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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

T0 review · 2 major / 1 minor · reviewed 2026-07-02 · grok-4.3

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Pith's one-line read Abundance ratios relative to oxygen, with stellar ages, reveal Milky Way disk population differences hidden in traditional [X/Fe] trends.

desk verdict 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. read the letter →

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

Thomas Bensby This is my paper
classification astro-ph.GAastro-ph.SR
keywords MilkyWaystellardiskchemicalabundancesthinandthickdisksFGdwarfsoxygenreferenceratiosGalacticevolutionagessolarneighbourhood
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

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.

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.

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

Extended reading notes

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.

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.

Editorial extensions

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.

Reading between the lines

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.
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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 · score 0.0 of 10

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.

Assumptions & free parameters 0 free parameters · 0 assumptions · 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.

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Cite this review

Pith. "Pith review of 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." pith.science (2026). https://pith.science/paper/CNAMLSJZ

@misc{pith2026260701013,
  author       = {Pith},
  title        = {Pith review of: 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},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/CNAMLSJZ}},
  note         = {Machine review of arXiv:2607.01013}
}
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 the authors.

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 differential line… view at source ↗
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 individual rea… view at source ↗
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 exhibiting l… view at source ↗
Figures from the paper (4 more)
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 abun…
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 Lucer…
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 th…
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: Differe…

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Works this paper leans on

124 extracted references · 124 canonical work pages

  1. [1]

    J., Carigi , L., Nissen , P

    Akerman , C. J., Carigi , L., Nissen , P. E., Pettini , M., & Asplund , M. 2004, , 414, 931

    work page 2004

  2. [2]

    Alexeeva , S. A. & Mashonkina , L. I. 2015, , 453, 1619

    work page 2015

  3. [3]

    M., Asplund , M., Collet , R., & Leenaarts , J

    Amarsi , A. M., Asplund , M., Collet , R., & Leenaarts , J. 2016, , 455, 3735

    work page 2016

  4. [4]

    M., Grevesse , N., Grumer , J., et al

    Amarsi , A. M., Grevesse , N., Grumer , J., et al. 2020 a , , 636, A120

    work page 2020

  5. [5]

    M., Li , W., Grevesse , N., & Jurewicz , A

    Amarsi , A. M., Li , W., Grevesse , N., & Jurewicz , A. J. G. 2025, , 703, A35

    work page 2025

  6. [6]

    M., Lind , K., Osorio , Y., et al

    Amarsi , A. M., Lind , K., Osorio , Y., et al. 2020 b , , 642, A62

    work page 2020

  7. [7]

    2018, , 473, 3377

    Andrievsky , S., Bonifacio , P., Caffau , E., et al. 2018, , 473, 3377

    work page 2018

  8. [8]

    M., Spite , M., Korotin , S

    Andrievsky , S. M., Spite , M., Korotin , S. A., et al. 2010, , 509, A88

    work page 2010

Show all 124 references
  1. [9]

    Ankush , B. K. & Deo , M. N. 2014, , 134, 21

    2014

  2. [10]

    1997, , 318, 521

    Asplund , M., Gustafsson , B., Kiselman , D., & Eriksson , K. 1997, , 318, 521

    1997

  3. [11]

    & Bensby , T

    Battistini , C. & Bensby , T. 2015, , 577, A9

    2015

  4. [12]

    & Bensby , T

    Battistini , C. & Bensby , T. 2016, , 586, A49

    2016

  5. [13]

    W., Koposov , S

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

    2018

  6. [14]

    2019, The Messenger, 175, 35

    Bensby , T., Bergemann , M., Rybizki , J., et al. 2019, The Messenger, 175, 35

    2019

  7. [15]

    & Feltzing , S

    Bensby , T. & Feltzing , S. 2006, , 367, 1181

    2006

  8. [16]

    2004, , 415, 155

    Bensby , T., Feltzing , S., & Lundstr \" o m , I. 2004, , 415, 155

    2004

  9. [17]

    Bensby , T., Feltzing , S., & Oey , M. S. 2014, , 562, A71

    2014

  10. [18]

    2021, , 655, A117

    Bensby , T., Gould , A., Asplund , M., et al. 2021, , 655, A117

    2021

  11. [19]

