Pith. sign in

REVIEW 3 major objections 5 minor 65 references

Tracing back a second-generation star stripped from Terzan 5 by the Galactic bar

T0 review · 3 major / 5 minor · reviewed 2026-08-12 · deepseek-v4-flash

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

Pith's one-line read The field star SOS1 was most likely stripped from Terzan 5 roughly 350 Myr ago by the Galactic bar, according to orbital traceback and chemical matching.

desk verdict The 2G chemistry is well supported and the traceback idea is genuinely new, but the dissociation-count statistic needs a null control before Terzan 5 can be called the parent. read the letter →

arxiv 2411.08096 v1 pith:2SBVGJPR submitted 2024-11-12 astro-ph.GA astro-ph.SR

Stefano O. Souza , Marica Valentini , Cristina Chiappini , Angeles Pérez-Villegas , Josefina Montalbán , Diego Bossini , Beatriz Barbuy , Yvonne Elsworth
show 1 more author
Rafael A. Garcia
This is my paper · ORCID
classification astro-ph.GAastro-ph.SR
keywords starsgalacticsos1bulgeterzanchemicalgalaxybuilding
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

Stars in globular clusters come in generations. In many clusters, a second generation forms from gas polluted by the first, carrying extra nitrogen, sodium, and aluminum. Such stars are rare in the ordinary field of the Milky Way, so when one appears far from any cluster, it is a candidate for having escaped from one. The authors found such a star, named SOS1, in the direction of the Galactic bulge, and used data from Gaia, APOGEE, and the K2 mission to measure its motion, distance, and chemical makeup.

This star is moving on an orbit that follows the Milky Way's bar. The team integrated its orbit backward in a model of the Galaxy's gravitational field and counted close encounters with all cataloged globular clusters. For Terzan 5, a massive and chemically unusual cluster near the Galactic center, they found more than 900 encounters in the last two billion years where the star was inside the cluster's tidal radius and gravitationally bound. For every other surviving cluster, they found zero such encounters. The most recent cluster of dissociation times is near 350 million years ago.

The chemical comparison is supportive but weaker. SOS1's iron content matches the most metal-poor population of Terzan 5, which is known from only three stars. The star's age, estimated from its carbon-to-nitrogen ratio after correcting for second-generation enrichment, is also consistent with Terzan 5's old age, although the correction itself assumes Terzan 5 was the parent. The authors caveat that a completely destroyed cluster cannot be excluded.

Extended reading notes

Core claim

The paper's central result is stated in Section 4: 'the dynamical results suggest that SOS1 was possibly gravitationally bound to Terzan 5 at -353 ± 12(±107) Myr ago.' If correct, SOS1 is a second-generation star originally belonging to Terzan 5's most metal-poor population, stripped by the Galactic bar, and this is the first chemodynamical tracing of a single non-stream field star back to a specific surviving globular cluster.

Load-bearing premise

The orbital traceback relies on a static, non-evolving Galactic potential (Sormani et al. 2022 approximation of Portail et al. 2017) with a fixed bar pattern speed, integrated 13 Gyr backward. The authors restrict trust to the last 2 Gyr and state that the boundedness criterion ignores dynamical friction and cluster evolution. If the bar potential or Terzan 5's orbit evolved significantly within the last roughly 1 Gyr, the more than 900 dissociation points in the 0 to -2 Gyr window could be artifacts. A second structural assumption is that the intact parent cluster must be among the observed Milky Way globular clusters, explicitly excluding a completely destroyed parent.

