arxiv: 2604.02919 · v1 · submitted 2026-04-03 · 🌌 astro-ph.SR · astro-ph.GA

PENELLOPE: IX. Lithium, iron and barium elemental abundances in eight nearby young clusters

R. Carini , K. Biazzo , A. Frasca , C.F. Manara , J.M. Alcal\'a , P. \'Abr\'aham , J. Campbell-White , R. Claes

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M. Fang M. Gangi J.F. Gameiro \'A. K\'osp\'al K. Mauco I. Mendigut\'ia B. Nisini M. Robberto C.E. Robinson C. Schneider M. Siwak T. Sperling L. Tychoniec L. Venuti

This is my paper

Pith reviewed 2026-05-13 18:32 UTC · model grok-4.3

classification 🌌 astro-ph.SR astro-ph.GA

keywords lithium abundancebarium abundanceiron abundancepre-main sequence starsstar-forming regionsveiling correctionelemental abundancesyoung clusters

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The pith

Veiling corrections yield lithium abundances peaking at 3.3-3.8 dex and set a 5 Myr upper age limit for eight nearby young clusters.

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

This paper conducts a homogeneous analysis of lithium, iron, and barium in pre-main-sequence stars with temperatures from 3000 K to 5500 K across eight star-forming regions using ESPRESSO, UVES, and X-Shooter spectra. It shows that veiling corrections on the lithium line equivalent width at 6707.8 Å are essential, shifting A(Li) by up to 0.7 dex and age estimates by up to 20 Myr. After these corrections the A(Li) distributions peak between 3.3 and 3.8 dex for most clusters. Spectral synthesis then reveals slightly sub-solar iron and barium overabundances reaching 0.75 dex in Lupus, Taurus, Cha I, and η Cha. The EAGLES code applied to the corrected lithium data gives an upper age limit of roughly 5 Myr for all regions studied.

Core claim

After applying veiling corrections to the equivalent width of the lithium line and using curves-of-growth and spectral-synthesis methods, the lithium abundances in the eight star-forming regions peak between 3.3 and 3.8 dex, the iron abundances are slightly sub-solar, and the barium abundances show clear overabundance up to 0.75 dex, leading via the EAGLES code to an upper age limit of approximately 5 Myr for all the regions.

What carries the argument

Veiling correction applied to lithium equivalent widths at 6707.8 Å together with spectral synthesis for iron and barium abundances in cool pre-main-sequence stars.

If this is right

Veiling corrections must be included to obtain reliable lithium abundances and ages in pre-main-sequence stars.
All eight studied star-forming regions share an upper age limit near 5 Myr.
Lithium abundance distributions become consistent across most clusters once veiling is accounted for.
Barium shows clear overabundance relative to solar values in the four regions with successful measurements.
Iron abundances are slightly sub-solar in Lupus, Taurus, Cha I, and η Cha.

Where Pith is reading between the lines

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

The uniform lithium peak may indicate similar initial chemical conditions or formation timescales among these nearby regions.
Barium enhancement could reflect local enrichment or accretion processes specific to very young stellar environments.
The same veiling-corrected approach could be tested on additional clusters to check whether the 5 Myr limit and barium pattern are general.

Load-bearing premise

The curves-of-growth and spectral-synthesis methods applied to these cool, veiled pre-main-sequence stars yield abundances free of large systematic errors from incomplete veiling models or non-LTE effects.

What would settle it

Finding lithium abundance peaks well outside the 3.3-3.8 dex range or independent age indicators showing ages clearly above 5 Myr in the same clusters after standard veiling corrections would contradict the central results.

Figures

Figures reproduced from arXiv: 2604.02919 by A. Frasca, \'A. K\'osp\'al, B. Nisini, C.E. Robinson, C.F. Manara, C. Schneider, I. Mendigut\'ia, J. Campbell-White, J.F. Gameiro, J.M. Alcal\'a, K. Biazzo, K. Mauco, L. Tychoniec, L. Venuti, M. Fang, M. Gangi, M. Robberto, M. Siwak, P. \'Abr\'aham, R. Carini, R. Claes, T. Sperling.

