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REVIEW 2 major objections 1 minor 64 references

Mild radial gas flows of 1.5 km/s let a chemical evolution model match the Milky Way disc's [O/Fe]-[Fe/H] distribution, stellar density profile, and abundance gradients at once.

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2026-07-01 05:05 UTC pith:2U7UJXKH

load-bearing objection The Lagrangian method of characteristics is a clean technical step for radial flows, but the simultaneous fits rest on the two-infall accretion history. the 2 major comments →

arxiv 2606.31161 v1 pith:2U7UJXKH submitted 2026-06-30 astro-ph.GA

Chemical evolution of the Milky Way disc with radial gas flows: a Lagrangian approach

Fiorenzo Vincenzo This is my paper
classification astro-ph.GA
keywords chemical evolutionMilky Way discradial gas flowsLagrangian approachabundance gradientstwo-infall scenarioalpha-elementsType Ia supernovae
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

The paper builds a semi-analytic chemical evolution model that follows gas parcels inward under radial flows using the method of characteristics. Gas at any radius carries the enrichment history from every radius it crossed, so the stellar mass formed along each trajectory is lower than the local in-situ value. With mild inflows at 1.5 km/s the same model simultaneously fits the observed abundance plane, the present-day stellar surface density, the [Fe/H] and [O/H] gradients, and improves the age-abundance relations. The [O/Fe] ratio is the quantity most sensitive to the flows because the stellar mass per Type Ia supernova changes by up to 50 percent along the path.

Core claim

When radial gas flows are present, the chemical abundances of the gas at a given radius result from its whole inward journey in the disc, reflecting the star formation and accretion experienced at every radius it crossed; models with mild flows of v = 1.5 km/s reproduce simultaneously the observed [O/Fe]-[Fe/H] distribution across the disc, the present-day stellar surface-density profile, and the [Fe/H] and [O/H] gradients.

What carries the argument

The Lagrangian method of characteristics that reduces the gas surface density and abundance equations to one-dimensional integrals while accounting for radial flows and enrichment from core-collapse and Type Ia supernovae.

Load-bearing premise

The two-infall scenario for gas accretion history is assumed to hold for the Milky Way disc.

What would settle it

A direct measurement of the radial dependence of the stellar mass formed per Type Ia supernova, or of the [O/Fe] offset at fixed [Fe/H] that contradicts the 50 percent departure predicted along trajectories at 1.5 km/s, would falsify the claim.

Watch this falsifier — get emailed when new claim-graph text bears on it.

If this is right

  • The integrated stellar mass along each characteristic drops by up to an order of magnitude at v = 1.5 km/s compared with the local value.
  • The [O/Fe] ratio departs from its in-situ value by up to 50 percent, making alpha-enhancement the strongest signature of the flows.
  • Even mild inflows require that the full gas trajectory be tracked to recover the correct enrichment history.
  • The same flow speed that fits abundances also improves the match to the observed age-abundance relations.

Where Pith is reading between the lines

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

  • The same characteristic-tracking method could be applied to external disc galaxies that show flat or inverted abundance gradients.
  • Stronger flows would demand compensatory changes in the accretion timeline or star-formation efficiency to keep the same observables in agreement.
  • Comparing the model's predicted radial variation in [O/Fe] at fixed [Fe/H] against large spectroscopic surveys would test whether the 50 percent offset is observed.
  • The public code allows direct substitution of different supernova yield tables to check how sensitive the flow signature remains.

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 develops a semi-analytic Lagrangian model for Milky Way disc chemical evolution that incorporates radial gas flows via the method of characteristics, reducing the PDEs for gas surface density and abundances of alpha-elements and iron to one-dimensional integrals. Assuming a two-infall gas accretion history, the authors report that a constant radial flow speed of v = 1.5 km/s simultaneously reproduces the observed [O/Fe]-[Fe/H] distribution across the disc, the present-day stellar surface-density profile, the [Fe/H] and [O/H] gradients, and improves agreement with age-abundance relations. The integrated stellar mass along each characteristic is reduced relative to the local value, and the stellar mass formed per Type Ia supernova (which sets [O/Fe]) departs from its in-situ value by up to ~50%. The code is made publicly available.