Share X Bluesky LinkedIn Reddit HN

Signed reviews

No signed human review yet.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 5 minor

Summary. The paper presents SOS1, an APOGEE/Gaia red giant in the inner Galaxy with a bar-trapped orbit and an abundance pattern (N, Al, Na enhancements, C depletion, Ce enhancement) typical of second-generation globular-cluster stars. The authors integrate orbits backward 13 Gyr in a fixed Sormani et al. (2022) approximation of the Portail et al. (2017) barred potential, select Galactic globular clusters with Jacobi energies within 1 sigma of SOS1, and compare 500 Monte Carlo orbital realizations per object (2.5e5 pair combinations). They count 'dissociation points' where SOS1 lies within a cluster's tidal radius and is energetically bound. Terzan 5 yields 3794 dissociation points (936 within the past 2 Gyr), versus at most 15 for any other surviving cluster; a GMM fit to the dissociation times gives tau_d1 = -353 +/- 12( +/- 107) Myr. The authors conclude that SOS1 was tidally stripped from Terzan 5's most metal-poor population (popC) by the Galactic bar and is a fossil record of early enrichment.

Significance. If correct, this would be the first chemodynamical tracing of an individual field star (not in a stream) back to a specific surviving globular cluster, with implications for Terzan 5's status as a bulge fossil fragment and for bar-driven cluster disruption. The paper's strengths include the use of independent external datasets (Gaia DR3, APOGEE DR17, Baumgardt & Vasiliev 2021, Portail et al. 2017), two independent spectral checks of the N and Al abundances (reference-star comparison and MOOG synthesis), transparent Monte Carlo uncertainties, and a clear statement of the caveats of the fixed potential. The dynamical identification, however, hinges on an uncalibrated count of orbital coincidences, and the paper contains internal inconsistencies in the quoted abundances; these issues must be addressed before the central claim is accepted.

major comments (3)
  1. [Section 3.2, Table 2] The dissociation-point statistic has no null control. Terzan 5 is by far the largest and most massive cluster in the selected sample (rt = 51.26 pc, M = 1.09e6 Msun), while the other candidates have rt between 10.98 and 33.88 pc and masses of roughly 1e4 to 6e5 Msun; because a dissociation point only requires entering the tidal sphere and being energetically bound in a fixed cluster potential, the expected encounter rate scales steeply with tidal radius and mass. Furthermore, SOS1 and Terzan 5 are both on bar-trapped orbits (Pbar = 84% and 94%), so their 500-orbit Monte Carlo ensembles may pass through the same volume repeatedly for geometric reasons. The factor of >200 in raw counts relative to all other clusters therefore cannot be interpreted as a likelihood ratio or false-positive rate without running the identical pipeline on a control sample of non-member field stars with the same measurement uncertainties. Please add such a null control, or otherwise calibrate the expected dissociation count under the hypothesis that SOS1 is not a member of Terzan 5.
  2. [Table 1; Section 5] The paper quotes internally inconsistent abundances: [N/Fe] is +1.15 in Table 1 but +0.71 in the Conclusions, [Al/Fe] is +0.96 in Table 1 but +0.31 in the Conclusions, and [Ce/Fe] is +0.43 in Table 1 but +0.60 in the Conclusions. Section 3.1 also describes the star as having '[N/Fe] > 1.0, [Al/Fe] > 1.0', which is not satisfied by the Table 1 value [Al/Fe] = +0.96. These differences are large enough to alter the qualitative chemical argument: with [Al/Fe] = +0.31 the star is much less extreme relative to the field than with +0.96. Please reconcile the tables and text and re-state the chemical characterization using the final adopted values.
  3. [Section 4; Appendix E] The [C/N]-based age estimate is not an independent confirmation of the Terzan 5 link. The 2G abundance correction is obtained by interpolating the Milone et al. (2018) variations to Terzan 5's mass (Appendix E, Eq. E2), and the same assumed Terzan 5 mass is then used to argue that the corrected [C/N] gives an age compatible with Terzan 5. The age compatibility is therefore partly built into the correction. Please either derive the correction without assuming Terzan 5's properties or explicitly state that the age is only a consistency check after assuming membership, not an independent line of evidence.
minor comments (5)
  1. [Section 2] The text refers to 'Apendix A' rather than 'Appendix A'.
  2. [Appendix B] The reference star is introduced as STARB but later referred to as 'SARTB' in the figure caption text; please make the spelling consistent.
  3. [References] The entries 'Rodrigues et al. 2017a' and 'Rodrigues et al. 2017b' share identical titles, journal, volume, and pages; if they are the same paper, the citation should be consolidated.
  4. [Figure 2] Figure 2 is described as an interactive figure; in a printed or static PDF version, the red dotted dissociation-point markers may not be legible. Please ensure a static version conveys the same information.
  5. [Appendix A] The error on A_V is reported as 'sigma_Av = 0.351 fit + 0.564 EW meas mag' with no explicit quadrature formula, while Table 1 lists AV = 4.48 +/- 0.92; please clarify how the total error is propagated and which error budget is adopted.
Assumptions & free parameters 2 free parameters · 5 assumptions · 0 invented entities

