, log g) and absolute magnitudes used to derive all abundances rely on Gaia photometry corrected with interstellar extinction maps (Schlegel et al. 1998 or Vergely et al. 2022), which have known zero-point uncertainties that propagate into abundance ratios at the level of 0.1–0.2 dex.

If the paper is right (Pith's inferences, not the authors')

The homogeneous abundance dataset for 37 stars, combined with previous MINCE samples, provides 102 stars with consistent measurements, strengthening constraints on chemical evolution models, particularly for neutron-capture elements.

The observed [α/Fe] knee positions for thick disc ([Fe/H]≈−0.59) and GSE ([Fe/H]≈−1.23) confirm different star-formation histories, with GSE having a lower-metallicity knee consistent with slower enrichment.

The lack of a radial gradient in [Zn/Fe] rules out the spatial gradient hypothesis for the zinc decline in giants, pointing to an alternative explanation such as NLTE effects or selection biases.

The abundance patterns of 10 neutron-capture elements, especially the [Ba/Eu] ratio, show that r-process dominated stars are common in this metallicity range, and that s-process contributions appear only at [Fe/H]>−0.66.

The kinematic classification combined with abundances could help identify additional GSE and Sequoia candidates in other surveys, as the chemical signatures of these accreted populations become better defined.

The discrepancy in zinc trends between giants and dwarfs might motivate a targeted NLTE analysis of Zn I and Zn II lines across a wider stellar parameter range to isolate atmospheric from evolutionary effects.

The systematic Sr I underabundance relative to literature suggests that future MINCE work should incorporate NLTE corrections for Sr, possibly altering conclusions about the r/s-process balance in individual stars.

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The paper

Abstract

The project called Measuring at Intermediate metallicity Neutron-Capture Elements (MINCE) primarily focuses on the photospheric abundances of several neutron-capture (NC) elements from high-quality spectra of metal-poor stars within the metallicity range of ${\rm -2.5 \leq\![Fe/H]\!\leq -1.5}$, aiming to provide homogeneous information on their chemical compositions. Furthermore, based on the Gaia mission, chemical abundances can now be coupled with kinematic properties, enabling investigations of the constituent substructures of the Milky Way. We analyse the fourth sample of MINCE stars in terms of atmospheric parameters and chemical composition. The results are then compared with the previously analysed MINCE samples. The observations were conducted with HARPS-N (${\rm R \approx 120\,000}$) at the Telescopio Nazionale Galileo (TNG) and FIES (${\rm R \approx 67\,000}$ ) at the Nordic Optical Telescope (NOT), providing optical spectra with a high signal-to-noise ratio (S/N) and high resolution. We then used the methods developed in previous MINCE works and Gaia photometric data to obtain the stellar atmospheric parameters. The chemical abundances were analysed using 1D-LTE model atmospheres. We present the photospheric abundances in 37 stars of up to 26 elements, including α, iron-peak, light-odd, and 10 NC−elements (Sr, Y, Zr, Ba, La, Ce, Pr, Nd, Sm, and Eu). Kinematic properties and membership assessments are provided for all stars. The MINCE catalogue is thus expanded by 13 thin-disc stars, 9 thick-disc stars, 1 star in a transition zone between the thin and thick disc, 9 stars of the halo, and 5 Gaia-Sausage-Enceladus stars. The results agree excellently with previous MINCE works. The comparison with a Gaia Sausage Enceladus GCE model is consistent with the scenario of a major accretion event on the Milky Way from a dwarf galaxy.

The paper's own sentences, arranged, kept beside the review and separate from it. Each label is drawn from a closed vocabulary; the number beside it is the probability the classifier gave that label. No sentence in this record was written by a model.

abstract compiled · 2026-09-23

The authors' main claim, as the classifier picked it out 0.97

“The comparison with a Gaia Sausage Enceladus GCE model is consistent with the scenario of a major accretion event on the Milky Way from a dwarf galaxy.”

How the main claim is stated: hedged possibility 0.99

What the abstract itself states, as probabilities: claims first 0.03 · states limitation 0.07 · human participants 0.02 · controlled comparison 0.30 · randomized assignment 0.01 · states quantitative result 0.97 · compares with prior results 0.98 · mentions code or data availability 0.05

The abstract, sentence by sentence

This table labels the abstract only (arXiv listing abstract v1). The number is the probability the classifier gave the label.