Significance. If the two-infall assumption holds and the simultaneous reproduction is quantitatively verified, the work demonstrates that even mild radial flows leave a strong signature on alpha-enhancement by integrating enrichment along gas trajectories rather than at fixed radius. The reduction to one-dimensional integrals and the public code are clear strengths that support reproducibility. This approach could be adopted in other galactic chemical evolution studies to efficiently include radial mixing effects.

major comments (2)
  1. [Abstract] Abstract: The headline claim that v = 1.5 km/s simultaneously reproduces the [O/Fe]-[Fe/H] distribution, stellar surface-density profile, [Fe/H] and [O/H] gradients, and age-abundance relations is load-bearing on the two-infall accretion history, which is adopted without any alternative histories or sensitivity tests. Because abundances are obtained from integrals along characteristics whose source terms are set by the accretion rate at every radius crossed, a qualitatively different infall timeline would change those integrals and could invalidate the simultaneous reproduction.
  2. [Abstract] Abstract: No quantitative fit metrics, residual statistics, or comparison tables are presented for any of the claimed reproductions (e.g., no R² values, chi-squared, or explicit data-model overlays for the gradients or [O/Fe]-[Fe/H] plane). Without these, the strength of the evidence for the central claim cannot be assessed beyond the qualitative statement in the abstract.
minor comments (1)
  1. The manuscript would benefit from a dedicated section or table listing all model parameters, their adopted values, and which are fixed versus tuned.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the constructive comments. We address each major comment below.

read point-by-point responses

  1. Referee: [Abstract] Abstract: The headline claim that v = 1.5 km/s simultaneously reproduces the [O/Fe]-[Fe/H] distribution, stellar surface-density profile, [Fe/H] and [O/H] gradients, and age-abundance relations is load-bearing on the two-infall accretion history, which is adopted without any alternative histories or sensitivity tests. Because abundances are obtained from integrals along characteristics whose source terms are set by the accretion rate at every radius crossed, a qualitatively different infall timeline would change those integrals and could invalidate the simultaneous reproduction.

    Authors: We agree that the results depend on the adopted two-infall accretion history. While this framework is standard in Milky Way chemical evolution studies, we will add a sensitivity analysis to variations in the infall parameters in the revised manuscript to illustrate how different timelines affect the integrals along characteristics. revision: yes

  2. Referee: [Abstract] Abstract: No quantitative fit metrics, residual statistics, or comparison tables are presented for any of the claimed reproductions (e.g., no R² values, chi-squared, or explicit data-model overlays for the gradients or [O/Fe]-[Fe/H] plane). Without these, the strength of the evidence for the central claim cannot be assessed beyond the qualitative statement in the abstract.

    Authors: We agree that quantitative metrics would strengthen the evidence presented. In the revised manuscript we will add chi-squared values, residual statistics, and comparison tables quantifying the agreement with data for the [O/Fe]-[Fe/H] distribution, stellar surface-density profile, and abundance gradients. revision: yes

Circularity Check

0 steps flagged

No circularity: Lagrangian integrals are independent math; two-infall is explicit assumption and v is tuned to external data

full rationale

The derivation reduces abundances to explicit one-dimensional integrals along characteristics whose source terms are the two-infall accretion history (an external premise stated in the abstract and methods). The value v = 1.5 km/s is introduced as a free parameter whose effect is then compared to observed [O/Fe]-[Fe/H] distributions, gradients, and surface-density profiles; the match is therefore a fit to independent benchmarks rather than a quantity defined from those same benchmarks. No self-citation is invoked as a uniqueness theorem, no ansatz is smuggled, and no fitted quantity is relabeled a first-principles prediction. The model is therefore self-contained against external data.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

The model rests on the two-infall accretion history and a chosen radial flow speed; no new particles or forces are introduced.