The central inference rests on adopted external models and assumptions: a static barred potential, the completeness of the observed globular cluster catalog for this purpose, and the standard second-generation interpretation of N and Al anomalies. No new physical entity is introduced. The only quantities close to free parameters are the GMM component count and the adopted 2G abundance correction, neither of which is fitted to SOS1's abundances as a model calibration.

free parameters (2)
  • GMM number of Gaussian components = 16
    Chosen by AIC to decompose the dissociation-time distribution; it determines which peaks are reported, including the 353 Myr peak.
  • 2G abundance correction for [C/N] = interpolated value for Terzan 5's mass, not quoted numerically
    Adopted from Milone et al. (2018) abundance variations and applied to SOS1 before age estimation; this input partly determines the age compatibility with Terzan 5.
assumptions (5)
  • domain assumption A static, non-evolving Galactic potential with fixed bar pattern speed is adequate for backward orbital integration.
    Invoked in Section 3.2 and Appendix C; the authors integrate 13 Gyr backward but explicitly say only the last 2 Gyr can be trusted, and the boundedness criterion ignores dynamical friction and cluster evolution.
  • domain assumption SOS1's parent cluster, if still intact, is among the 165 observed Milky Way globular clusters.
    Stated in Section 3.2: 'Assuming that the parent cluster of SOS1 is still orbiting the MW.' The destroyed-cluster scenario is explicitly deferred to future work.
  • domain assumption High N and Al abundances in a field star uniquely indicate a second-generation globular cluster star.
    Used in Section 3.1 to classify SOS1 as a 2G GC star, citing Carretta et al. 2009 and Gratton et al. 2012. This is the standard interpretation but is applied to a single field star.
  • domain assumption The Milone et al. (2018) 1G-to-2G abundance variation relations apply to Terzan 5's most metal-poor population and to SOS1.
    Used in Section 4 and Appendix E.2 to compute expected abundance ranges for chemical compatibility and to correct [C/N] before age derivation.
  • domain assumption The APOGEE DR17 abundances for SOS1, after the authors' spectral sanity checks, are accurate for the key light elements.
    The paper performs two validation tests in Appendix B, but the claimed [N/Fe] > 1 and [Al/Fe] near 1 depend on those checks and on ASPCAP systematics.

how reviews work

0 comments
Cite this review

Pith. "Pith review of Tracing back a second-generation star stripped from Terzan 5 by the Galactic bar." pith.science (2026). https://pith.science/paper/2SBVGJPR

@misc{pith2026241108096,
  author       = {Pith},
  title        = {Pith review of: Tracing back a second-generation star stripped from Terzan 5 by the Galactic bar},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/2SBVGJPR}},
  note         = {Machine review of arXiv:2411.08096}
}
read the original abstract