SentenceRoleThe authors' own workStates the main conclusionStrength
The project called Measuring at Intermediate metallicity Neutron-Capture Elements (MINCE) primarily focuses on the photospheric abundances of several neutron-capture (NC) elements from high-quality spectra of metal-poor stars within the metallicity range of ${\rm -2.5 \leq\![Fe/H]\!\leq -1.5}$, aiming to provide homogeneous information on their chemical compositions. background 0.60 0.64 0.04 asserted 0.99
Furthermore, based on the Gaia mission, chemical abundances can now be coupled with kinematic properties, enabling investigations of the constituent substructures of the Milky Way. background 1.00 0.08 0.03 asserted 0.83
We analyse the fourth sample of MINCE stars in terms of atmospheric parameters and chemical composition. contribution 0.99 0.93 0.03 asserted 0.99
The results are then compared with the previously analysed MINCE samples. method 0.67 0.81 0.03 asserted 0.85
The observations were conducted with HARPS-N (${\rm R \approx 120\,000}$) at the Telescopio Nazionale Galileo (TNG) and FIES (${\rm R \approx 67\,000}$ ) at the Nordic Optical Telescope (NOT), providing optical spectra with a high signal-to-noise ratio (S/N) and high resolution. method 1.00 0.83 0.02 asserted 1.00
We then used the methods developed in previous MINCE works and Gaia photometric data to obtain the stellar atmospheric parameters. method 1.00 0.92 0.02 asserted 1.00
The chemical abundances were analysed using 1D-LTE model atmospheres. method 1.00 0.84 0.02 asserted 1.00
We present the photospheric abundances in 37 stars of up to 26 elements, including $\alpha$, iron-peak, light-odd, and 10 NC$-$elements (Sr, Y, Zr, Ba, La, Ce, Pr, Nd, Sm, and Eu). result 0.73 0.95 0.11 asserted 1.00
Kinematic properties and membership assessments are provided for all stars. result 0.57 0.92 0.05 asserted 1.00
The MINCE catalogue is thus expanded by 13 thin-disc stars, 9 thick-disc stars, 1 star in a transition zone between the thin and thick disc, 9 stars of the halo, and 5 Gaia-Sausage-Enceladus stars. result 0.81 0.92 0.15 asserted 1.00
The results agree excellently with previous MINCE works. result 0.95 0.80 0.15 asserted 1.00
The comparison with a Gaia Sausage Enceladus GCE model is consistent with the scenario of a major accretion event on the Milky Way from a dwarf galaxy. interpretation 0.96 0.75 0.33 hedged possibility 0.99

What kind of paper the classifier reports this is: dataset or benchmark 0.59 · evidence from observation or experiment 0.98

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How the labels were made

Compiled by classifier-1.13.0 via TypeSafe API, question bank abstract-p1-20260923, 2026-09-23: 1 request, 9,234 input tokens.

Every quoted sentence on this record is the authors'. Every label is from Pith's closed vocabulary, with the probability shown beside it. This record as JSON