free parameters (1)
  • radial gas flow velocity v = 1.5 km/s
    Chosen at 1.5 km/s to reproduce multiple Milky Way observables simultaneously
axioms (1)
  • domain assumption Two-infall scenario accurately describes the gas accretion history of the Milky Way disc
    Invoked to set the boundary conditions for the Lagrangian characteristics

pith-pipeline@v0.9.1-grok · 5875 in / 1272 out tokens · 31048 ms · 2026-07-01T05:05:31.221047+00:00 · methodology

0 comments
read the original abstract

Chemical abundance patterns result from the interplay between gas accretion, star formation, and radial mixing of gas and stars. Disentangling these processes is crucial to recover the mechanisms shaping the formation and evolution of galaxies. We model the chemical evolution of the Galactic disc in the presence of radial gas flows, to assess their impact on the [O/Fe]-[Fe/H] abundance patterns and on the radial gradients of [Fe/H] and [O/H]. We develop fast, semi-analytic solutions for the gas surface mass density and the abundances of alpha-elements and iron, accounting for radial gas flows and chemical enrichment from core-collapse and Type Ia supernovae. The model follows a Lagrangian approach, using the method of characteristics, reducing the solutions to one-dimensional integrals. We apply our model to the Milky Way disc assuming a two-infall scenario. When radial gas flows are present, the chemical abundances of the gas at a given radius result from its whole inward journey in the disc, reflecting the star formation and accretion experienced at every radius it crossed. The integrated stellar mass along the characteristic is lower than the local value by up to an order of magnitude at v = 1.5 km/s. Models with mild flows of v = 1.5 km/s reproduce simultaneously the observed [O/Fe]-[Fe/H] distribution across the disc, the present-day stellar surface-density profile, and the [Fe/H] and [O/H] gradients, improving also the agreement with the observed age-abundance relations. The stellar mass formed per Type Ia supernova sets the [O/Fe] ratio and departs from its in-situ value by up to ~50 per cent, making the alpha-enhancement the quantity on which radial flows leave their strongest signature. Following the gas along its trajectory is essential to recover the correct enrichment history even for models with mild radial gas inflows. The code is made publicly available.

Figures

Figures reproduced from arXiv: 2606.31161 by Fiorenzo Vincenzo.

Figure 1
Figure 1. Figure 1: The [O/Fe]–[Fe/H] abundance plane in eight radial bins spanning 3.5 ≤ R/kpc < 11.5. The background colour map shows the stellar number density of APOGEE DR17 stars estimated via a 2D Gaussian kernel density estimator, with regions below 2% of the peak density shown in white. Stars are selected within |z| ≤ 0.5 kpc of the Galactic plane. The coloured tracks show the predictions of the chemical evolution mod… view at source ↗
Figure 2
Figure 2. Figure 2: Same as Fig [PITH_FULL_IMAGE:figures/full_fig_p009_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Chemical evolution tracks in the [O/Fe]–[Fe/H] plane of the gas residing at fixed Galactocentric radii R = 6, 8, 10 kpc (rows) for constant inflow velocities v = 0.5, 1.0, 1.5 km s−1 (columns). Each track is the Eulerian abundance history of the gas located at R, coloured by the radius ξ from which that gas originated, i.e. the Lagrangian label of the characteristic passing through R at each time (ξ = R + … view at source ↗
Figure 4
Figure 4. Figure 4: Left: present-day stellar surface-density profile [PITH_FULL_IMAGE:figures/full_fig_p011_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Age–abundance relations across the disc. Each column corresponds to a Galactocentric ring (labelled on top), and the three [PITH_FULL_IMAGE:figures/full_fig_p011_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Radial gradients of [Fe/H] (top row) and [O/H] (bottom row) for the OCCAM sample of open clusters (Myers et al. 2022), divided into the same four age bins used in their analysis (black stars with error bars; for [O/H] the uncertainty is propagated from [Fe/H] and [O/Fe]). In each panel the coloured lines show the predicted Eulerian gas-phase abundance profiles of models for constant inflow velocities v = 0… view at source ↗
Figure 7
Figure 7. Figure 7: Top row: the total stellar mass formed Mchar ⋆ , the total number of Type Ia SNe N char Ia , and the total accreted gas mass Mchar inf , integrated along the characteristic of the gas that reaches each radius R today (equations 26), as a function of R, for inflow velocities v = 0.5, 1.0, 1.5, 2.0 km s−1 (coloured solid lines) and for the in-situ case with v = 0 (dashed line). Bottom row: the present-day ga… view at source ↗
Figure 8
Figure 8. Figure 8: Ratio between the quantities integrated along the flow characteristic, [PITH_FULL_IMAGE:figures/full_fig_p013_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: Effect of radial gas flows on the ratios that drive the abundances, shown as the ratio between each driver evaluated along the flow characteristic and the same driver that would be measured locally at the same radius, as a function of Galactocentric radius R, for inflow velocities v = 0.5, 1.0, 1.5, 2.0 km s−1 . From left to right: M⋆/Minf, NIa/Minf, and M⋆/NIa. The dotted line marks unity, where the chara… view at source ↗