The Galactic bulge hosts the Milky Way's oldest stars, possibly coming from disrupted globular clusters (GCs) or the bulge's primordial building blocks, making these stars witnesses to the Galaxy's early chemical enrichment. The Galactic bar currently dominates the bulge's region, altering the orbits of objects formed before its formation and complicating the trace of the field stars' original clusters. Here, we present the discovery of a fossil record of this evolution, SOS1 -- a star trapped in the bar, exhibiting significant enhancements in nitrogen, sodium, and aluminum, typical of second-generation GC stars. SOS1 also shows an s-process Ce enhancement, suggesting an old age and early enrichment by fast-rotating massive stars in the Galaxy's earliest phases. With the purpose of finding the SOS1's parent GC, we derive its precise chemodynamical properties by combining high-precision proper motions from Gaia with APOGEE detailed chemical abundances. Our analysis suggests that SOS1 was possibly stripped from the GC Terzan 5 by the Galactic bar's gravitational influence approximately 350 Myr ago. We also found chemical similarities suggesting that SOS1 belonged to the most metal-poor, ancient, and peripheral stellar population of Terzan 5. These results not only support the hypothesis that Terzan 5 is a remnant of a primordial building block of the Galactic bulge, but also suggest this cluster continues losing stars to the bar. Our method highlights how powerful the use of chemodynamical properties in the Gaia era is for tracing the Galaxy's evolutionary history.

Figures

Figures reproduced from arXiv: 2411.08096 by the authors.

Figure 1
Figure 1. Chemo-dynamical properties of SOS1. a, X-Y and X-Z density projections of the Galaxy with the orbit of SOS1 star (red line). b, abundances of and light-elements for SOS1 (yellow star symbol) compared with field stars in the inner Galaxy (density plot). c, the left panel shows the Jacobi energy of the GCs compatible within 1σ with SOS1 (shaded yellow region), and the right panel shows the SOS1 distance to the centre … view at source ↗
Figure 3
Figure 3. Dissociation time calculation. The gray histogram shows the distribution of lookback time obtained from the dissociation points. The black solid line shows the multiple Gaussian distribution obtained through the GMM fitting, and the individual Gaussians are as black thin dashed lines. The two significant dissociation times τd1 and τd2 are highlighted as red and yellow lines, respectively. The number above each Gauss… view at source ↗
Figure 2
Figure 2. Dissociation point selection criteria (Inter￾active figure). The top panel shows the SOS1 distance to GC’s centre in units of tidal radius as a function of time. The black horizontal dotted line shows the tidal radius region lim￾iting the cluster volume. The bottom panel shows the SOS1 total energy with respect to the GC as a function of time. The black horizontal dotted line represents the bound energy limit. The r… view at source ↗
Figures from the paper (4 more)
Figure 4
Figure 4. Figure 4: Chrono-Chemical comparison between SOS1 and Terzan 5 [PITH_FULL_IMAGE:figures/full_fig_p007_4.png]
Figure 5
Figure 5. Figure 5: Verification of the APOGEE-ASPCAP abundances of Al (upper panels) and N (bottom panels): comparison of spectra of the sample star SOS1 (red line) with a reference star (STARB) with similar stellar parameters and solar abundances (blue line) [PITH_FULL_IMAGE:figures/fu…
Figure 6
Figure 6. Figure 6: Verification of APOGEE-ASPCAP abundances. Upper panels: Spectrum synthesis of Al. The coloured lines repre￾sent synthetic spectra with no Al abundance (blue), solar Al abundance (orange), and [Al/Fe]= 1.17 (green, the value provided by APOGEE). Bottom panels: Spectrum …
Figure 7
Figure 7. Figure 7: Derivation of the abundance contribution for the elements O, Mg, Si, C, Al, and N due to the MPs. Baumgardt, H., & Vasiliev, E. 2021, MNRAS, 505, 5957, doi: 10.1093/mnras/stab1474 Bica, E., Ortolani, S., Barbuy, B., & Oliveira, R. A. P. 2024, A&A, 687, A201, doi: 10.10…

Discussion (0). Continue with ORCID to comment.

Reference graph

Works this paper leans on

65 extracted references · 11 canonical work pages

  1. [1]

    , " * write output.state after.block = add.period write newline

    ENTRY address archivePrefix author booktitle chapter doi edition editor eprint howpublished institution journal key month number organization pages publisher school series title misctitle type volume year version url label extra.label sort.label short.list INTEGERS output.state before.all mid.sentence after.sentence after.block FUNCTION init.state.consts ...

