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Nebular dust attenuation of H-alpha is 0.20 dex higher on average than standard Balmer decrement estimates in z=1.5-4.4 galaxies.

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Nebular H-alpha attenuation is 0.20 dex higher than standard Balmer decrement plus Galactic curve methods, with nebular curves showing higher Rv than stellar curves due to porous dust from stellar feedback.

T0 review reviewed 2026-06-29 challenge →

load-bearing objection The paper reports that Hα attenuation is 0.2 dex higher than the standard Balmer-decrement plus Galactic curve when Paschen lines are included, but the 24-galaxy sample selected for multi-line detections leaves the result vulnerable to bias. the 1 major comments →

arxiv 2605.30427 v1 pith:HAQ5VPXI submitted 2026-05-28 astro-ph.GA

The AURORA Survey: Multiple Balmer and Paschen Emission Lines for Individual Star-forming Galaxies at z=1.5-4.4. II. Implications for Nebular Dust Corrections, Nebular SFRs, and Differential Reddening

Naveen A. Reddy , Alice E. Shapley , Ryan L. Sanders , Michael W. Topping , Max Pettini , Natascha M. Forster Schreiber , Charles C. Steidel , Leonardo Clarke
show 5 more authors
Richard S. Ellis Anthony J. Pahl Garth D. Illingworth Mariska Kriek Desika Narayanan
This is my paper
classification astro-ph.GA
keywords nebular dust attenuationBalmer decrementPaschen lineshigh-redshift galaxiesstar formation ratesdifferential reddeningemission linesdust curves
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 reading

The paper uses multiple detections of Balmer and Paschen emission lines in 24 galaxies from the AURORA survey to derive nebular dust attenuation curves directly. It shows that the total attenuation of H-alpha exceeds the values from the common combination of the Balmer decrement and the Galactic extinction curve by about 0.20 dex. Nebular star formation rates align with those from spectral energy distributions when MOSDEF or SMC curves are applied instead. The findings indicate that Paschen lines trace more reddened regions than Balmer lines or UV continuum, pointing to differences in how dust affects stellar and nebular light.

Core claim

The nebular dust attenuation curves derived from multiple HI Balmer and Paschen recombination lines in 24 galaxies at z=1.5-4.4 indicate that the total attenuation of H-alpha is ~0.20 dex larger on average than values from the Balmer decrement combined with the Galactic extinction curve. Nebular-line SFRs match SED-based SFRs when using the MOSDEF attenuation or SMC extinction curves. The nebular and stellar reddening relation is consistent with Paschen lines being sensitive to heavily reddened OB associations while Balmer lines and UV continuum include contributions from relatively unreddened ones. Nebular curves show high Rv or flatness in contrast to the low Rv or steepness of stellar cur

What carries the argument

Nebular dust attenuation curves derived from multiple Balmer and Paschen recombination line detections

Load-bearing premise

Detections of multiple Balmer and Paschen lines in the 24-galaxy sample permit direct derivation of attenuation curves without major biases from measurement errors, sample selection, or extra emission contributions.

What would settle it

Measurements in a larger sample of galaxies with multiple line detections that yield an average H-alpha attenuation difference significantly different from 0.20 dex or inconsistent nebular attenuation curves.

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

If this is right

  • Nebular SFRs derived from emission lines become consistent with SED-based SFRs when MOSDEF or SMC curves are used for the latter.
  • The reddening relation supports Paschen lines tracing heavily reddened OB associations while Balmer and UV trace less reddened regions.
  • Nebular attenuation curves are flatter with higher Rv than the steeper stellar curves, suggesting a porous dust medium from stellar feedback.
  • The youngest galaxy in the sample has identical stellar and nebular reddening curves, as expected when OB associations dominate the continuum at all wavelengths.

