pith. sign in

arxiv: 2511.06820 · v2 · submitted 2025-11-10 · 🌌 astro-ph.GA · astro-ph.SR

APOGEE chemical abundances of stars in the MW satellites Fornax, Sextans, Draco and Carina

Cheng Xu , Yi Qiao , Baitian Tang , Jos\'e G. Fern\'andez-Trincado , Zhiqiang Yan , Doug Geisler This is my paper

Pith reviewed 2026-05-18 00:14 UTC · model grok-4.3

classification 🌌 astro-ph.GA astro-ph.SR
keywords dwarf galaxieschemical abundancesAPOGEE surveyMilky Way satellitesalpha elementsgalaxy masschemical evolutionFornax
0
0 comments X

The pith

Alpha-element ratios in four Milky Way dwarf satellites correlate directly with galaxy luminosity and mass.

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

The paper measures abundances of iron, carbon, nitrogen, oxygen, magnesium, aluminum, silicon, calcium, titanium, chromium, manganese, nickel and cerium in 74 stars across Fornax, Sextans, Draco and Carina using APOGEE near-infrared spectra. It finds that alpha-element ratios such as silicon over iron vary systematically with each galaxy's luminosity, indicating that galaxy mass controls the pace and products of chemical enrichment. The same data show aluminum-to-iron ratios near minus 0.5, matching metal-poor Milky Way stars, and reveal nitrogen-rich field stars in Fornax whose metallicities differ from the galaxy's known globular clusters.

Core claim

The distribution of alpha elements strongly correlates with galaxy luminosity and hence mass, underscoring the critical role of galaxy mass in shaping chemical evolution. These dwarf galaxies exhibit [Al/Fe] approximately minus 0.5, comparable to metal-poor stars in the Milky Way. Nitrogen-rich field stars identified in Fornax display distinct metallicities from its known globular clusters and may represent relics of destroyed clusters.

What carries the argument

APOGEE-derived [Si/Fe] and other alpha-element abundance ratios plotted against galaxy luminosity, which directly traces the mass-dependent chemical evolution pathway.

If this is right

  • Higher-luminosity dwarfs experienced more rapid or efficient alpha-element production than their fainter counterparts.
  • Shallow gravitational potentials in low-mass dwarfs allowed greater loss of metals and altered the balance of core-collapse versus Type Ia supernovae contributions.
  • Nitrogen-rich stars in Fornax provide direct evidence that globular-cluster disruption has contributed field stars to the dwarf's present population.
  • Similar abundance patterns can be used to chemically tag stars in the Milky Way halo that originated in now-disrupted satellites.

Where Pith is reading between the lines

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

  • The observed mass-abundance relation offers a way to estimate the masses of fully disrupted progenitor galaxies whose stars now reside in stellar streams.
  • Extending the same abundance analysis to additional satellites would test whether the correlation holds across the full range of dwarf galaxy luminosities.
  • The similarity in [Al/Fe] between dwarfs and the Milky Way hints that early aluminum production occurred under comparable conditions before the galaxies assembled.

Load-bearing premise

The 74 observed stars are representative of each galaxy's overall stellar population and APOGEE abundance measurements carry no large systematic offsets in these very metal-poor systems.

What would settle it

A larger sample of stars in the same four galaxies showing no trend between [Si/Fe] and galaxy luminosity would remove support for the claimed mass dependence.

Figures

Figures reproduced from arXiv: 2511.06820 by Baitian Tang, Cheng Xu, Doug Geisler, Jos\'e G. Fern\'andez-Trincado, Yi Qiao, Zhiqiang Yan.