  2. [2]

    write newline

    " write newline "" before.all 'output.state := FUNCTION format.url url empty "" new.block "" url * "" * if FUNCTION format.eprint eprint empty "" archivePrefix empty "" archivePrefix "arXiv" = new.block " " eprint * " " * new.block " " eprint * " " * if if if FUNCTION format.doi doi empty "" " " doi * " " * if FUNCTION format.pid doi empty eprint empty ur...

  3. [3]

    Ѐ 3gjڴiںuUV R!Ѐr͚5KO<6nRnz'7 @ ̾.eɒ h @ ; ! w 4C h ŋ +;;[Ǐ W -d ]V 2zwQ ;veTD Wdd H_U ڴiq_V۶m T?Y)))JLL3<S?**J>̻RSS=ꫯԩS' T &Od_ӧOu9u05mcX & WczRy<g Xxy6l6sakL< V6Dx =zTǎ TLۧ ｷ

    thebibliography [1] 20pt to REFERENCES 6pt =0pt -12pt 10pt plus 3pt =0pt =0pt =1pt plus 1pt =0pt =0pt -12pt =13pt plus 1pt =20pt =13pt plus 1pt \@M =10000 =-1.0em =0pt =0pt 0pt =0pt =1.0em @enumiv\@empty 10000 10000 `\.\@m \@noitemerr \@latex@warning Empty `thebibliography' environment \@ifnextchar \@reference \@latexerr Missing key on reference command E...

    2021

  4. [4]

    2022, , 259, 35, 10.3847/1538-4365/ac4414

    Abdurro'uf , Accetta , K., Aerts , C., et al. 2022, , 259, 35, 10.3847/1538-4365/ac4414

    doi:10.3847/1538-4365/ac4414 2022

  5. [5]

    J., & Scott , P

    Asplund , M., Grevesse , N., Sauval , A. J., & Scott , P. 2009, , 47, 481, 10.1146/annurev.astro.46.060407.145222

    arXiv 2009

  6. [6]

    2018, , 56, 223, 10.1146/annurev-astro-081817-051826

    Barbuy , B., Chiappini , C., & Gerhard , O. 2018, , 56, 223, 10.1146/annurev-astro-081817-051826

    doi:10.1146/annurev-astro-081817-051826 2018

  7. [7]

    2018, , 478, 1520, 10.1093/mnras/sty1057

    Baumgardt , H., & Hilker , M. 2018, , 478, 1520, 10.1093/mnras/sty1057

    doi:10.1093/mnras/sty1057 2018

  8. [8]

    2021, , 505, 5957, 10.1093/mnras/stab1474

    Baumgardt , H., & Vasiliev , E. 2021, , 505, 5957, 10.1093/mnras/stab1474

    doi:10.1093/mnras/stab1474 2021

Show all 65 references
  1. [9]

    Bica , E., Ortolani , S., Barbuy , B., & Oliveira , R. A. P. 2024, , 687, A201, 10.1051/0004-6361/202346377

    2024 doi

  2. [10]

    2017, , 469, 4718, 10.1093/mnras/stx1135

    Bossini , D., Miglio , A., Salaris , M., et al. 2017, , 469, 4718, 10.1093/mnras/stx1135

    2017 doi

  3. [11]

    W., Hunt , J

    Bovy , J., Leung , H. W., Hunt , J. A. S., et al. 2019, , 490, 4740, 10.1093/mnras/stz2891

    2019 doi

  4. [12]

    2009, , 508, 695, 10.1051/0004-6361/200913003

    Carretta , E., Bragaglia , A., Gratton , R., D'Orazi , V., & Lucatello , S. 2009, , 508, 695, 10.1051/0004-6361/200913003

    2009 doi

  5. [13]

    2019, , 629, A62, 10.1051/0004-6361/201935282

    Casali , G., Magrini , L., Tognelli , E., et al. 2019, , 629, A62, 10.1051/0004-6361/201935282