Figures (12)
Figure 1 of the paper
Figure 1. Comparison on microturbulent velocity ξ between the results derived by using sbundance and Mashonkina empirical law. 4.2. Kinematics The kinematics of our stars were evaluated following the methodology in previous MINCE papers. We used astromet￾ric data from Gaia DR3 (Gaia Collaboration et al. 2023b) and computed orbital parameters and actions with galpy. The MWPotential2014 Milky Way potential (Bovy 2015) was adopted; the circular velocity was set to v0 = 220 km s−1 at a solar Galactocentric distance of 8 kpc. We also adopted the solar motion of Schönrich et al. (2010). Kinematic
Figure 2 of the paper
Figure 2. Stars are colour-shape coded, GSE stars are in red squares, halo stars are blue stars, thin-thick transition yellow circle, cyan diamonds thick disc stars and magenta triangles thin disc. Panel a) Cylindrical Galactocentric radius R vs. height above Galactic plane Z. Panel b) apocentre distance rap from Galactic centre vs maximum height over Galactic plane Zmax. Panel c) rap vs. pericentre distance from the Galactic centre rperi. Panel d) Cartesian coordinates X vs. Y. Panels e) and f) are a close-up of b) and c), excluding GSE stars; the zoom is performed over the area identified…
Figure 3 of the paper
Figure 3. a): Toomre diagram q V2 z + V 2 R vs. VT , where Vz , VR, VT are the stars’ velocity components in galactocentric cylindrical coordinates. b): VT vs. VR. c): E vs. Lz , orbital energy and angular momentum, respectively. d): eccentricity e vs. Lz . e): the radial action Jr vs. the azimuthal action Jϕ. f): the action diamond (Jz−Jr) Jtot vs. Jϕ Jtot , where Jz is the vertical action and Jtot = Jr + Jz + |Jϕ|. The colour code is the same as
Figure 4 of the paper
Figure 4. Abundances for alpha-elements. The abundance ratios are computed using Fe I for Mg, Si, Ca, and Ti I. Fe II abundances have been used to compute the ratios of O I and Ti II. The colour-shape code is the same as that defined in
Figure 5 of the paper
Figure 5. Panel a) through d) abundances for light odd-Z elements vs [Fe/H]. The panel presents chemical patterns for Na I, Al I, V I and Sc II. Panels e) through j) show abundances for iron-peak elements. their membership. Strontium displays a somewhat convex pat￾tern: Sr abundance drops with increasing metallicities, though at higher metallicity, this trend seems inverted, especially for thin disc stars. An interesting feature of these patterns (exclud￾ing Sr, Zr, and Eu) is that the scatter shrinks significantly around [Fe/H]=−1 dex. This is particularly evident in the variations of barium…
Figure 6 of the paper
Figure 6. Abundance ratios Sr I, Y II, Zr II, Ba II, La II, Ce II, Pr II, Nd II, Sm II, Eu II vs [Fe/H]. The smaller symbols are from previous MINCE papers. Panel k) highlights the quality of the analysis as the scatter in Nd and La is drastically reduced once they are combined. This also suggests that the scatter is real and likely not due to observational effects. The star TYC 5333-1917-1 is highlighted with a red cross superimposed. to be approximately at this metallicity value. Interestingly, the presence of a slightly subsolar-metallicity halo star shows a clear decline from the α…
Figure 7 of the paper
Figure 7. Magnesium abundances of MINCE GSE stars (red squares), su￾perimposed with a GCE model. The grey symbols are all the MINCE stars not belonging to GSE. 6.2. Light-odd elements Unlike alpha-elements, these elements have more heterogeneous nucleosynthetic origins. Sodium and Al are mainly produced during carbon burning in massive stars and released by core￾collapse supernovae (CCSNe), although additional late contri￾Article number, page 9
Figure 8 of the paper
Figure 8. [α/Fe] ratios of the sample stars plotted vs. [Fe/H]. The colour coding is the same as described in
Figure 9 of the paper
Figure 9. [Na/Al] vs. [Fe/H]. Showing [Na/Al] significantly reduces the scatter in the distribution of points, suggesting a shared production his￾tory for these two elements. even though there may be discrepancies in the absolute [X/Fe] values likely due to different methods employed in the analysis. Regarding light-odd elements, our results show very good agree￾ment with data from Ishigaki et al. (2013) in terms of overall trends, scatter, and absolute values. We also find general agree￾ment with the trends reported by Feuillet et al. (2021), although our absolute Al abundances tend to be…
Figure 11 of the paper
Figure 11. [Ba/Eu] ratio vs. [Fe/H] in GSE stars. In grey all MINCE non GSE stars. with observations (e.g. Burris et al. (2000); Beers & Christlieb (2005); Mashonkina et al. (2014); Lombardo et al. (2025)). In this work, 30 stars have [Ba/Eu]< 0, including seven with < −0.7, while only six have [Ba/Eu]> 0, all at [Fe/H] > -0.65 dex. According to Beers & Christlieb (2005), the majority of our sample is further classified as r − I stars, with +0.3 ≤ [Eu/Fe] ≤ +1. This suggests that these kind of stars are actu￾ally typical in this metallicity range, rather than having under￾gone peculiar…
Figure 12 of the paper
Figure 12. Comparison of [Y/Fe], [Ba/Fe], [Eu/Fe] abundance ratios vs. [Fe/H] with selected literature in figure a), b) and c) respectively. The bigger symbols represent MINCE data. with previous studies across the full metallicity range explored. For Ba, the abundances reported by Bensby et al. (2014) display a small systematic offset with respect to our measurements. This discrepancy may arise from differences in the adopted line list. In particular, our analysis consistently relies on the Ba II 5853,Å transition, which remains unsaturated over the metallicity range covered by our sample,…

Showing 11 of the paper's 12 figures. Figures are the authors', reproduced from the paper.

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