Figure 1
Figure 1. Figure 1: Target information. (a): Spatial distribution of target stars in Fnx dwarf galaxy. The black ellipse indicates the tidal radius of Fnx and its center is labelled with black cross. Target stars from R20 and this work are marked as blue triangles and red dots, respectively. The N-rich stars are further marked with red circles. The black stars represent GC Fnx 1-5 while the purple star represents GC Fnx 6. (b… view at source ↗
Figure 2
Figure 2. Figure 2: [α/Fe] vs. [Fe/H]. Fnx, Dra, Car and Sex stars from this work are labeled as red, cyan, blue and green stars respectively. The error bar in each panel indicates the median uncertainty of available measurements. Black dots correspond to MW stars from the halo (Fulbright 2000; Cayrel et al. 2004; Barklem et al. 2005; Yong et al. 2013; Roederer et al. 2014), and MW stars from the disc (Reddy et al. 2003, 2006… view at source ↗
Figure 3
Figure 3. Figure 3: [Al/Fe] vs. [Fe/H] relations. Symbols are the same as in [PITH_FULL_IMAGE:figures/full_fig_p011_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Derived LTE abundances of [Si/Fe] over metallicities for indi￾vidual dwarf galaxies. MW stars (black dots) are described in [PITH_FULL_IMAGE:figures/full_fig_p012_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Abundances of iron peak elements vs. [Fe/H]. Symbols are the same as in [PITH_FULL_IMAGE:figures/full_fig_p012_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Comparison of stellar parameters and chemical abundances of this work with those from the R20. Our results are denoted “our” and shown in the x-axis. The black solid line is the 1:1 relation. 2.5 2.0 1.5 1.0 0.5 0.0 [Fe/H] 0.4 0.2 0.0 0.2 0.4 0.6 0.8 1.0 1.2 [Ce/Fe] MW Carina Fornax Draco Sextans [PITH_FULL_IMAGE:figures/full_fig_p013_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: [Ce/Fe] vs. [Fe/H]. Symbols are the same as in [PITH_FULL_IMAGE:figures/full_fig_p013_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Metallicity distribution of stars in Fnx. Left panel: [Fe/H] as a function of elliptical radius in degrees. The green dashed line represents the best least-squared fit. They are divided into a metal-rich population ([Fe/H] > −1, blue dots) and a metal-poor population ([Fe/H] < −1, red dots). Right panel: the radial distribution of the metal-rich population (blue histogram) and the metal-poor population (re… view at source ↗
Figure 9
Figure 9. Figure 9: Abundance comparison between our identified N-rich stars [PITH_FULL_IMAGE:figures/full_fig_p015_9.png] view at source ↗
read the original abstract

During its evolution, the Milky Way (MW) incorporated numerous dwarf galaxies, particularly low-mass systems. The surviving dwarf galaxies orbiting the MW serve as exceptional laboratories for studying the unique properties of these systems. Their metal-poor environments and shallow gravitational potentials likely drive significant differences in star formation and star cluster properties compared to those in the MW. Using high-quality near-infrared spectra from the APOGEE survey, we determined abundances of Fe, C, N, O, Mg, Al, Si, Ca, Ti, Cr, Mn, Ni, and Ce for 74 stars in four MW satellite dwarf galaxies: Fornax, Sextans, Draco, and Carina. Our analysis reveals that the distribution of $\alpha$ elements (e.g., [Si/Fe]) strongly correlates with galaxy luminosity (and hence mass), underscoring the critical role of galaxy mass in shaping chemical evolution. These dwarf galaxies exhibit [Al/Fe$]\sim -0.5$, which is comparable to those of the metal-poor stars in the MW. Additionally, we identified nitrogen-rich field stars in the Fornax dwarf galaxy, which display distinct metallicities compared to its known globular clusters (GCs). If these stars originated in GCs and subsequently escaped, their presence suggests we are observing relics of destroyed GCs, offering possible evidence of cluster disruption.

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.

Referee Report

2 major / 1 minor

Summary. The manuscript analyzes high-quality APOGEE near-infrared spectra to derive abundances of Fe, C, N, O, Mg, Al, Si, Ca, Ti, Cr, Mn, Ni, and Ce for a total of 74 stars in four Milky Way satellite dwarf galaxies: Fornax, Sextans, Draco, and Carina. The central result is a reported strong correlation between α-element distributions (exemplified by [Si/Fe]) and galaxy luminosity/mass, with additional notes that [Al/Fe] ≈ −0.5 matches Milky Way metal-poor stars and that nitrogen-rich field stars in Fornax may represent relics of disrupted globular clusters.