discussion (0)

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Works this paper leans on

64 extracted references · 64 canonical work pages

  1. [1]

    2022, ApJS, 259, 35

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

    work page 2022

  2. [2]

    J., & Scott, P

    Asplund, M., Grevesse, N., Sauval, A. J., & Scott, P. 2009, ARA&A, 47, 481

    work page 2009

  3. [3]

    F., McIntosh, D

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

    work page 2003

  4. [4]

    2019, The Messenger, 175, 35

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

    work page 2019

  5. [5]

    2003, A&A, 410, 527

    Bensby, T., Feltzing, S., & Lundström, I. 2003, A&A, 410, 527

    work page 2003

  6. [6]

    & Schönrich, R

    Bilitewski, T. & Schönrich, R. 2012, MNRAS, 426, 2266

    work page 2012

  7. [7]

    & Gerhard, O

    Bland-Hawthorn, J. & Gerhard, O. 2016, ARA&A, 54, 529

    work page 2016

  8. [8]

    R., Bershady, M

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

    work page 2017

  9. [9]

    2018, MNRAS, 478, 4513

    Buder, S., Asplund, M., Duong, L., et al. 2018, MNRAS, 478, 4513

    work page 2018

  10. [10]

    E., et al

    Buder, S., Kos, J., Wang, X. E., et al. 2025, PASA, 42, e051

    work page 2025

  11. [11]

    1997, ApJ, 477, 765

    Chiappini, C., Matteucci, F., & Gratton, R. 1997, ApJ, 477, 765

    work page 1997

  12. [12]

    2019, The Messenger, 175, 30

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

    work page 2019

  13. [13]

    2014, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, V ol

    Cirasuolo, M., Afonso, J., Carollo, M., et al. 2014, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, V ol. 9147, Ground- based and Airborne Instrumentation for Astronomy V , ed. S. K. Ramsay, I. S. McLean, & H. Takami, 91470N de Jong, R. S., Agertz, O., Berbel, A. A., et al. 2019, The Messenger, 175, 3

    work page 2014

  14. [14]

    Deason, A. J. & Belokurov, V . 2024, New A Rev., 99, 101706

    work page 2024

  15. [15]

    O., Johnson, J

    Dubay, L. O., Johnson, J. A., Johnson, J. W., & Roberts, J. D. 2026, ApJ, 1000, 244

    work page 2026

  16. [16]

    W., Lang, D., & Goodman, J

    Foreman-Mackey, D., Hogg, D. W., Lang, D., & Goodman, J. 2013, PASP, 125, 306

    work page 2013

  17. [17]

    & Bland-Hawthorn, J

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

    work page 2002

  18. [18]

    1998, A&A, 338, 161 Gaia Collaboration, Vallenari, A., Brown, A

    Fuhrmann, K. 1998, A&A, 338, 161 Gaia Collaboration, Vallenari, A., Brown, A. G. A., et al. 2023, A&A, 674, A1

    work page 1998

  19. [19]