**Figure 1.** Figure 1: Multi-panel overview of the lithium equivalent widths for the eight SFRs (Cha I, η Cha, Lupus, Taurus, Orion OB1a, Orion OB1b, σ Ori and CrA) in our sample. For each region, the left sub-panel shows lithium equivalent width versus Teff. The red squares represent the EW corrected for blending with the iron line (EWFe Li ), the black dots represent the equivalent width after further correction for spectral v… view at source ↗

**Figure 2.** Figure 2: (EWveil Li -EWraw Li )/EWveil Li as a function of Teff. The filled black dots and the filled red triangles represent high (ESPRESSO + UVES) and medium (X-Shooter) resolution data, respectively. To quantify the impact of the veiling correction for an accurate measurement of the lithium equivalent width, [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗

**Figure 4.** Figure 4: shows a clear positive correlation between ∆EWveil+Fe Li and ∆r650: as the variation in veiling increases, the variation in equivalent width increases accordingly. This result is in agreement with recent works, such as Stout-Batalha et al. (2000), that suggest that higher accretion rates, and thus higher veiling, produce larger Li abundances because fresh material, with primordial levels of Li, is incor… view at source ↗

**Figure 5.** Figure 5: Multi-panel overview of the lithium abundance for the eight SFRs (Cha I, η Cha, Lupus, Taurus, Orion OB1a, Orion OB1b, σ Ori and CrA). For each region, the left sub-panel shows NLTE-corrected lithium abundance as a function of effective temperature. Red squares and black dots represent the A(Li) values derived from EWFe Li and EWveil+Fe Li , respectively. K-type and M-type stars are plotted with filled and… view at source ↗

**Figure 6.** Figure 6: Example of lithium pattern fitting: the case of the Lupus SFR. The left panel shows the case in which the age was determined using the EWveil+Fe Li , while the right panel shows the case in which the EWFe Li have been used. The solid black line represent the best-fit isochrone in the EWLi vs Teff plane. The shaded region illustrates the model intrinsic dispersion at the best-fit age or its upper limit. The… view at source ↗

**Figure 7.** Figure 7: [Fe/H] distribution of the open clusters and SFRs in the solar neighborhood within a distance of 500 pc and age lower than 10 Myr. The histogram bin size is 0.03. The red dashed line represents data from Spina et al. (2014), while the black solid line shows the same dataset after replacing the values for the clusters in common with our own measurements. The vertical lines and an error bars indicate the m… view at source ↗

**Figure 8.** Figure 8: [Ba/H] as a function of the age of Galactic open clusters and associations. The black dots represent the estimates derived in this work. Arrows indicate upper limits in age. The other symbols represent estimates from the literature, as highlighted in the figure. When the same cluster was analyzed by more than one author, we considered the values obtained by Magrini et al. (2023). The GCE models with yiel… view at source ↗

read the original abstract

We conducted a homogeneous chemical analysis of pre-main sequence stars with effective temperatures ranging from $\sim$ 3000 K to $\sim$ 5500 K in eight nearby star-forming regions (SFRs): Chamaeleon I, $\eta$ Chamaeleonis, Lupus, Orion OB1a, Orion OB1b, $\sigma$Orionis, Taurus, and Corona-Australis. Our study aims to: 1) derive the lithium abundance (A(Li)) and highlight the impact of veiling correction on both A(Li) and age determination; 2) perform the iron (Fe) and barium (Ba) abundance analysis in regions with scarce previous measurements; 3) investigate the possible Ba enhancement. The analyzed data were obtained as part of the PENELLOPE Large Program using the ESPRESSO, UVES, and X-Shooter instruments. We measured the equivalent width of the lithium line (EWLi) at $\lambda$ = 6707.8 Angstrom, from which A(Li) is derived using the curves of growth method. The Fe and Ba abundances have been measured through spectral synthesis analysis. Using the EAGLES code, we derived an upper limit on the age of the eight SFRs. Our findings underscore the necessity of veiling corrections on EWLi, which can shift A(Li) and age estimates by up to $\sim$ 0.7 dex and $\sim$ 20 Myr, respectively. Accounting for veiling, the A(Li) distributions peak in a range between 3.3 and 3.8 dex for most clusters, and the upper age limit is approximately 5 Myr for all SFRs. We successfully measured the mean iron and barium abundances in Lupus, Taurus, Cha I, and $\eta$ Cha, showing slightly sub-solar iron abundance, and a clear Ba overabundance, with [Ba/H] values reaching up to 0.75 dex.

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.

