Beryllium enhancement in stars of the accreted Thamnos-2 system

Elisabetta Caffau; Gabriele Cescutti; Lorenzo Monaco; Paolo Molaro; Piercarlo Bonifacio

REVIEW 2 major objections 5 minor 40 references

Beryllium enhancement in stars of the accreted Thamnos-2 system

T0 review · 2 major / 5 minor · reviewed 2026-07-10 · grok-4.5

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗

Pith's one-line read All known Be-rich stars belong to the accreted Thamnos-2 structure and point to a single hypernova-like spallation event.

desk verdict Solid new Be abundances that cleanly tag Thamnos-2; the hypernova story is plausible but the membership of the two literature stars is only qualitative. read the letter →

arxiv 2607.08179 v1 pith:A3UNODGH submitted 2026-07-09 astro-ph.SR

Paolo Molaro , Piercarlo Bonifacio , Elisabetta Caffau , Lorenzo Monaco , Gabriele Cescutti This is my paper

classification astro-ph.SR

keywords berylliumabundancesThamnosGalactichalosubstructuresspallationhypernovachemicaltagginglithiumaccreteddwarfgalaxies

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

This paper reports that every currently known star with an anomalous beryllium overabundance belongs to the same accreted halo substructure, Thamnos-2. Four newly analysed stars show clear Be excesses of 0.4–0.7 dex, and two previously known Be-rich stars are kinematically consistent with the same group. The Be enhancement tracks elevated silicon and neutron-capture elements, while the ratio of excess Be to excess Li is about 8–9, matching the expected yield ratio from spallation of energetic CNO nuclei. The authors argue that a single highly energetic event—most likely a hypernova—both produced the light elements by spallation and rapidly enriched the surrounding gas to [Fe/H] ≈ −1.5, explaining why these ~13 Gyr-old stars are relatively metal-rich. No comparable Be-rich population is known elsewhere in the Galaxy, so the chemical signature itself becomes a membership tag for Thamnos-2.

What carries the argument

The A(Be)/A(Li) excess ratio (~8–9) together with the Be–Si–n-capture abundance correlations. These ratios and trends are used as a chemical tag that both identifies the enrichment process (spallation by energetic CNO nuclei) and chemically tags membership in Thamnos-2.

What would settle it

A statistically significant sample of confirmed Thamnos-2 members that show normal Be abundances at the same metallicity, or a Be-rich star whose orbit and chemistry place it firmly outside Thamnos-2.

Watch

Extended reading notes

Core claim

All currently known Be-rich stars are associated with the Thamnos-2 structure. The Be excess is accompanied by elevated Si and a correlation with neutron-capture elements; the A(Be)/A(Li) excess ratio of ~8–9 matches spallation yields and is interpreted as the chemical fingerprint of a single hypernova-like event that also raised the ambient metallicity to [Fe/H] ≃ −1.5.

Load-bearing premise

That the observed Be–Si–n-capture correlations and the Be/Li excess ratio of ~8–9 were produced by one hypernova (or equivalent energetic event) whose ejecta mixed into roughly 10 000 solar masses of gas, rather than by several ordinary supernovae or other processes.

Editorial extensions

If this is right

Beryllium abundance becomes a practical chemical tag that can separate Thamnos-2 members from the more metal-poor Thamnos-1 and from in-situ halo contaminants.
The high [Si/Fe] and neutron-capture overabundances observed in Thamnos candidates can be re-interpreted as products of the same energetic event rather than ordinary chemical evolution or heavy in-situ contamination.
Old (~13 Gyr) stars can form at [Fe/H] ≈ −1.5 if a single hypernova rapidly pollutes a limited gas reservoir, relaxing the usual age–metallicity expectation for dwarf-galaxy debris.
The same light-element signature is not expected in other accreted systems (GSE, Sequoia proper), so absence of Be-rich stars elsewhere supports the uniqueness of the Thamnos-2 event.

Reading between the lines

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

If the hypernova interpretation holds, similar rare Be-rich populations could exist in other low-mass accreted dwarfs that experienced a single extreme explosion early in their history; targeted Be surveys of other retrograde substructures would test this.
The correlation of Be with neutron-capture elements suggests that the same event may have contributed an r-process component, offering a possible link between hypernovae and early heavy-element enrichment in dwarf galaxies.
Because the dilution mass required (~10^4 M⊙) is a tiny fraction of the estimated stellar mass of the Thamnos progenitor, the event need not have disrupted the whole galaxy, only a local star-forming cloud.