    A., Mucciarelli, A., Origlia, L., et al

    Gonzalez, O. A., Mucciarelli, A., Origlia, L., et al. 2020, The Messenger, 180, 18

    work page 2020

  20. [20]

    & Weare, J

    Goodman, J. & Weare, J. 2010, Communications in Applied Mathematics and Computational Science, 5, 65

    work page 2010

  21. [21]

    R., Bland-Hawthorn, J., Sharma, S., et al

    Hayden, M. R., Bland-Hawthorn, J., Sharma, S., et al. 2020, MNRAS, 493, 2952

    work page 2020

  22. [22]

    R., Bovy, J., Holtzman, J

    Hayden, M. R., Bovy, J., Holtzman, J. A., et al. 2015, ApJ, 808, 132

    work page 2015

  23. [23]

    R., Recio-Blanco, A., de Laverny, P., et al

    Hayden, M. R., Recio-Blanco, A., de Laverny, P., et al. 2018, A&A, 609, A79

    work page 2018

  24. [24]

    1999, ApJS, 125, 439

    Iwamoto, K., Brachwitz, F., Nomoto, K., et al. 1999, ApJS, 125, 439

    work page 1999

  25. [25]

    C., Dalton, G

    Jin, S., Trager, S. C., Dalton, G. B., et al. 2024, MNRAS, 530, 2688

    work page 2024

  26. [26]

    Johnson, J. W. 2025, arXiv e-prints, arXiv:2510.05223

    work page arXiv 2025

  27. [27]

    W., Weinberg, D

    Johnson, J. W., Weinberg, D. H., Vincenzo, F., et al. 2021, MNRAS, 508, 4484

    work page 2021

  28. [28]

    Kennicutt, Jr., R. C. 1998, ApJ, 498, 541

    work page 1998

  29. [29]

    A., & Gilmore, G

    Kroupa, P., Tout, C. A., & Gilmore, G. 1993, MNRAS, 262, 545

    work page 1993

  30. [30]

    2015, A&A, 580, A126

    Kubryk, M., Prantzos, N., & Athanassoula, E. 2015, A&A, 580, A126

    work page 2015

  31. [31]

    Lacey, C. G. & Fall, S. M. 1985, ApJ, 290, 154

    work page 1985

  32. [32]

    Leung, H. W. & Bovy, J. 2019, MNRAS, 483, 3255

    work page 2019

  33. [33]

    Licquia, T. C. & Newman, J. A. 2015, ApJ, 806, 96

    work page 2015

  34. [34]

    2015, Research in Astronomy and As- trophysics, 15, 1095

    Luo, A.-L., Zhao, Y .-H., Zhao, G., et al. 2015, Research in Astronomy and As- trophysics, 15, 1095

    work page 2015

  35. [35]

    T., Bovy, J., Leung, H

    Mackereth, J. T., Bovy, J., Leung, H. W., et al. 2019, MNRAS, 489, 176

    work page 2019

  36. [36]

    R., Schiavon, R

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

    work page 2017

  37. [37]

    & Graur, O

    Maoz, D. & Graur, O. 2017, ApJ, 848, 25

    work page 2017

  38. [38]

    2014, ARA&A, 52, 107

    Maoz, D., Mannucci, F., & Nelemans, G. 2014, ARA&A, 52, 107

    work page 2014

  39. [39]

    & Francois, P

    Matteucci, F. & Francois, P. 1989, MNRAS, 239, 885

    work page 1989

  40. [40]

    & Greggio, L

    Matteucci, F. & Greggio, L. 1986, A&A, 154, 279 Mollá, M., Díaz, Á. I., Gibson, B. K., Cavichia, O., & López-Sánchez, Á.-R. 2016, MNRAS, 462, 1329

    work page 1986

  41. [41]

    2013, MNRAS, 435, 2918

    Mott, A., Spitoni, E., & Matteucci, F. 2013, MNRAS, 435, 2918

    work page 2013

  42. [42]

    2022, AJ, 164, 85

    Myers, N., Donor, J., Spoo, T., et al. 2022, AJ, 164, 85

    work page 2022

  43. [43]