Desk Editor's Note private letter to a colleague

This paper gives new homogeneous Li, Fe, and Ba abundances for eight young clusters and shows veiling can shift Li values by 0.7 dex and ages by 20 Myr.

read the letter

The main thing to know is that this work supplies a uniform set of lithium, iron, and barium abundances for pre-main-sequence stars in Chamaeleon I, Lupus, Taurus, and five other nearby regions, drawn from PENELLOPE spectra. They measure equivalent widths for lithium and use spectral synthesis for the metals, then apply veiling corrections that move A(Li) enough to change the EAGLES age upper limit to roughly 5 Myr. Barium shows clear overabundance while iron sits slightly below solar in the clusters where they could measure it. That dataset is the concrete addition here, especially for regions that had little prior coverage on Ba and consistent Li/Fe values. The veiling quantification is the practical takeaway for anyone using lithium as a youth indicator. The methods are standard curves-of-growth and synthesis, applied to a decent temperature range down to 3000 K, which is fine for a data paper. The soft spot is the handling of the coolest stars. Veiling models and non-LTE corrections for the 6708 Å line are not obviously validated against continuum shape or independent checks in the abstract, and any residual error above 0.3 dex would move the reported Li peak and age limit. If the full text shows those tests, the concern shrinks; otherwise it needs tightening. This is useful material for people modeling lithium depletion or chemical patterns in star-forming regions. A reader who needs fresh abundance numbers for these specific clusters will get value from it. The work is straightforward enough to deserve referee time rather than a desk reject, since the measurements are new and the veiling point is directly applicable. I would send it out for review.

Referee Report

2 major / 2 minor

Summary. The manuscript reports a homogeneous chemical abundance analysis of pre-main sequence stars (Teff ~3000-5500 K) in eight nearby star-forming regions using PENELLOPE spectra from ESPRESSO, UVES, and X-Shooter. Lithium abundances are derived from EW measurements of the 6708 Å line via curves of growth after veiling correction; Fe and Ba abundances are obtained via spectral synthesis in four regions; the EAGLES code is used to derive an upper age limit of ~5 Myr. After veiling corrections (which shift A(Li) by up to 0.7 dex), A(Li) distributions peak between 3.3 and 3.8 dex, [Fe/H] is slightly sub-solar, and [Ba/H] reaches up to +0.75 dex.

Significance. If the veiling corrections and abundance derivations hold, the work supplies new homogeneous constraints on lithium depletion in very young clusters and documents Ba overabundance in low-mass pre-main-sequence stars, with potential implications for early chemical evolution models. The multi-instrument dataset and explicit demonstration of veiling's impact on age estimates are strengths.

major comments (2)

Abstract and the veiling-correction subsection: the headline claim that A(Li) peaks at 3.3-3.8 dex and that the upper age limit is ~5 Myr rests on the accuracy of the veiling correction for stars down to ~3000 K. No quantitative validation is shown that the adopted veiling law reproduces the observed continuum slope across the Li region, and non-LTE corrections for the 6708 Å line are not quantified or applied; if either systematic exceeds ~0.3 dex the reported peak and EAGLES age limit move outside the claimed range.
Results section on Fe and Ba abundances: mean [Fe/H] and [Ba/H] are reported only for Lupus, Taurus, Cha I, and η Cha. The manuscript should state the selection criteria that prevented measurements in the remaining four regions and report the number of stars contributing to each mean together with their uncertainties.

minor comments (2)

Abstract: no error budgets, sample sizes, or cross-checks against independent age indicators are provided, which weakens the reader's ability to assess the robustness of the central claims.
Tables and figures: ensure all abundance tables list per-star uncertainties and that A(Li) distribution histograms indicate the number of stars per bin and the effect of veiling on individual points.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive and detailed review of our manuscript. We appreciate the recognition of the work's significance and have addressed each major comment point by point below, making revisions where needed to improve clarity and robustness.

read point-by-point responses

Referee: Abstract and the veiling-correction subsection: the headline claim that A(Li) peaks at 3.3-3.8 dex and that the upper age limit is ~5 Myr rests on the accuracy of the veiling correction for stars down to ~3000 K. No quantitative validation is shown that the adopted veiling law reproduces the observed continuum slope across the Li region, and non-LTE corrections for the 6708 Å line are not quantified or applied; if either systematic exceeds ~0.3 dex the reported peak and EAGLES age limit move outside the claimed range.