    2019 doi

  6. [14]

    2011, , 472, 454, 10.1038/nature10000

    Chiappini , C., Frischknecht , U., Meynet , G., et al. 2011, , 472, 454, 10.1038/nature10000

    2011 doi

  7. [15]

    P., & Giuli , R

    Cox , J. P., & Giuli , R. T. 1968, Principles of stellar structure

    1968

  8. [16]

    R., et al

    Crociati , C., Valenti , E., Ferraro , F. R., et al. 2023, , 951, 17, 10.3847/1538-4357/acd382

    2023 doi

  9. [17]

    P., Liddicott , D

    Debattista , V. P., Liddicott , D. J., Gonzalez , O. A., et al. 2023, , 946, 118, 10.3847/1538-4357/acbb00

    2023 doi

  10. [18]

    Elyajouri , M., Lallement , R., Monreal-Ibero , A., Capitanio , L., & Cox , N. L. J. 2017, , 600, A129, 10.1051/0004-6361/201630088

    2017 doi

  11. [19]

    G., Zamora , O., Souto , D., et al

    Fern \'a ndez-Trincado , J. G., Zamora , O., Souto , D., et al. 2019, , 627, A178, 10.1051/0004-6361/201834391

    2019 doi

  12. [20]

    G., Beers , T

    Fern \'a ndez-Trincado , J. G., Beers , T. C., Barbuy , B., et al. 2022, , 663, A126, 10.1051/0004-6361/202243195

    2022 doi

  13. [21]

    R., Massari , D., Dalessandro , E., et al

    Ferraro , F. R., Massari , D., Dalessandro , E., et al. 2016, , 828, 75, 10.3847/0004-637X/828/2/75

    2016 doi

  14. [22]

    R., Dalessandro , E., Mucciarelli , A., et al

    Ferraro , F. R., Dalessandro , E., Mucciarelli , A., et al. 2009, , 462, 483, 10.1038/nature08581

    2009 doi

  15. [23]

    2016, , 456, 1803

    Frischknecht , U., Hirschi , R., Pignatari , M., et al. 2016, , 456, 1803

    2016

  16. [24]

    2018, , 616, A12, 10.1051/0004-6361/201832698

    Gaia Collaboration , Helmi , A., van Leeuwen , F., et al. 2018, , 616, A12, 10.1051/0004-6361/201832698

    2018 doi

  17. [25]

    E., Allende Prieto , C., Holtzman , J

    Garc \' a P \'e rez , A. E., Allende Prieto , C., Holtzman , J. A., et al. 2016, , 151, 144, 10.3847/0004-6256/151/6/144

    2016 doi

  18. [26]

    G., Carretta , E., & Bragaglia , A

    Gratton , R. G., Carretta , E., & Bragaglia , A. 2012, , 20, 50, 10.1007/s00159-012-0050-3

    2012 doi

  19. [27]

    2024, , 631, 285, 10.1038/s41586-024-07511-z

    H \"a berle , M., Neumayer , N., Seth , A., et al. 2024, , 631, 285, 10.1038/s41586-024-07511-z

    2024 doi

  20. [28]

    P., Mackereth , J

    Horta , D., Schiavon , R. P., Mackereth , J. T., et al. 2021, , 500, 1385, 10.1093/mnras/staa2987

    2021 doi

  21. [29]

    B., Sobeck, C., Haas, M., et al

    Howell, S. B., Sobeck, C., Haas, M., et al. 2014, Publications of the Astronomical Society of the Pacific, 126, 398, 10.1086/676406

    2014 doi

  22. [30]

    2019, in Bulletin of the American Astronomical Society, Vol

    Kahn , S., Ivezi \'c , Z., Ritz , S., et al. 2019, in Bulletin of the American Astronomical Society, Vol. 51, 273, 10.48550/arXiv.1907.10487

    2019 doi arXiv

  23. [31]