Share X Bluesky LinkedIn Reddit HN

Editorial analysis

A structured set of objections, weighed in public.

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

Desk Editor's Note

read the letter

The real news here is straightforward: four new Be-rich stars in Thamnos candidates, plus the two previously known Galactic Be-rich stars (HD 106038, HD 132475) sitting in the same E–Lz region, so that every known Be-rich star now looks associated with Thamnos-2. They also show a clear Be–Si correlation and a similar trend with the n-capture elements, and the Be/Li excess ratio in the two extreme cases is ~8–9, which matches the spallation cross-section ratio. That is new and useful for both Galactic archaeology and light-element nucleosynthesis.

The observational work is careful. Homogeneous UVES analysis with ATLAS9 + Turbospectrum + MyGIsFOS, direct profile fitting for Be and Li, Gaia-based parameters, and ages from SPInS + BASTI. The spectra and abundance tables look solid; the re-analysis of the two literature stars recovers earlier values. Membership for the new targets follows Feuillet et al. selection plus a posteriori E–Lz placement; Be is then used as a chemical tag rather than as the membership criterion, so the circularity burden is low.

The soft spots are real but limited. Sample size is ~10 stars, two of them only moderately enhanced. The hypernova + dilution calculation leans on one Fields et al. (2002) model and a free dilution mass of ~10^4 M⊙; it is a coherent hypothesis, not a unique proof. More importantly, the claim that “all currently known Be-rich stars” belong to Thamnos-2 rests, for HD 106038 and HD 132475, on a qualitative “same region of the diagram” statement rather than published membership probabilities or action-space distances. That is the weakest link in the strongest claim, though it does not erase the new abundances or the correlations.

This is for people working on halo substructures, chemical tagging, or Be/Li production. It deserves a serious referee; the data are good enough that the interpretation can be sharpened in review. I would engage with it and expect to cite the new Be measurements and the Thamnos association.

Referee Report

2 major / 5 minor

Summary. The paper reports homogeneous UVES abundances of Be and Li (plus a suite of heavier elements) for ten stars selected as Thamnos candidates, plus a reanalysis of the two previously known Be-rich stars HD 106038 and HD 132475. Four new stars show clear Be overabundances relative to the Galactic Be–Fe relation; two more are moderately elevated. All currently known Be-rich stars are argued to lie in the Thamnos-2 region of the (E, Lz) plane. The Be excess is accompanied by elevated [Si/Fe] and by a correlation with neutron-capture elements (Sr, Y, Zr, Ba), while O, Ca, Cr and V remain essentially flat. In the two most extreme objects the A(Be)/A(Li) excess ratio is ~8–9, matching spallation cross-section ratios. The authors interpret the pattern as the signature of a single hypernova (or equivalent energetic event) whose ejecta were diluted into ~10^4 M⊙ of pristine gas, rapidly enriching the gas to [Fe/H] ≃ −1.5 and explaining the high metallicities of these ~13 Gyr-old stars.

Significance. If the association of every known Be-rich star with Thamnos-2 holds, the result supplies a rare chemical tag for an accreted halo substructure and the first clear stellar evidence that a hypernova-scale spallation event can dominate light-element enrichment in a dwarf-galaxy progenitor. The homogeneous ATLAS9 + Turbospectrum + MyGIsFOS analysis, direct line-profile fitting of the Be II 313 nm doublet, and the clear Be–Si–n-capture correlations (Figs. 7–8) are solid technical contributions. The work also reinforces that unevolved stars from accreted systems share the same Spite-plateau Li abundance as the Galactic halo, thereby extending the cosmological lithium problem beyond the Milky Way.

major comments (2)

The load-bearing claim that “all currently known Be-rich stars appear associated with the Thamnos-2 structure” rests, for HD 106038 and HD 132475, solely on a qualitative statement that they “fall in the same region of the diagram” (Sect. 3.2 and Fig. 5 caption). No orbital integrals, action-space distances, or membership probabilities from Dodd et al. (2023) or any other catalogue are reported for these two objects. Because the subsequent hypernova interpretation is built on the premise that Be enhancement is unique to Thamnos-2, a quantitative kinematic membership assessment (or an explicit statement of the selection criteria used for these two stars) is required.
Sect. 4.2 and the dilution calculation that follows Fields et al. (2002) model (b) treat a single hypernova diluted into ~10^4 M⊙ as the preferred explanation. The same section notes that oxygen does not correlate with Be (Fig. 8), which is attributed to HN oxygen burning into Si. While the Be/Li excess ratio of ~8–9 is a strong spallation signature, the paper does not quantitatively exclude multiple ordinary CCSNe, a series of less energetic events, or residual selection effects within a mixed population (the contamination fraction discussed by Ceccarelli et al. 2025). A short quantitative comparison of expected yields and dilution masses for ordinary SNe versus HNe would strengthen the central interpretation.