Significance. If the α-element versus luminosity correlation is shown to be robust, the work would supply useful observational constraints on how galaxy mass influences chemical evolution in low-mass systems and on the role of dwarf satellites in Milky Way assembly. The identification of candidate globular-cluster escapees in Fornax would also contribute to understanding cluster disruption. The use of APOGEE spectra for these faint, metal-poor targets is a methodological strength, but the small total sample limits the strength of the conclusions.

major comments (2)
  1. [Abstract] Abstract: the claim that α-element distributions (e.g. [Si/Fe]) 'strongly correlate' with galaxy luminosity is presented without per-galaxy star counts, a correlation coefficient or p-value, or any test of robustness (e.g., removal of the most metal-poor stars or the dominant galaxy). With only 74 stars total, even modest imbalances or a few outliers can generate an apparent trend, directly undermining the load-bearing conclusion that galaxy mass shapes chemical evolution.
  2. [Methods / Results] Sample selection and error analysis (likely §2–3): the manuscript does not provide explicit criteria for choosing the 74 stars, an error budget that accounts for possible systematic offsets in APOGEE abundances at [Fe/H] ≲ −2 in low-mass systems, or direct comparisons to literature values for the same galaxies. These omissions leave the representativeness of the sample and the accuracy of the reported trends unverified.
minor comments (1)
  1. [Abstract] Abstract: the notation '[Al/Fe$]' contains a stray dollar sign and should be rendered consistently as [Al/Fe].

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their careful reading and constructive feedback on our manuscript. We agree that additional quantitative details and methodological transparency will strengthen the presentation of our results. Below we respond to each major comment and indicate the revisions we will make.

read point-by-point responses

  1. Referee: [Abstract] Abstract: the claim that α-element distributions (e.g. [Si/Fe]) 'strongly correlate' with galaxy luminosity is presented without per-galaxy star counts, a correlation coefficient or p-value, or any test of robustness (e.g., removal of the most metal-poor stars or the dominant galaxy). With only 74 stars total, even modest imbalances or a few outliers can generate an apparent trend, directly undermining the load-bearing conclusion that galaxy mass shapes chemical evolution.

    Authors: We accept that the abstract would be improved by explicit quantification. In the revised manuscript we will report the number of stars per galaxy, compute and quote the Spearman rank correlation coefficient together with its p-value for the [Si/Fe]–luminosity relation, and add a short robustness check that excludes both the most metal-poor stars and the dominant galaxy (Fornax). These additions will be placed in the abstract and expanded in the results section while preserving the original scientific interpretation. revision: yes

  2. Referee: [Methods / Results] Sample selection and error analysis (likely §2–3): the manuscript does not provide explicit criteria for choosing the 74 stars, an error budget that accounts for possible systematic offsets in APOGEE abundances at [Fe/H] ≲ −2 in low-mass systems, or direct comparisons to literature values for the same galaxies. These omissions leave the representativeness of the sample and the accuracy of the reported trends unverified.

    Authors: We agree that these details should be stated more explicitly. We will expand Section 2 to list the precise selection criteria (APOGEE quality flags, minimum S/N, radial-velocity membership cuts, and spatial/kinematic criteria). In Section 3 we will add a dedicated paragraph on possible systematic offsets in APOGEE abundances at [Fe/H] ≲ −2, referencing existing APOGEE validation studies, and we will insert direct abundance comparisons with published optical studies of the same four galaxies to demonstrate consistency of the reported trends. revision: yes

Circularity Check

0 steps flagged

No circularity: purely observational abundance study with no derivations or self-referential reductions

full rationale

The paper presents direct APOGEE spectroscopic abundance measurements (Fe, C, N, O, Mg, Al, Si, Ca, Ti, Cr, Mn, Ni, Ce) for 74 stars in Fornax, Sextans, Draco, and Carina, followed by empirical comparisons of alpha-element distributions (e.g., [Si/Fe]) against galaxy luminosity. No equations, model derivations, fitted parameters renamed as predictions, or uniqueness theorems appear in the provided text. The central claim is an observed correlation from the data itself, not a quantity forced by the paper's own inputs or self-citations. This matches the default expectation for an observational measurement paper and receives the lowest circularity score.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

Observational abundance study; no free parameters, axioms, or invented entities are introduced beyond standard spectroscopic analysis assumptions drawn from prior APOGEE literature.

pith-pipeline@v0.9.0 · 5568 in / 1186 out tokens · 45549 ms · 2026-05-18T00:14:47.275345+00:00 · methodology

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Lean theorems connected to this paper

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

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.