    Kjeldsen , H., & Bedding , T. R. 1995, , 293, 87, 10.48550/arXiv.astro-ph/9403015

    1995 doi arXiv

  24. [32]

    2014, Science, 345, 791, 10.1126/science.1253171

    Kos , J., Zwitter , T., Wyse , R., et al. 2014, Science, 345, 791, 10.1126/science.1253171

    2014 doi

  25. [33]

    C., Reyl \'e , C., & Nasello , G

    Lagarde , N., Robin , A. C., Reyl \'e , C., & Nasello , G. 2017, , 601, A27, 10.1051/0004-6361/201630253

    2017 doi

  26. [34]

    R., Dalessandro , E., et al

    Lanzoni , B., Ferraro , F. R., Dalessandro , E., et al. 2010, , 717, 653, 10.1088/0004-637X/717/2/653

    2010 doi

  27. [35]

    O., P \'e rez-Villegas , A., et al

    Limberg , G., Souza , S. O., P \'e rez-Villegas , A., et al. 2022, , 935, 109, 10.3847/1538-4357/ac8159

    2022 doi

  28. [36]

    2015, , 453, 1855, 10.1093/mnras/stv1731

    Masseron , T., & Gilmore , G. 2015, , 453, 1855, 10.1093/mnras/stv1731

    2015 doi

  29. [37]

    Merrow , A., Grand , R. J. J., Fragkoudi , F., & Martig , M. 2024, , 531, 1520, 10.1093/mnras/stae1250

    2024 doi

  30. [38]

    A., et al

    M \'e sz \'a ros , S., Masseron , T., Garc \' a-Hern \'a ndez , D. A., et al. 2020, , 492, 1641, 10.1093/mnras/stz3496

    2020 doi

  31. [39]

    P., Marino , A

    Milone , A. P., Marino , A. F., Di Criscienzo , M., et al. 2018, , 477, 2640, 10.1093/mnras/sty661

    2018 doi

  32. [40]

    G., et al

    Minniti , D., Matsunaga , N., Fern \'a ndez-Trincado , J. G., et al. 2024, , 683, A150, 10.1051/0004-6361/202348100

    2024 doi

  33. [41]

    G., P \'e rez-Villegas , A., Chaves-Velasquez , L., & Schuster , W

    Moreno , E., Fern \'a ndez-Trincado , J. G., P \'e rez-Villegas , A., Chaves-Velasquez , L., & Schuster , W. J. 2022, , 510, 5945, 10.1093/mnras/stab3724

    2022 doi

  34. [42]

    2024, , 681, L8, 10.1051/0004-6361/202348365

    Nepal , S., Chiappini , C., Guiglion , G., et al. 2024, , 681, L8, 10.1051/0004-6361/202348365

    2024 doi

  35. [43]

    2020, , 28, 4, 10.1007/s00159-020-00125-0

    Neumayer , N., Seth , A., & B \"o ker , T. 2020, , 28, 4, 10.1007/s00159-020-00125-0

    2020 doi

  36. [44]

    M., et al

    Origlia , L., Massari , D., Rich , R. M., et al. 2013, , 779, L5, 10.1088/2041-8205/779/1/L5

    2013 doi

  37. [45]

    M., Ferraro , F

    Origlia , L., Rich , R. M., Ferraro , F. R., et al. 2011, , 726, L20, 10.1088/2041-8205/726/2/L20

    2011 doi

  38. [46]

    B., et al

    Paxton , B., Schwab , J., Bauer , E. B., et al. 2018, , 234, 34, 10.3847/1538-4365/aaa5a8

    2018 doi

  39. [47]

    O., et al

    P \'e rez-Villegas , A., Barbuy , B., Kerber , L. O., et al. 2020, , 491, 3251, 10.1093/mnras/stz3162

    2020 doi

  40. [48]

    2017, , 465, 1621, 10.1093/mnras/stw2819

    Portail , M., Gerhard , O., Wegg , C., & Ness , M. 2017, , 465, 1621, 10.1093/mnras/stw2819