minor comments (5)

Table 1 lists eleven programme stars plus BPM 3066; the abstract and conclusions speak of “nine stars” and “ten stars.” Clarify the final sample size consistently.
Fig. 5 caption and the surrounding text use both “Thamnos” and “Thamnos-2” without always distinguishing the two components defined by Koppelman et al. (2019). A brief reminder of the [Fe/H] and vφ cuts would help the reader.
The online CSV table of abundances is mentioned but not described; a short note on which solar scale and which NLTE corrections (if any) are applied for each species would improve reproducibility.
Typographical slips: “sellar explosion” in the keyword list; “turbospectrumand” missing a space (Methods); “a posteriori” is used correctly but “a posteriory” appears once in the text.
Ages derived with SPInS + BASTI are quoted with formal errors of 0.3–1 Gyr (Table 2), yet the discussion treats the ~13 Gyr clustering as essentially free of systematic uncertainty. A one-sentence caveat on isochrone systematics would be appropriate.

Circularity Check

1 steps flagged · score 1.0 of 10

Minor non-load-bearing self-citation of the authors' own prior Be-rich star (Monaco et al. 2025); new abundances, kinematics, and hypernova interpretation remain independent of that input.

self citation load bearing [Abstract / §1 / Table 2 (TS 0)]
"following the discovery of a Be-rich star BPM 3066 by Monaco et al. (2025). ... The results for BPM 3066 (TS 0) are taken from Monaco et al. (2025)."

BPM 3066 is the most extreme Be-rich object and is included as TS 0 with its A(Be)=2.10 taken directly from the authors' own prior paper (overlapping author list). This supplies the upper end of the claimed Thamnos-2 Be sequence and the clearest Li/Be excess ratio, but the new measurements of the other nine stars and the kinematic placement of the literature Be-rich stars are independent; the self-citation is therefore present yet not load-bearing for the central claim.

full rationale

The paper is an empirical abundance survey. Targets are selected from independent GALAH+Gaia dynamical criteria (Feuillet et al. 2021; Dodd et al. 2023 E–Lz plane), Be and Li are measured from new or archival UVES spectra with ATLAS9/Turbospectrum/MyGIsFOS, and the known Be-rich stars HD 106038/HD 132475 are re-analysed only for homogeneity (recovering literature values). The association of all known Be-rich stars with Thamnos-2 is an a-posteriori kinematic observation, not a definition. The A(Be)/A(Li) excess ratio ~8–9 and the dilution calculation are compared to external spallation cross-sections and Fields et al. (2002) hypernova yields; neither quantity is fitted from the present sample and then re-predicted. The sole self-citation of note is Monaco et al. (2025) for BPM 3066 (TS 0), which supplies one extreme data point and the same analysis pipeline; it is not used to define membership, abundances, or the hypernova scenario. No self-definitional loop, fitted-input-as-prediction, uniqueness theorem, or ansatz smuggling appears. Score 1 reflects only that minor, non-load-bearing self-citation.

Assumptions & free parameters 2 free parameters · 4 assumptions · 0 invented entities

The observational abundances rest on standard stellar-atmosphere and spectral-synthesis assumptions. The hypernova interpretation rests on literature yields and an ad-hoc dilution mass chosen to match the observed metallicities; no new free parameters are fitted to the Be data themselves.

free parameters (2)

dilution mass of pristine ISM = ~10^4 M⊙
Chosen as ~10^4 M⊙ so that Fields et al. (2002) hypernova yields reproduce the observed [Fe/H]≈−1.5 and Be levels; not independently measured.
stellar ages from SPInS + BASTI isochrones = 11.8–13.5 Gyr
Derived ages (11.8–13.5 Gyr) depend on the chosen isochrone set, Gaia photometry, and assumed distance/reddening; typical uncertainties 0.3–1 Gyr are quoted but systematic isochrone differences are not explored.