    & Lind , K

    Bensby , T. & Lind , K. 2018, , 615, A151

    2018

  12. [20]

    2026, , 708, A215

    Boin , T., Casamiquela , L., Haywood , M., et al. 2026, , 708, A215

    2026

  13. [21]

    2005, , 441, 533

    Caffau , E., Bonifacio , P., Faraggiana , R., et al. 2005, , 441, 533

    2005

  14. [22]

    2009, , 498, 877

    Caffau , E., Maiorca , E., Bonifacio , P., et al. 2009, , 498, 877

    2009

  15. [23]

    M., Racca , M., et al

    Caliskan , S., Amarsi , A. M., Racca , M., et al. 2025, , 696, A210

    2025

  16. [24]

    2009, , 505, 605

    Cescutti , G., Matteucci , F., McWilliam , A., & Chiappini , C. 2009, , 505, 605

    2009

  17. [25]

    Q., Nissen , P

    Chen , Y. Q., Nissen , P. E., Zhao , G., & Asplund , M. 2002, , 390, 225

    2002

  18. [26]

    2019, The Messenger, 175, 30

    Chiappini , C., Minchev , I., Starkenburg , E., et al. 2019, The Messenger, 175, 30

    2019

  19. [27]

    2003, , 339, 63

    Chiappini , C., Romano , D., & Matteucci , F. 2003, , 339, 63

    2003

  20. [28]

    2016, , 823, 102

    Choi , J., Dotter , A., Conroy , C., et al. 2016, , 823, 102

    2016

  21. [29]

    R., Delgado Mena , E., & Tsantaki , M

    Costa Silva , A. R., Delgado Mena , E., & Tsantaki , M. 2020, , 634, A136

    2020

  22. [30]

    2020, , 493, 5195

    Das , P., Hawkins , K., & Jofr \'e , P. 2020, , 493, 5195

    2020

  23. [31]

    M., Freeman , K

    De Silva , G. M., Freeman , K. C., Bland-Hawthorn , J., et al. 2015, , 449, 2604

    2015

  24. [32]

    C., et al

    Delgado Mena , E., Adibekyan , V., Santos , N. C., et al. 2021, , 655, A99

    2021

  25. [33]

    Z., et al

    Delgado Mena , E., Tsantaki , M., Adibekyan , V. Z., et al. 2017, , 606, A94

    2017

  26. [34]

    Demarque , P., Woo , J.-H., Kim , Y.-C., & Yi , S. K. 2004, , 155, 667

    2004

  27. [35]

    2016, , 222, 8

    Dotter , A. 2016, , 222, 8

    2016

  28. [36]

    2017, , 604, A128

    Duffau , S., Caffau , E., Sbordone , L., et al. 2017, , 604, A128

    2017

  29. [37]

    1993, , 275, 101

    Edvardsson , B., Andersen , J., Gustafsson , B., et al. 1993, , 275, 101

    1993

  30. [38]

    Ernandes , H., Barbuy , B., Fria c a , A. C. S., et al. 2020, , 640, A89

    2020

  31. [39]

    S., Carlsson , M., & Kiselman , D

    Fabbian , D., Asplund , M., Barklem , P. S., Carlsson , M., & Kiselman , D. 2009 a , , 500, 1221

    2009

  32. [40]

    2006, , 458, 899

    Fabbian , D., Asplund , M., Carlsson , M., & Kiselman , D. 2006, , 458, 899

    2006

  33. [41]

    E., Asplund , M., Pettini , M., & Akerman , C

    Fabbian , D., Nissen , P. E., Asplund , M., Pettini , M., & Akerman , C. 2009 b , , 500, 1143

    2009

  34. [42]

    K., Feltzing , S., Sahlholdt , C., & Bensby , T

    Feuillet , D. K., Feltzing , S., Sahlholdt , C., & Bensby , T. 2022, , 934, 21

    2022

  35. [43]

    2021, , 161, 9

    Franchini , M., Morossi , C., Di Marcantonio , P., et al. 2021, , 161, 9

    2021

  36. [44]

    2020, , 888, 55

    Franchini , M., Morossi , C., Di Marcantonio , P., et al. 2020, , 888, 55

    2020

  37. [45]