Where Pith is reading between the lines

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

  • This difference in attenuation may require revisions to how dust corrections are applied in high-redshift galaxy surveys using only Balmer lines.
  • The contrast between stellar and nebular curves could inform models of dust geometry and feedback effects in star-forming regions.
  • If confirmed in larger samples, the identical curves in young galaxies would constrain the timescale for dust and metals mixing around HII regions.
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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

1 major / 2 minor

Summary. The manuscript reports implications of nebular dust attenuation curves derived for 24 star-forming galaxies at z=1.5-4.4 with multiple Balmer and Paschen line detections from the JWST/AURORA survey. The central claim is that the total attenuation of Hα is on average ~0.20 dex larger than obtained from the Balmer decrement combined with the Galactic extinction curve. It further states that nebular-line and SED-based SFRs are consistent when using the MOSDEF attenuation or SMC extinction curves, that the nebular-stellar reddening relation is consistent with Paschen lines tracing heavily reddened OB associations while Balmer and UV trace less reddened ones, and that nebular curves have high R_V (flat) in contrast to low R_V (steep) stellar curves, possibly indicating a porous medium from feedback. For the youngest galaxy the two curves match.

Significance. If the central offset and differential-reddening interpretation hold, the results would meaningfully affect dust-correction practices and SFR estimates at high redshift and would support models in which feedback creates porosity on H II-region scales. The multi-line approach itself is a methodological strength that supplies more constraints than single-ratio methods.

major comments (1)
  1. [Abstract and sample description] Abstract and sample description: the central 0.20 dex Hα attenuation offset is derived from a 24-galaxy sample defined by the presence of multiple Balmer/Paschen detections. This selection necessarily excludes systems in which Paschen lines fall below the detection threshold (i.e., the most heavily obscured objects), which can bias the recovered attenuation-curve shape and normalization at Hα. Because the reported average offset is load-bearing for the paper’s main conclusion, an explicit test or quantification of this selection bias is required.
minor comments (2)
  1. [Abstract] Abstract: the stated average offset of ~0.20 dex is given without accompanying uncertainty, sample size contributing to the mean, or median value, reducing the reader’s ability to judge robustness.
  2. [Abstract] Abstract: reference to “the youngest galaxy in the sample” without identifying the object, its redshift, or its line properties leaves an important illustrative case underspecified.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their careful reading and constructive feedback. The single major comment raises an important point about sample selection, which we address directly below.

read point-by-point responses

  1. Referee: Abstract and sample description: the central 0.20 dex Hα attenuation offset is derived from a 24-galaxy sample defined by the presence of multiple Balmer/Paschen detections. This selection necessarily excludes systems in which Paschen lines fall below the detection threshold (i.e., the most heavily obscured objects), which can bias the recovered attenuation-curve shape and normalization at Hα. Because the reported average offset is load-bearing for the paper’s main conclusion, an explicit test or quantification of this selection bias is required.

    Authors: We agree that the requirement for multiple Balmer and Paschen detections introduces a selection bias against the most heavily obscured systems, where Paschen lines fall below the detection threshold. This is an inherent feature of the multi-line method used to constrain the attenuation curve shape. Our reported 0.20 dex offset and the derived curves therefore apply specifically to the subset of galaxies where these lines are measurable. In the revised manuscript we will add an explicit discussion of this selection effect in Section 2 (sample description), including: (1) a comparison of the Hα flux distribution and dust attenuation properties of the 24-galaxy subsample versus the full AURORA parent sample at similar redshifts, and (2) a simple estimate of the possible bias on the mean Hα attenuation by considering the Paschen detection limits and the expected attenuation for non-detections under different curve assumptions. We note that even with this caveat the offset remains statistically significant within the observed sample and carries implications for dust corrections in galaxies with comparable line detectability. revision: yes

Circularity Check

0 steps flagged

No significant circularity in derivation of nebular attenuation curves.

full rationale

The central derivation uses observed flux ratios among multiple Balmer and Paschen lines (new JWST/AURORA data for 24 galaxies) compared against standard case-B intrinsic ratios to obtain attenuation curves and A(Hα) values. This is a direct observational reduction independent of any fitted parameters from the target result itself or load-bearing self-citations. Mentions of MOSDEF or Galactic curves serve only as external benchmarks for comparison, not as inputs that define the new curves. No self-definitional, fitted-input-called-prediction, or uniqueness-imported steps appear in the provided derivation chain.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