assumptions (4)

domain assumption ATLAS9 model atmospheres with KOALA ODFs and microturbulence 1 km s−1 adequately describe the stellar atmospheres for abundance work.
Standard assumption in the field; used throughout §3.1 to generate the synthetic grids.
domain assumption Spallation of energetic CNO on protons/α-particles produces 7Li and 9Be with a yield ratio ≈8–9 (Steigman & Walker 1992; Fields et al. 2002).
Invoked in §4 to interpret the observed excess A(Be)/A(Li) ratio as a spallation signature.
domain assumption Hypernova models of Fields et al. (2002) and Nomoto et al. (2013) correctly predict high Si yields and the absolute Li/Be masses used for the dilution argument.
Central to the hypernova scenario in §4.2; no alternative yield sets are tested.
domain assumption Kinematic selection in the (E, Lz) plane following Dodd et al. (2023) and Feuillet et al. (2021) correctly isolates Thamnos members.
Used for target selection (§2) and for associating HD 106038/HD 132475 with Thamnos.

how reviews work

0 comments

Cite this review

Pith. "Pith review of Beryllium enhancement in stars of the accreted Thamnos-2 system." pith.science (2026). https://pith.science/paper/A3UNODGH

@misc{pith2026260708179,
  author       = {Pith},
  title        = {Pith review of: Beryllium enhancement in stars of the accreted Thamnos-2 system},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/A3UNODGH}},
  note         = {Machine review of arXiv:2607.08179}
}

read the original abstract

Surveys of Galactic halo stars have revealed numerous streams and substructures tracing stellar populations accreted by the Milky Way. Among these, Gaia-Sausage-Enceladus (GSE) and Sequoia are the most prominent, both associated with dwarf galaxies accreted about 10 Gyr ago. We aim to measure beryllium abundances in nine stars associated with Thamnos, a substructure possibly linked to Sequoia, following the discovery of a Be-rich star BPM3066 by Monaco et al (2025). We used Gaia photometry and parallaxes to compute ATLAS9 model atmospheres. Synthetic spectra were generated with Turbospectrum and used with MyGIsFOS in single-model mode to analyze UVES high resolution spectra. Four new stars exhibit a significant beryllium overabundance. Moreover, the two known Be-rich stars, HD 106038 and HD 132475, are also found consistent with Thamnos membership. Thus, all currently known Be-rich stars appear associated with the Thamnos-2 structure. The Be enhancement is accompanied by elevated Si abundances, and we detect a correlation between Be and neutron-capture elements. No comparable Be-rich population is known elsewhere in the Galaxy, pointing to a rare enrichment event. The measured A(Be)/A(Li) excess ratio bears the imprint of spallation reactions, pointing to a highly energetic event in which fast CNO nuclei fragmented upon collision with the surrounding medium. The silicon overabundance is also consistent with a hypernova origin. Such an event may have rapidly enriched the surrounding gas to [Fe/H] about -1.5 explaining the relatively high metallicities of stars formed from this material despite their old ages (about 13 Gyr).

Figures

Figures reproduced from arXiv: 2607.08179 by the authors.

**Figure 1.** Spectral regions for the program stars around the BeII 313.0 nm doublet lines together with the best fit (red dots) for stars TS 1, TS 2, TS 3 and TS 4. 3.1. Chemical Abundances All spectra, both those acquired by us and those retrieved from the ESO archive, were analysed in a homogeneous manner. Stellar parameters were first determined using Gaia photometry and parallaxes, following the method described in Lombard… view at source ↗

**Figure 3.** As in [PITH_FULL_IMAGE:figures/full_fig_p003_3.png] view at source ↗

**Figure 2.** As in [PITH_FULL_IMAGE:figures/full_fig_p003_2.png] view at source ↗

Figures from the paper (4 more)

**Figure 5.** Figure 5: Galactic halo stars groups according to Dodd et al. (2023) with seven main groups indicated in different colours. The light green corresponds to Sequoia. The green is the hot thick disk and the Helmi Stream is magenta. The ED-1 (Emma Dodd 1) is orange. The GSE is in b…

**Figure 6.** Figure 6: Beryllium abundances versus ages for the program stars. The upper limit is for TS 9, which is the star likely belonging to Thamnos-1. This is the level of beryllium expected to be present in such old stars. Note that typical age uncertainties are of the order of about …

**Figure 7.** Figure 7: A(Be) is plotted against the [Si, Sr, Ba, Y, Zr/Fe] abundances. Empty symbols indicate the two Thamnos-1 stars. A strong correlation is found between the Be and Si abundances, spanning approximately 1.5 dex. A similar trend is observed for all the measured neutron-capt…

**Figure 8.** Figure 8: A(Be) is plotted against the [Cr, V, Ca, O/Fe] abundances. These elements exhibit minimal variation, remaining constant within 0.2 dex regardless of the Be abundance. it was plunging into the Galactic potential. However, all of the stars in Thamnos-2 should have been f…

Discussion (0). Sign in to comment.