    & Bland-Hawthorn , J

    Freeman , K. & Bland-Hawthorn , J. 2002, , 40, 487

    2002

  38. [46]

    Gaia Collaboration , Prusti , T., de Bruijne , J. H. J., et al. 2016, , 595, A1

    2016

  39. [47]

    Gaia Collaboration , Vallenari , A., Brown , A. G. A., et al. 2023, , 674, A1

    2023

  40. [48]

    C., et al

    Gilmore , G., Randich , S., Worley , C. C., et al. 2022, , 666, A120

    2022

  41. [49]

    Giribaldi , R. E. & Smiljanic , R. 2023, , 673, A18

    2023

  42. [50]

    Grevesse , N., Asplund , M., & Sauval , A. J. 2007, Space Science Reviews, 130, 105

    2007

  43. [51]

    2021, , 508, 719

    Grisoni , V., Matteucci , F., & Romano , D. 2021, , 508, 719

    2021

  44. [52]

    2022, Universe, 8, 409

    Gustafsson , B. 2022, Universe, 8, 409

    2022

  45. [53]

    A., Eriksson , K., & Nordlund , A

    Gustafsson , B., Bell , R. A., Eriksson , K., & Nordlund , A. 1975, , 42, 407

    1975

  46. [54]

    2008, , 486, 951

    Gustafsson , B., Edvardsson , B., Eriksson , K., et al. 2008, , 486, 951

    2008

  47. [55]

    1999, , 342, 426

    Gustafsson , B., Karlsson , T., Olsson , E., Edvardsson , B., & Ryde , N. 1999, , 342, 426

    1999

  48. [56]

    2015, , 453, 758

    Hawkins , K., Jofr \'e , P., Masseron , T., & Gilmore , G. 2015, , 453, 758

    2015

  49. [57]

    H., et al

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

    2018

  50. [58]

    Henry , R. B. C., Edmunds , M. G., & K \"o ppen , J. 2000, , 541, 660

    2000

  51. [59]

    Ho , A. Y. Q., Rix , H.-W., Ness , M. K., et al. 2017, , 841, 40

    2017

  52. [60]

    P., Mackereth , J

    Horta , D., Schiavon , R. P., Mackereth , J. T., et al. 2023, , 520, 5671

    2023

  53. [61]

    2004, , 421, 649

    Israelian , G., Ecuvillon , A., Rebolo , R., et al. 2004, , 421, 649

    2004

  54. [62]

    & Rebolo , R

    Israelian , G. & Rebolo , R. 2001, , 557, L43

    2001

  55. [63]

    2017, , 604, A106

    Jean-Baptiste , I., Di Matteo , P., Haywood , M., et al. 2017, , 604, A106

    2017

  56. [64]

    W., Weinberg , D

    Johnson , J. W., Weinberg , D. H., Vincenzo , F., Bird , J. C., & Griffith , E. J. 2023, , 520, 782

    2023

  57. [65]

    I., & Lugaro , M

    Kobayashi , C., Karakas , A. I., & Lugaro , M. 2020, , 900, 179

    2020

  58. [66]

    A., Andrievsky , S

    Korotin , S. A., Andrievsky , S. M., & Zhukova , A. V. 2018, , 480, 965

    2018

  59. [67]

    A., Stempels , H

    Kupka , F., Piskunov , N., Ryabchikova , T. A., Stempels , H. C., & Weiss , W. W. 1999, , 138, 119

    1999

  60. [68]

    G., Ryabchikova , T

    Kupka , F. G., Ryabchikova , T. A., Piskunov , N. E., Stempels , H. C., & Weiss , W. W. 2000, Baltic Astronomy, 9, 590

    2000

  61. [69]

    2012, , 427, 50

    Lind , K., Bergemann , M., & Asplund , M. 2012, , 427, 50

    2012

  62. [70]

    2022, , 657, A29

    Lucertini , F., Monaco , L., Caffau , E., Bonifacio , P., & Mucciarelli , A. 2022, , 657, A29

    2022

  63. [71]

    2023, , 671, A137

    Lucertini , F., Monaco , L., Caffau , E., et al. 2023, , 671, A137

    2023

  64. [72]