Reference graph

Works this paper leans on

118 extracted references · 118 canonical work pages

  1. [1]

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

    ENTRY address archiveprefix author booktitle chapter edition editor howpublished institution eprint journal key month note number organization pages publisher school series title type volume year label extra.label sort.label short.list INTEGERS output.state before.all mid.sentence after.sentence after.block FUNCTION init.state.consts #0 'before.all := #1 ...

    work page

  2. [2]

    write newline

    " write newline "" before.all 'output.state := FUNCTION n.dashify 't := "" t empty not t #1 #1 substring "-" = t #1 #2 substring "--" = not "--" * t #2 global.max substring 't := t #1 #1 substring "-" = "-" * t #2 global.max substring 't := while if t #1 #1 substring * t #2 global.max substring 't := if while FUNCTION word.in bbl.in " " * FUNCTION format....

    work page

  3. [3]

    2022, , 259, 35

    Abdurro'uf , Accetta , K., Aerts , C., et al. 2022, , 259, 35

    work page 2022

  4. [4]

    D., Vanzella , E., et al

    Adamo , A., Bradley , L. D., Vanzella , E., et al. 2024, , 632, 513

    work page 2024

  5. [5]

    C., Wilhelm , R., et al

    Allende Prieto , C., Beers , T. C., Wilhelm , R., et al. 2006, , 636, 804

    work page 2006

  6. [6]

    1999, , 140, 261

    Alonso , A., Arribas , S., & Mart \' nez-Roger , C. 1999, , 140, 261

    work page 1999

  7. [7]

    & Plez , B

    Alvarez , R. & Plez , B. 1998, , 330, 1109

    work page 1998

  8. [8]

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

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

    work page 2020

  9. [9]

    Amorisco , N. C. & Evans , N. W. 2012, , 756, L2

    work page 2012

  10. [10]

    Arnett , W. D. 1971, , 166, 153

    work page 1971

  11. [11]

    1999, , 347, 572

    Arnould , M., Goriely , S., & Jorissen , A. 1999, , 347, 572

    work page 1999

  12. [12]

    Asplund , M., Grevesse , N., & Sauval , A. J. 2005, in Astronomical Society of the Pacific Conference Series, Vol. 336, Cosmic Abundances as Records of Stellar Evolution and Nucleosynthesis, ed. I. Barnes , Thomas G. & F. N. Bash , 25

    work page 2005

  13. [13]

    S., Christlieb , N., Beers , T

    Barklem , P. S., Christlieb , N., Beers , T. C., et al. 2005, , 439, 129

    work page 2005

  14. [14]

    & Lardo , C

    Bastian , N. & Lardo , C. 2018, , 56, 83

    work page 2018

  15. [15]

    2006, , 459, 423

    Battaglia , G., Tolstoy , E., Helmi , A., et al. 2006, , 459, 423

    work page 2006

  16. [16]

    L., Oelkers , R

    Beaton , R. L., Oelkers , R. J., Hayes , C. R., et al. 2021, , 162, 302

    work page 2021

  17. [17]

    F., McIntosh , D

    Bell , E. F., McIntosh , D. H., Katz , N., & Weinberg , M. D. 2003, , 149, 289

    work page 2003

  18. [18]

    W., Koposov , S

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

    work page 2018

  19. [19]

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

    work page 2014

  20. [20]

    2014, , 787, 10

    Bisterzo , S., Travaglio , C., Gallino , R., Wiescher , M., & K \"a ppeler , F. 2014, , 787, 10

    work page 2014

  21. [21]

    R., Bershady , M

    Blanton , M. R., Bershady , M. A., Abolfathi , B., et al. 2017, , 154, 28

    work page 2017

  22. [22]

    Bowen , I. S. & Vaughan , A. H., J. 1973, , 12, 1430

    work page 1973

  23. [23]

    L., Travaglio , C., & Smith , V

    Busso , M., Gallino , R., Lambert , D. L., Travaglio , C., & Smith , V. V. 2001, , 557, 802

    work page 2001

  24. [24]

    L., Sheffield , A

    Carlin , J. L., Sheffield , A. A., Cunha , K., & Smith , V. V. 2018, , 859, L10

    work page 2018

  25. [25]

    G., et al

    Carretta , E., Bragaglia , A., Gratton , R. G., et al. 2010, , 516, A55

    work page 2010

  26. [26]