Reference graph

Works this paper leans on

40 extracted references · 40 canonical work pages

[1]

L., Nissen, P

Asplund, M., Lambert, D. L., Nissen, P. E., Primas, F., & Smith, V . V . 2006, ApJ, 644, 229

work page 2006
[2]

W., Koposov, S

Belokurov, V ., Erkal, D., Evans, N. W., Koposov, S. E., & Deason, A. J. 2018, MNRAS, 478, 611

work page 2018
[3]

M., Rich, J

Boesgaard, A. M., Rich, J. A., Levesque, E. M., & Bowler, B. P. 2011, ApJ, 743, 140

work page 2011
[4]

2024, A&A, 691, A245

Caffau, E., Bonifacio, P., Monaco, L., et al. 2024, A&A, 691, A245

work page 2024
[5]

2025, A&A, 704, A180

Ceccarelli, E., Massari, D., Palla, M., et al. 2025, A&A, 704, A180

work page 2025
[6]

M., Helmi, A., et al

Dodd, E., Callingham, T. M., Helmi, A., et al. 2023, A&A, 670, L2

work page 2023
[7]

2025, A&A, 698, A277

Dodd, E., Ruiz-Lara, T., Helmi, A., et al. 2025, A&A, 698, A277

work page 2025
[8]

K., Sahlholdt, C

Feuillet, D. K., Sahlholdt, C. L., Feltzing, S., & Casagrande, L. 2021, MNRAS, 508, 1489

work page 2021

Show all 40 references

[9]

D., Daigne, F., Cassé, M., & Vangioni-Flam, E

Fields, B. D., Daigne, F., Cassé, M., & Vangioni-Flam, E. 2002, ApJ, 581, 389

2002
[10]

D., et al

Haywood, M., Di Matteo, P., Lehnert, M. D., et al. 2018, ApJ, 863, 113

2018
[11]

H., et al

Helmi, A., Babusiaux, C., Koppelman, H. H., et al. 2018, Nature, 563, 85

2018
[12]

C., Lehner, N., Fields, B

Howk, J. C., Lehner, N., Fields, B. D., & Mathews, G. J. 2012, Nature, 489, 121

2012
[13]

H., Helmi, A., Massari, D., Price-Whelan, A

Koppelman, H. H., Helmi, A., Massari, D., Price-Whelan, A. M., & Starkenburg, T. K. 2019, A&A, 631, L9

2019
[14]

Kurucz, R. L. 2005, Memorie della Societá Astronomica Italiana Supplementi, 8, 14

2005
[15]

& Reese, D

Lebreton, Y . & Reese, D. R. 2020, A&A, 642, A88

2020
[16]

2009, Landolt Börnstein [arXiv:0901.1149]

Lodders, K., Palme, H., & Gail, H.-P. 2009, Landolt Börnstein [arXiv:0901.1149]

2009 arXiv
[17]

2021, A&A, 656, A155

Lombardo, L., François, P., Bonifacio, P., et al. 2021, A&A, 656, A155

2021
[18]

& Beckman, J

Molaro, P. & Beckman, J. 1984, A&A, 139, 394

1984
[19]

1997, A&A, 319, 593

Molaro, P., Bonifacio, P., Castelli, F., & Pasquini, L. 1997, A&A, 319, 593

1997
[20]

Molaro, P., Bonifacio, P., Cupani, G., & Howk, J. C. 2024, A&A, 690, A38

2024
[21]

2020, MNRAS, 496, 2902

Molaro, P., Cescutti, G., & Fu, X. 2020, MNRAS, 496, 2902

2020
[22]

2010, A&A, 519, L3

Monaco, L., Bonifacio, P., Sbordone, L., Villanova, S., & Pancino, E. 2010, A&A, 519, L3

2010
[23]

2025, A&A, 697, A75

Monaco, L., Caffau, E., Molaro, P., Bonifacio, P., & Cescutti, G. 2025, A&A, 697, A75

2025
[24]

2026, A&A, 705, A134

Mucciarelli, A., Bonifacio, P., & Lardo, C. 2026, A&A, 705, A134

2026
[25]