    2017, , 603, A2

    Magrini , L., Randich , S., Kordopatis , G., et al. 2017, , 603, A2

    2017

  65. [73]

    2018, , 618, A102

    Magrini , L., Vincenzo , F., Randich , S., et al. 2018, , 618, A102

    2018

  66. [74]

    R., Schiavon , R

    Majewski , S. R., Schiavon , R. P., Frinchaboy , P. M., et al. 2017, , 154, 94

    2017

  67. [75]

    L., Sharma , S., Buder , S., et al

    Martell , S. L., Sharma , S., Buder , S., et al. 2017, , 465, 3203

    2017

  68. [76]

    & Gilmore , G

    Masseron , T. & Gilmore , G. 2015, , 453, 1855

    2015

  69. [77]

    Matrozis , E., Ryde , N., & Dupree , A. K. 2013, , 559, A115

    2013

  70. [78]

    2010, , 515, A68

    Mattsson , L. 2010, , 515, A68

    2010

  71. [79]

    G., et al

    Mel \'e ndez , J., Bergemann , M., Cohen , J. G., et al. 2012, , 543, A29

    2012

  72. [80]

    V., Kovtyukh , V

    Mishenina , T. V., Kovtyukh , V. V., Soubiran , C., Travaglio , C., & Busso , M. 2002, , 396, 189

    2002

  73. [81]

    W., et al

    Ness , M., Rix , H.-W., Hogg , D. W., et al. 2018, , 853, 198

    2018

  74. [82]

    Nissen , P. E. 2013, , 552, A73

    2013

  75. [83]

    Nissen , P. E. 2016, , 593, A65

    2016

  76. [84]

    E., Akerman , C., Asplund , M., et al

    Nissen , P. E., Akerman , C., Asplund , M., et al. 2007, , 469, 319

    2007

  77. [85]

    E., Chen , Y

    Nissen , P. E., Chen , Y. Q., Asplund , M., & Pettini , M. 2004, , 415, 993

    2004

  78. [86]

    E., Chen , Y

    Nissen , P. E., Chen , Y. Q., Carigi , L., Schuster , W. J., & Zhao , G. 2014, , 568, A25

    2014

  79. [87]

    2013, , 51, 457

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

    2013

  80. [88]

    V., Ryabchikova , T

    Pakhomov , Y. V., Ryabchikova , T. A., & Piskunov , N. E. 2019, Astronomy Reports, 63, 1010

    2019

  81. [89]

    2021, , 647, A162

    Perdigon , J., de Laverny , P., Recio-Blanco , A., et al. 2021, , 647, A162

    2021

  82. [90]

    Petigura , E. A. & Marcy , G. W. 2011, , 735, 41

    2011

  83. [91]

    & Valenti , J

    Piskunov , N. & Valenti , J. A. 2017, , 597, A16

    2017

  84. [92]

    E., Kupka , F., Ryabchikova , T

    Piskunov , N. E., Kupka , F., Ryabchikova , T. A., Weiss , W. W., & Jeffery , C. S. 1995, , 112, 525

    1995

  85. [93]

    2022, , 666, A121

    Randich , S., Gilmore , G., Magrini , L., et al. 2022, , 666, A121

    2022

  86. [94]

    & Magrini , L

    Randich , S. & Magrini , L. 2021, Frontiers in Astronomy and Space Sciences, 8, 6

    2021

  87. [95]

    E., Lambert , D

    Reddy , B. E., Lambert , D. L., & Allende Prieto , C. 2006, , 367, 1329

    2006

  88. [96]

    E., Tomkin , J., Lambert , D

    Reddy , B. E., Tomkin , J., Lambert , D. L., & Allende Prieto , C. 2003, , 340, 304

    2003

  89. [97]

    M., Lind , K., et al

    Reggiani , H., Amarsi , A. M., Lind , K., et al. 2019, , 627, A177

    2019

  90. [98]

    2022, , 30, 7

    Romano , D. 2022, , 30, 7

    2022

  91. [99]

    I., Tosi , M., & Matteucci , F

    Romano , D., Karakas , A. I., Tosi , M., & Matteucci , F. 2010, , 522, A32

    2010

  92. [100]