    2004, , 416, 1117

    Cayrel , R., Depagne , E., Spite , M., et al. 2004, , 416, 1117

    work page 2004

  27. [27]

    & Gnedin , O

    Chen , Y. & Gnedin , O. Y. 2023, , 522, 5638

    work page 2023

  28. [28]

    L., Belczynski , K., et al

    C \^o t \'e , B., Fryer , C. L., Belczynski , K., et al. 2018, , 855, 99

    work page 2018

  29. [29]

    de los Reyes , M. A. C., Kirby , E. N., Ji , A. P., & Nu \ n ez , E. H. 2022, , 925, 66

    work page 2022

  30. [30]

    J., Weinberg , D

    Eisenstein , D. J., Weinberg , D. H., Agol , E., et al. 2011, , 142, 72

    work page 2011

  31. [31]

    & Feuillet , D

    Feltzing , S. & Feuillet , D. 2023, , 953, 143

    work page 2023

  32. [32]

    G., Beers , T

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

    work page 2022

  33. [33]

    G., Beers , T

    Fern \'a ndez-Trincado , J. G., Beers , T. C., Minniti , D., et al. 2020, , 903, L17

    work page 2020

  34. [34]

    G., Beers , T

    Fern \'a ndez-Trincado , J. G., Beers , T. C., Minniti , D., et al. 2021, , 648, A70

    work page 2021

  35. [35]

    G., Beers , T

    Fern \'a ndez-Trincado , J. G., Beers , T. C., Tang , B., et al. 2019, , 488, 2864

    work page 2019

  36. [36]

    G., Robin , A

    Fern \'a ndez-Trincado , J. G., Robin , A. C., Moreno , E., et al. 2016, , 833, 132

    work page 2016

  37. [37]

    G., Zamora , O., Garc \' a-Hern \'a ndez , D

    Fern \'a ndez-Trincado , J. G., Zamora , O., Garc \' a-Hern \'a ndez , D. A., et al. 2017, , 846, L2

    work page 2017

  38. [38]

    A., Alabi , A., Romanowsky , A

    Forbes , D. A., Alabi , A., Romanowsky , A. J., Brodie , J. P., & Arimoto , N. 2020, , 492, 4874

    work page 2020

  39. [39]

    M., Gunawardhana , M., et al

    Foster , C., Hopkins , A. M., Gunawardhana , M., et al. 2012, , 547, A79

    work page 2012

  40. [40]

    Fulbright , J. P. 2000, , 120, 1841

    work page 2000

  41. [41]

    2018, , 616, A12

    Gaia Collaboration , Helmi , A., van Leeuwen , F., et al. 2018, , 616, A12

    work page 2018

  42. [42]

    Gonz \'a lez Hern \'a ndez , J. I. & Bonifacio , P. 2009, , 497, 497

    work page 2009

  43. [43]

    K., Gallagher , III, J

    Grebel , E. K., Gallagher , III, J. S., & Harbeck , D. 2003, , 125, 1926

    work page 2003

  44. [44]

    2008, , 486, 951

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

    work page 2008

  45. [45]

    R., Lian , J., et al

    Hasselquist , S., Hayes , C. R., Lian , J., et al. 2021, , 923, 172

    work page 2021

  46. [46]

    2017, , 845, 162

    Hasselquist , S., Shetrone , M., Smith , V., et al. 2017, , 845, 162

    work page 2017

  47. [47]

    H., et al

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

    work page 2018

  48. [48]

    1989, , 27, 139

    Hodge , P. 1989, , 27, 139

    work page 1989

  49. [49]

    Hodge , P. W. 1971, , 9, 35

    work page 1971

  50. [50]

    P., Mackereth , J

    Horta , D., Schiavon , R. P., Mackereth , J. T., et al. 2021, , 500, 1385

    work page 2021

  51. [51]

    & Koposov , S

    Huang , K.-W. & Koposov , S. E. 2021, , 500, 986

    work page 2021

  52. [52]

    2024, Science China Physics, Mechanics, and Astronomy, 67, 259513

    Huang , R., Tang , B., Li , C., et al. 2024, Science China Physics, Mechanics, and Astronomy, 67, 259513

    work page 2024

  53. [53]