2014, MNRAS, 444, 1812

Mucciarelli, A., Salaris, M., Bonifacio, P., Monaco, L., & Villanova, S. 2014, MNRAS, 444, 1812

2014
[26]

C., Vasiliev, E., Iorio, G., Evans, N

Myeong, G. C., Vasiliev, E., Iorio, G., Evans, N. W., & Belokurov, V . 2019, MNRAS, 488, 1235

2019
[27]

2013, ARA&A, 51, 457

Nomoto, K., Kobayashi, C., & Tominaga, N. 2013, ARA&A, 51, 457

2013
[28]

2021, ApJ, 908, 102

Pietrinferni, A., Hidalgo, S., Cassisi, S., et al. 2021, ApJ, 908, 102

2021
[29]

2025 [ascl:2504.012] Prodanovi´c, T., Bogdanovi´c, T., & Uroševi´c, D

Plez, B., Gerber, J., Magg, E., & Bergemann, M. 2025 [ascl:2504.012] Prodanovi´c, T., Bogdanovi´c, T., & Uroševi´c, D. 2013, Phys. Rev. D, 87, 103014 Prodanovi´c, T. & ´Ciprijanovi´c, A. 2019, 219, 417

2025
[30]

Reese, D. R. & Lebreton, Y . 2020, SPInS: Stellar Parameters INferred System- atically, Astrophysics Source Code Library, record ascl:2009.006

2020
[31]

A., & Hoyle, F

Reeves, H., Fowler, W. A., & Hoyle, F. 1970, Nature, 226, 727

1970
[32]

S., et al

Ruiz-Lara, T., Matsuno, T., Lövdal, S. S., et al. 2022, A&A, 665, A58

2022
[33]

2010, A&A, 522, A26

Sbordone, L., Bonifacio, P., Caffau, E., et al. 2010, A&A, 522, A26

2010
[34]

2014, Astronomy & Astro- physics, 564, A109

Sbordone, L., Caffau, E., Bonifacio, P., & Duffau, S. 2014, Astronomy & Astro- physics, 564, A109

2014
[35]

D., Martell, S

Simpson, J. D., Martell, S. L., Buder, S., et al. 2021, MNRAS, 507, 43

2021
[36]

2009, A&A, 499, 103

Smiljanic, R., Pasquini, L., Bonifacio, P., et al. 2009, A&A, 499, 103

2009
[37]

2008, MNRAS, 385, L93

Smiljanic, R., Pasquini, L., Primas, F., et al. 2008, MNRAS, 385, L93

2008
[38]

& Walker, T

Steigman, G. & Walker, T. P. 1992, ApJ, 385, L13

1992
[39]

F., Shi, J

Tan, K. F., Shi, J. R., & Zhao, G. 2009, MNRAS, 392, 205

2009
[40]

2024, MNRAS, 527, 7144 Article number, page 8 of 8

Wang, J., Hammer, F., Yang, Y ., et al. 2024, MNRAS, 527, 7144 Article number, page 8 of 8

2024

Pith tools

Reviewed July 10, 2026 · model on record in the stance chip above.

[1] [1]

L., Nissen, P

Asplund, M., Lambert, D. L., Nissen, P. E., Primas, F., & Smith, V . V . 2006, ApJ, 644, 229

work page 2006

[2] [2]

W., Koposov, S

Belokurov, V ., Erkal, D., Evans, N. W., Koposov, S. E., & Deason, A. J. 2018, MNRAS, 478, 611

work page 2018

[3] [3]

M., Rich, J

Boesgaard, A. M., Rich, J. A., Levesque, E. M., & Bowler, B. P. 2011, ApJ, 743, 140

work page 2011

[4] [4]

2024, A&A, 691, A245

Caffau, E., Bonifacio, P., Monaco, L., et al. 2024, A&A, 691, A245

work page 2024

[5] [5]

2025, A&A, 704, A180

Ceccarelli, E., Massari, D., Palla, M., et al. 2025, A&A, 704, A180

work page 2025

[6] [6]

M., Helmi, A., et al

Dodd, E., Callingham, T. M., Helmi, A., et al. 2023, A&A, 670, L2

work page 2023

[7] [7]

2025, A&A, 698, A277

Dodd, E., Ruiz-Lara, T., Helmi, A., et al. 2025, A&A, 698, A277

work page 2025

[8] [8]

K., Sahlholdt, C

Feuillet, D. K., Sahlholdt, C. L., Feltzing, S., & Casagrande, L. 2021, MNRAS, 508, 1489

work page 2021