    2017 doi

  41. [49]

    2015, , 450, L66, 10.1093/mnrasl/slv048

    Portail , M., Wegg , C., & Gerhard , O. 2015, , 450, L66, 10.1093/mnrasl/slv048

    2015 doi

  42. [50]

    Queiroz , A. B. A., Chiappini , C., Perez-Villegas , A., et al. 2021, , 656, A156, 10.1051/0004-6361/202039030

    2021 doi

  43. [51]

    Queiroz , A. B. A., Anders , F., Chiappini , C., et al. 2023, , 673, A155, 10.1051/0004-6361/202245399

    2023 doi

  44. [52]

    C., et al

    Razera , R., Barbuy , B., Moura , T. C., et al. 2022, , 517, 4590, 10.1093/mnras/stac2136

    2022 doi

  45. [54]

    2017 b , , 467, 1433, 10.1093/mnras/stx120

    ---. 2017 b , , 467, 1433, 10.1093/mnras/stx120

    2017 doi

  46. [55]

    R., Origlia , L., et al

    Romano , D., Ferraro , F. R., Origlia , L., et al. 2023, , 951, 85, 10.3847/1538-4357/acd8ba

    2023 doi

  47. [56]

    M., & Cassisi , S

    Salaris , M., Pietrinferni , A., Piersimoni , A. M., & Cassisi , S. 2015, , 583, A87, 10.1051/0004-6361/201526951

    2015 doi

  48. [57]

    V., Cunha , K., Smith , V

    Sales-Silva , J. V., Cunha , K., Smith , V. V., et al. 2024, , 965, 119, 10.3847/1538-4357/ad28c2

    2024 doi

  49. [58]

    2012, MOOG: LTE line analysis and spectrum synthesis , Astrophysics Source Code Library, record ascl:1202.009

    Sneden , C., Bean , J., Ivans , I., Lucatello , S., & Sobeck , J. 2012, MOOG: LTE line analysis and spectrum synthesis , Astrophysics Source Code Library, record ascl:1202.009. 1202.009

    2012

  50. [59]

    C., Gerhard , O., Portail , M., Vasiliev , E., & Clarke , J

    Sormani , M. C., Gerhard , O., Portail , M., Vasiliev , E., & Clarke , J. 2022, , 514, L1, 10.1093/mnrasl/slac046

    2022 doi

  51. [60]

    O., Ernandes , H., Valentini , M., et al

    Souza , S. O., Ernandes , H., Valentini , M., et al. 2023, , 671, A45, 10.1051/0004-6361/202245286

    2023 doi

  52. [61]

    O., Libralato , M., Nardiello , D., et al

    Souza , S. O., Libralato , M., Nardiello , D., et al. 2024, arXiv e-prints, arXiv:2407.15918, 10.48550/arXiv.2407.15918

    2024 doi arXiv

  53. [62]

    M., et al

    Spoo , T., Tayar , J., Frinchaboy , P. M., et al. 2022, , 163, 229, 10.3847/1538-3881/ac5d53

    2022 doi

  54. [63]

    R., & Origlia , L

    Valenti , E., Ferraro , F. R., & Origlia , L. 2007, , 133, 1287, 10.1086/511271

    2007 doi

  55. [64]

    2019, , 482, 1525, 10.1093/mnras/sty2672

    Vasiliev , E. 2019, , 482, 1525, 10.1093/mnras/sty2672

    2019 doi

  56. [65]

    C., K ro g lu , F., Fragione , G., et al

    Weatherford , N. C., K ro g lu , F., Fragione , G., et al. 2023, , 946, 104, 10.3847/1538-4357/acbcc1

    2023 doi

  57. [66]

    M., Clarke , J

    Wylie , S. M., Clarke , J. P., & Gerhard , O. E. 2022, , 659, A80, 10.1051/0004-6361/202142343

    2022 doi

Pith tools

Reviewed August 12, 2026 · model on record in the stance chip above.