    & Matteucci , F

    Romano , D. & Matteucci , F. 2007, , 378, L59

    2007

  93. [101]

    J., & Ventura , P

    Romano , D., Matteucci , F., Zhang , Z.-Y., Ivison , R. J., & Ventura , P. 2019, , 490, 2838

    2019

  94. [102]

    L., et al

    Ryabchikova , T., Piskunov , N., Kurucz , R. L., et al. 2015, Physica Scripta, 90, 054005

    2015

  95. [103]

    A., Piskunov , N

    Ryabchikova , T. A., Piskunov , N. E., Kupka , F., & Weiss , W. W. 1997, Baltic Astronomy, 6, 244

    1997

  96. [104]

    & Lambert , D

    Ryde , N. & Lambert , D. L. 2004, , 415, 559

    2004

  97. [105]

    1993, , 414, 580

    Salaris , M., Chieffi , A., & Straniero , O. 1993, , 414, 580

    1993

  98. [106]

    R., Gehren , T., Zeng , J

    Shi , J. R., Gehren , T., Zeng , J. L., Mashonkina , L., & Zhao , G. 2014, , 782, 80

    2014

  99. [107]

    R., Yan , H

    Shi , J. R., Yan , H. L., Zhou , Z. M., & Zhao , G. 2018, , 862, 71

    2018

  100. [108]

    G., & Crocker , D

    Sneden , C., Gratton , R. G., & Crocker , D. A. 1991, , 246, 354

    1991

  101. [109]

    G., et al

    Spina , L., Magrini , L., Sacco , G. G., et al. 2022, , 668, A16

    2022

  102. [110]

    e , E., Chorniy , Y., Tautvai s ien \

    Stonkut \. e , E., Chorniy , Y., Tautvai s ien \. e , G., et al. 2020, , 159, 90

    2020

  103. [111]

    2026, , 1003, 27

    Storm , N., Bergemann , M., R \'o \.z a \'n ski , T., et al. 2026, , 1003, 27

    2026

  104. [112]

    2005, , 57, 751

    Takeda , Y., Hashimoto , O., Taguchi , H., et al. 2005, , 57, 751

    2005

  105. [113]

    1996, , 48, 511

    Takeda , Y., Kato , K.-I., Watanabe , Y., & Sadakane , K. 1996, , 48, 511

    1996

  106. [114]

    2016, , 68, 81

    Takeda , Y., Omiya , M., Harakawa , H., & Sato , B. 2016, , 68, 81

    2016

  107. [115]

    2002, , 54, 275

    Takeda , Y., Zhao , G., Chen , Y.-Q., Qiu , H.-M., & Takada-Hidai , M. 2002, , 54, 275

    2002

  108. [116]

    2015, , 807, 104

    Ting , Y.-S., Conroy , C., & Goodman , A. 2015, , 807, 104

    2015

  109. [117]

    Valenti , J. A. & Piskunov , N. 1996, , 118, 595

    1996

  110. [118]

    & Kobayashi , C

    Vincenzo , F. & Kobayashi , C. 2018, , 610, L16

    2018

  111. [119]

    2022, , 660, A135

    Viscasillas V \'a zquez , C., Magrini , L., Casali , G., et al. 2022, , 660, A135

    2022

  112. [120]

    2023, , 671, A171

    Wehrhahn , A., Piskunov , N., & Ryabchikova , T. 2023, , 671, A171

    2023

  113. [121]

    D., Shi , J

    Xu , X. D., Shi , J. R., & Yan , H. L. 2019, , 875, 142

    2019

  114. [122]

    L., Shi , J

    Yan , H. L., Shi , J. R., & Zhao , G. 2015, , 802, 36

    2015

  115. [123]

    W., Butler , K., Gehren , T., Shi , J

    Zhang , H. W., Butler , K., Gehren , T., Shi , J. R., & Zhao , G. 2006 a , , 453, 723

    2006

  116. [124]

    W., Gehren , T., Butler , K., Shi , J

    Zhang , H. W., Gehren , T., Butler , K., Shi , J. R., & Zhao , G. 2006 b , , 457, 645

    2006

Pith tools

Reviewed July 2, 2026 · model on record in the stance chip above.