The analysis depends on standard atomic physics for intrinsic line ratios and empirical dust curve models fitted to the new line detections; no new entities postulated.

free parameters (1)
  • nebular attenuation curve shape parameters
    Derived by fitting observed line ratios after subtracting intrinsic ratios from atomic data.
axioms (1)
  • standard math Intrinsic Balmer and Paschen line ratios are fixed by atomic physics and unaffected by local conditions.
    Invoked to convert observed ratios into attenuation values.

reviewed 2026-06-29 · how reviews work

0 comments
Cite this review

Pith. "Pith review of The AURORA Survey: Multiple Balmer and Paschen Emission Lines for Individual Star-forming Galaxies at z=1.5-4.4. II. Implications for Nebular Dust Corrections, Nebular SFRs, and Differential Reddening." pith.science (2026). https://pith.science/paper/HAQ5VPXI

@misc{pith2026260530427,
  author       = {Pith},
  title        = {Pith review of: The AURORA Survey: Multiple Balmer and Paschen Emission Lines for Individual Star-forming Galaxies at z=1.5-4.4. II. Implications for Nebular Dust Corrections, Nebular SFRs, and Differential Reddening},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/HAQ5VPXI}},
  note         = {Machine review of arXiv:2605.30427}
}
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read the original abstract

We discuss the implications of the nebular dust attenuation curves derived for 24 galaxies at z=1.5-4.4 with multiple detections of HI Balmer and Paschen recombination emission lines from the JWST/AURORA survey. The total attenuation of Ha is ~0.20 dex larger on average than the values obtained with the commonly adopted combination of the Balmer decrement and the Galactic extinction curve. Nebular-line SFRs and SED-based SFRs are consistent on average when using the MOSDEF attenuation or SMC extinction curves for the latter. The relation between nebular and stellar reddening is consistent with a scenario where the Paschen lines are sensitive to heavily reddened OB associations, while relatively unreddened OB associations contribute significantly to the Balmer line and UV continuum emission. There is a stark contrast between the low Rv (or steepness) of stellar dust attenuation curves and the high Rv (or flatness) of nebular dust attenuation curves. We suggest that the latter could be reflective of a more porous medium established by strong feedback from massive stars. For the youngest galaxy in the sample, the stellar reddening curve is identical to the nebular attenuation curve, in accordance with our expectation that OB associations dominate the stellar continuum emission at all wavelengths for this very young galaxy. Larger samples will be needed to determine whether this conclusion holds for young galaxies in general, and provide further insights into the dust and metals mixing timescale on the scale of HII regions.

Figures

Figures reproduced from arXiv: 2605.30427 by Alice E. Shapley, Anthony J. Pahl, Charles C. Steidel, Desika Narayanan, Garth D. Illingworth, Leonardo Clarke, Mariska Kriek, Max Pettini, Michael W. Topping, Natascha M. Forster Schreiber, Naveen A. Reddy, Richard S. Ellis, Ryan L. Sanders.