    2020, MNRAS, 498, 1710

    Palla, M., Matteucci, F., Spitoni, E., Vincenzo, F., & Grisoni, V . 2020, MNRAS, 498, 1710

    work page 2020

  44. [44]

    & Fraternali, F

    Pezzulli, G. & Fraternali, F. 2016, MNRAS, 455, 2308

    work page 2016

  45. [45]

    & Chiosi, C

    Portinari, L. & Chiosi, C. 2000, A&A, 355, 929

    work page 2000

  46. [46]

    2022, A&A, 666, A121 Schönrich, R

    Randich, S., Gilmore, G., Magrini, L., et al. 2022, A&A, 666, A121 Schönrich, R. & Binney, J. 2009, MNRAS, 396, 203

    work page 2022

  47. [47]

    R., & Bland-Hawthorn, J

    Sharma, S., Hayden, M. R., & Bland-Hawthorn, J. 2021, MNRAS, 507, 5882

    work page 2021

  48. [48]

    2017, A&A, 605, A38

    Spitoni, E., Gioannini, L., & Matteucci, F. 2017, A&A, 605, A38

    work page 2017

  49. [49]

    & Matteucci, F

    Spitoni, E. & Matteucci, F. 2011, A&A, 531, A72

    work page 2011

  50. [50]

    Spitoni, E., Matteucci, F., & Marcon-Uchida, M. M. 2013, A&A, 551, A123

    work page 2013

  51. [51]

    2015, ApJ, 802, 129

    Spitoni, E., Romano, D., Matteucci, F., & Ciotti, L. 2015, ApJ, 802, 129

    work page 2015

  52. [52]

    2019, A&A, 623, A60

    Spitoni, E., Silva Aguirre, V ., Matteucci, F., Calura, F., & Grisoni, V . 2019, A&A, 623, A60

    work page 2019

  53. [53]

    2020, A&A, 635, A58

    Spitoni, E., Verma, K., Silva Aguirre, V ., & Calura, F. 2020, A&A, 635, A58

    work page 2020

  54. [54]

    2021, A&A, 647, A73

    Spitoni, E., Verma, K., Silva Aguirre, V ., et al. 2021, A&A, 647, A73

    work page 2021

  55. [55]

    & Price, K

    Storn, R. & Price, K. 1997, Journal of Global Optimization, 11, 341

    work page 1997

  56. [56]

    Tinsley, B. M. 1980, Fund. Cosmic Phys., 5, 287

    work page 1980

  57. [57]

    2016, MNRAS, 455, 4183

    Vincenzo, F., Matteucci, F., Belfiore, F., & Maiolino, R. 2016, MNRAS, 455, 4183

    work page 2016

  58. [58]

    2017, MNRAS, 466, 2939

    Vincenzo, F., Matteucci, F., & Spitoni, E. 2017, MNRAS, 466, 2939

    work page 2017

  59. [59]

    A., Weinberg, D

    Vincenzo, F., Thompson, T. A., Weinberg, D. H., et al. 2021, MNRAS, 508, 3499

    work page 2021

  60. [60]

    E., et al

    Virtanen, P., Gommers, R., Oliphant, T. E., et al. 2020, Nature Methods, 17, 261

    work page 2020

  61. [61]

    H., Griffith, E

    Weinberg, D. H., Griffith, E. J., Johnson, J. W., & Thompson, T. A. 2024, ApJ, 973, 122

    work page 2024

  62. [62]

    H., Holtzman, J

    Weinberg, D. H., Holtzman, J. A., Hasselquist, S., et al. 2019, ApJ, 874, 102

    work page 2019

  63. [63]

    H., Holtzman, J

    Weinberg, D. H., Holtzman, J. A., Johnson, J. A., et al. 2022, ApJS, 260, 32

    work page 2022

  64. [64]

    2019, ApJS, 245, 34 Article number, page 15

    Xiang, M., Ting, Y .-S., Rix, H.-W., et al. 2019, ApJS, 245, 34 Article number, page 15

    work page 2019