    F., Martin , N

    Ibata , R., Lewis , G. F., Martin , N. F., Bellazzini , M., & Correnti , M. 2013, , 765, L15

    work page 2013

  54. [54]

    Karakas , A. I. & Lattanzio , J. C. 2014, , 31, e030

    work page 2014

  55. [55]

    N., Gilbert , K

    Kirby , E. N., Gilbert , K. M., Escala , I., et al. 2020, , 159, 46

    work page 2020

  56. [56]

    I., & Lugaro , M

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

    work page 2020

  57. [57]

    2006, , 653, 1145

    Kobayashi , C., Umeda , H., Nomoto , K., Tominaga , N., & Ohkubo , T. 2006, , 653, 1145

    work page 2006

  58. [58]

    & okas , E

    Kowalczyk , K. & okas , E. L. 2022, , 659, A119

    work page 2022

  59. [59]

    2012, , 543, A108

    Lagarde , N., Decressin , T., Charbonnel , C., et al. 2012, , 543, A108

    work page 2012

  60. [60]

    S., Eitner , P., Magg , E., et al

    Larsen , S. S., Eitner , P., Magg , E., et al. 2022, , 660, A88

    work page 2022

  61. [61]

    Law , D. R. & Majewski , S. R. 2010, , 718, 1128

    work page 2010

  62. [62]

    F., Serrano , A., & Torres-Peimbert , S

    Lequeux , J., Peimbert , M., Rayo , J. F., Serrano , A., & Torres-Peimbert , S. 1979, , 80, 155

    work page 1979

  63. [63]

    2006, , 453, 547

    Letarte , B., Hill , V., Jablonka , P., et al. 2006, , 453, 547

    work page 2006

  64. [64]

    P., et al

    Li , C., Tang , B., Milone , A. P., et al. 2021, , 906, 133

    work page 2021

  65. [65]

    & Gnedin , O

    Li , H. & Gnedin , O. Y. 2019, , 486, 4030

    work page 2019

  66. [66]

    & Chieffi , A

    Limongi , M. & Chieffi , A. 2006, , 647, 483

    work page 2006

  67. [67]

    E., Battistini , C., et al

    Lind , K., Koposov , S. E., Battistini , C., et al. 2015, , 575, L12

    work page 2015

  68. [68]

    2017, , 603, A2

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

    work page 2017

  69. [69]

    R., Schiavon , R

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

    work page 2017

  70. [70]

    R., Skrutskie , M

    Majewski , S. R., Skrutskie , M. F., Weinberg , M. D., & Ostheimer , J. C. 2003, , 599, 1082

    work page 2003

  71. [71]

    L., Shetrone , M

    Martell , S. L., Shetrone , M. D., Lucatello , S., et al. 2016, , 825, 146

    work page 2016

  72. [72]

    H., & Helmi , A

    Massari , D., Koppelman , H. H., & Helmi , A. 2019, , 630, L4

    work page 2019

  73. [73]

    2016, BACCHUS: Brussels Automatic Code for Characterizing High accUracy Spectra , Astrophysics Source Code Library, record ascl:1605.004

    Masseron , T., Merle , T., & Hawkins , K. 2016, BACCHUS: Brussels Automatic Code for Characterizing High accUracy Spectra , Astrophysics Source Code Library, record ascl:1605.004

    work page 2016

  74. [74]

    A., et al

    Masseron , T., Osorio , Y., Garc \' a-Hern \'a ndez , D. A., et al. 2021, , 647, A24

    work page 2021

  75. [75]

    McConnachie , A. W. 2012, , 144, 4

    work page 2012

  76. [76]

    2013, , 778, 149

    McWilliam , A., Wallerstein , G., & Mottini , M. 2013, , 778, 149

    work page 2013

  77. [77]

    L., Shetrone , M., et al

    M \'e sz \'a ros , S., Martell , S. L., Shetrone , M., et al. 2015, , 149, 153

    work page 2015

  78. [78]

    P., Marino , A

    Milone , A. P., Marino , A. F., Piotto , G., et al. 2015, , 808, 51

    work page 2015

  79. [79]

    R., C \^o t \'e , P., Santana , F

    Mu \ n oz , R. R., C \^o t \'e , P., Santana , F. A., et al. 2018, , 860, 66

    work page 2018

  80. [80]

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

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

    work page 2019

Showing first 80 references.