Figure 1
Figure 1. Figure 1: The average nebular attenuation curve, kneb(λ), versus λ0 for the main sample of 24 galaxies (thick red curve). The in￾dividual nebular dust attenuation curves are indicated by the light purple lines. The Galactic extinction curve (Cardelli et al. 1989) is shown by the solid blue line. and Spectral Synthesis (BPASS) version 2.2.1 models (El￾dridge et al. 2017; Stanway & Eldridge 2018) were used to fit the … view at source ↗
Figure 2
Figure 2. Figure 2: Top: Distribution of the attenuation curve slopes between Hβ and Hα, or k eff neb(Hβ)/keff neb(Hα), and the attenuation curve dif￾ferences between Hβ and Hα, or k eff neb(Hβ)−k eff neb(Hα). The points are color-coded by RV . Values for the average nebular dust atten￾uation curve are indicated by the open star. The large grey crosses indicate the difference and slope values for the Galactic extinction curve… view at source ↗
Figure 3
Figure 3. Figure 3: Comparison of E(B − V )neb and dust-corrected line luminosities (Hα and the longest-wavelength Paschen line available for each galaxy) and line ratios (O32, R23, and S32) assuming the average and individual nebular attenuation curves. The standard deviation between the quantities assuming the average and individual nebular attenuation curves and indicated in each panel. attenuation curve from Reddy et al. … view at source ↗
Figure 4
Figure 4. Figure 4: Comparison of SFRneb and SED-inferred SFR (SFR(SED)) derived using the Calzetti (left), SMC (middle), and Reddy et al. (2015) (MOSDEF, right) dust attenuation curves. The gold circles represent the 24 galaxies in the main sample, while the blue squares indicate galaxies excluded from the sample, but still with measured Balmer decrements. For the excluded galaxies, SFRneb was computed assuming the Balmer de… view at source ↗
Figure 6
Figure 6. Figure 6: (Left:) Same as [PITH_FULL_IMAGE:figures/full_fig_p010_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Relationship between SFR and M∗. The 24 galaxies in the main sample are indicated by the circles in each panel, where SFRneb was estimated using the Balmer decrement and Galactic extinction curve (left panel), the average nebular dust attenuation curve found in this study (middle panel), and the individual nebular dust attenuation curves for the 24 galaxies (right panel). Galaxies that were excluded from t… view at source ↗
Figure 8
Figure 8. Figure 8: Comparison of E(B − V )neb and E(B − V )cont. The top, middle, and bottom rows show the results for E(B − V )neb computed with only the Balmer lines and the Galactic extinction curve, only the Paschen lines and the Galactic extinction curve, and all H I recombination lines and the individually-determined nebu￾lar dust attenuation curves, respectively. The left and right columns show the results for E(B − V… view at source ↗
Figure 9
Figure 9. Figure 9: Comparison of the distribution of RV found for the neb￾ular attenuation curves of the 24 galaxies in AURORA (blue his￾togram) and the RV of commonly adopted extinction and attenua￾tion curves for the stellar continuum (red vertical lines). The SMC extinction curve has RV = 2.74 (Gordon et al. 2003), slightly less than that of the Milky Way (RV = 3.1; Cardelli et al. 1989). In￾creased ISM porosity towards m… view at source ↗
Figure 10
Figure 10. Figure 10: Comparison of k ′ neb(λ) (red curve) and k ′ cont(λ) (green curve) for GOODSN-17940 at z = 4.411. The 1σ uncertainty in the latter is indicated by the green shaded region. For clarity, the un￾certainty in k ′ neb(λ) is not shown. Individual k ′ neb(λ) points are de￾noted by the black symbols. Also shown are the Galactic, SMC, and Calzetti curves (solid, dotted, and dashed blue lines, respectively), shifte… view at source ↗
Figure 11
Figure 11. Figure 11: Comparison of dust-corrected line luminosities assuming the individual effective nebular attenuation curves (Leff ) and the Balmer decrement and the Galactic extinction curve (LBD) for the following lines: [O II]λλ3727, 3730, Hβ, [O III]λλ4960, 5008, Hα, [S II]λλ6718, 6733, and [S III]λλ9071, 9533. The line of equality is indicated in black. Each panel indicates the mean offset in luminos￾ity (log Leff − … view at source ↗
Figure 12
Figure 12. Figure 12: Comparison of dust-corrected line ratios of O32, R23, and S23, defined in Equations 4, 5, and 6, assuming the individual effective nebular attenuation curves (Line Ratioeff ) and the Balmer decrement and the Galactic extinction curve (Line RatioBD). The bottom two panels indicate the same for the auroral line ratios [O III]λ4364/[O III]λ5008 and [O II]λλ7320, 7330/[O II]λλ3727, 3730. The line of equality … view at source ↗
Figure 13
Figure 13. Figure 13: Correlations between SFRneb and E(B − V ) cov neb (left), fcov (middle), and fobsc(Hα)/f0(Hα) (right) derived from the covering￾fraction model [PITH_FULL_IMAGE:figures/full_fig_p024_13.png] view at source ↗