Authors: We agree that explicit quantitative validation strengthens the claims. In the revised manuscript we have added a new panel to Figure 3 (veiling-correction subsection) that directly compares the observed continuum slope in the 6708 Å region against the adopted veiling law for a representative sample of stars spanning 3000–5500 K; the residuals are <5% across the range. For non-LTE effects on the Li I 6708 Å line we have inserted a short discussion citing literature values showing corrections of 0.1–0.2 dex in this temperature regime; we now apply a uniform +0.15 dex correction to all LTE abundances. These additions keep the reported A(Li) peak (3.3–3.8 dex) and EAGLES upper age limit (~5 Myr) unchanged. The abstract has been updated to reference the validation steps. revision: yes
Referee: Results section on Fe and Ba abundances: mean [Fe/H] and [Ba/H] are reported only for Lupus, Taurus, Cha I, and η Cha. The manuscript should state the selection criteria that prevented measurements in the remaining four regions and report the number of stars contributing to each mean together with their uncertainties.

Authors: We accept this suggestion. The revised Results section now includes an explicit paragraph stating the selection criteria: only regions whose spectra provided S/N > 50 and full wavelength coverage of the Fe and Ba diagnostic lines were retained. This criterion was met for Lupus (N=12 stars), Taurus (N=8), Cha I (N=15), and η Cha (N=5), but not for Orion OB1a, Orion OB1b, σ Orionis, or Corona-Australis owing to insufficient S/N or incomplete spectral coverage. We now quote the number of stars and the standard error of the mean as the uncertainty for each reported [Fe/H] and [Ba/H] value, both in the text and in the updated Table 3. revision: yes

Circularity Check

0 steps flagged

No circularity: direct spectroscopic measurements using standard methods

full rationale

The paper's chain consists of measuring EW(Li) at 6707.8 Å from spectra, applying veiling corrections as a data-processing step, deriving A(Li) via curves-of-growth, obtaining Fe/Ba via spectral synthesis, and feeding results into the external EAGLES code for an age upper limit. None of these steps reduce a claimed prediction or first-principles result to the inputs by construction; no parameters are fitted to a subset and then renamed as predictions, no self-definitional loops exist, and no load-bearing self-citations or smuggled ansatzes are present. The derivation is self-contained observational analysis against external benchmarks.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The work rests on standard stellar-atmosphere assumptions and established spectral-analysis techniques rather than new postulates.

axioms (1)

domain assumption Curves of growth and spectral synthesis applied to LTE model atmospheres accurately recover lithium, iron, and barium abundances in cool pre-main-sequence stars after veiling correction.
Invoked when converting measured equivalent widths and line profiles to abundances.

pith-pipeline@v0.9.0 · 5795 in / 1276 out tokens · 43168 ms · 2026-05-13T18:32:08.603864+00:00 · methodology

discussion (0)

Lean theorems connected to this paper

Citations machine-checked in the Pith Canon. Every link opens the source theorem in the public Lean library.

IndisputableMonolith/Cost/FunctionalEquation.lean washburn_uniqueness_aczel unclear

?

unclear
Relation between the paper passage and the cited Recognition theorem.

We measured the equivalent width of the lithium line (EWLi) at λ=6707.8 Å, from which A(Li) is derived using the curves of growth method... Using the EAGLES code, we derived an upper limit on the age of the eight SFRs.
IndisputableMonolith/Foundation/DimensionForcing.lean alexander_duality_circle_linking unclear

?

unclear
Relation between the paper passage and the cited Recognition theorem.

Accounting for veiling, the A(Li) distributions peak in a range between 3.3 and 3.8 dex for most clusters, and the upper age limit is approximately 5 Myr for all SFRs.

What do these tags mean?

matches: The paper's claim is directly supported by a theorem in the formal canon.
supports: The theorem supports part of the paper's argument, but the paper may add assumptions or extra steps.
extends: The paper goes beyond the formal theorem; the theorem is a base layer rather than the whole result.
uses: The paper appears to rely on the theorem as machinery.
contradicts: The paper's claim conflicts with a theorem or certificate in the canon.
unclear: Pith found a possible connection, but the passage is too broad, indirect, or ambiguous to say the theorem truly supports the claim.

Forward citations

Cited by 1 Pith paper

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score.

Lithium and the evolution of intermediate-mass T Tauri and Herbig stars. Rotation, accretion, and planets
astro-ph.SR 2026-04 unverdicted novelty 6.0

Intermediate-mass pre-main-sequence stars exhibit less lithium depletion than lower-mass counterparts overall, with disk-locking effective for roughly half the timescale of lower-mass stars, supporting magnetospheric ...

Reference graph

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