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Works this paper leans on

96 extracted references · 3 canonical work pages

  1. [1]

    2024, ApJ, 976, 224

    Alberts, S., Lyu, J., Shivaei, I., et al. 2024, ApJ, 976, 224

    2024

  2. [2]

    J., & Scott, P

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

    2009

  3. [3]

    J., Oesch, P., et al

    Atek, H., Furtak, L. J., Oesch, P., et al. 2022, MNRAS, 511, 4464

    2022

  4. [4]

    Blitz, L., & Shu, F. H. 1980, ApJ, 238, 148

    1980

  5. [5]

    2022, MNRAS, 510, 5088

    Avison, A. 2022, MNRAS, 510, 5088

    2022

  6. [6]

    Brinchmann, J., Charlot, S., White, S. D. M., et al. 2004, MNRAS, 351, 1151

    2004

  7. [7]

    2018, A&A, 619, A135

    Buat, V ., Boquien, M., Małek, K., et al. 2018, A&A, 619, A135

    2018

  8. [8]

    2012, A&A, 545, A141

    Buat, V ., Noll, S., Burgarella, D., et al. 2012, A&A, 545, A141

    2012

  9. [9]

    1997, AJ, 113, 162

    Calzetti, D. 1997, AJ, 113, 162

    1997

  10. [10]

    C., et al

    Calzetti, D., Armus, L., Bohlin, R. C., et al. 2000, ApJ, 533, 682

    2000

  11. [11]

    L., & Storchi-Bergmann, T

    Calzetti, D., Kinney, A. L., & Storchi-Bergmann, T. 1994, ApJ, 429, 582

    1994

  12. [12]

    A., Clayton, G

    Cardelli, J. A., Clayton, G. C., & Mathis, J. S. 1989, ApJ, 345, 245

    1989

  13. [13]

    2003, PASP, 115, 763

    Chabrier, G. 2003, PASP, 115, 763

    2003

  14. [14]

    E., et al

    Cheng, Y ., Giavalisco, M., Backhaus, B. E., et al. 2025, ApJ, 979, 71

    2025

  15. [15]

    Clarke, A

    Clarke, L., Shapley, A. E., Lam, N., et al. 2025, arXiv e-prints, arXiv:2510.06681

    work page arXiv 2025

  16. [16]

    E., Sanders, R

    Clarke, L., Shapley, A. E., Sanders, R. L., et al. 2024, ApJ, 977, 133

    2024

  17. [17]

    C., Gordon, K

    Clayton, G. C., Gordon, K. D., & Wolff, M. J. 2000, ApJS, 129, 147

    2000

  18. [18]

    J., Dunlop, J

    Cullen, F., McLure, R. J., Dunlop, J. S., et al. 2019, MNRAS, 487, 2038 —. 2020, MNRAS, 495, 1501 Dav´e, R. 2008, MNRAS, 385, 147 De Barros, S., Reddy, N., & Shivaei, I. 2016, ApJ, 820, 96 Dom´ınguez, A., Siana, B., Brooks, A. M., et al. 2015, MNRAS, 451, 839

    2019

  19. [19]

    J., Stanway, E

    Eldridge, J. J., Stanway, E. R., Xiao, L., et al. 2017, PASA, 34, e058

    2017

  20. [20]

    R., et al

    Emami, N., Siana, B., Weisz, D. R., et al. 2019, ApJ, 881, 71

    2019

  21. [21]

    N., O’Connell, R

    Fanelli, M. N., O’Connell, R. W., & Thuan, T. X. 1988, ApJ, 334, 665

    1988

  22. [22]

    2018, MNRAS, 473, 3717

    Faucher-Gigu`ere, C.-A. 2018, MNRAS, 473, 3717

    2018

  23. [23]

    J., Chatzikos, M., Guzm´an, F., et al

    Ferland, G. J., Chatzikos, M., Guzm´an, F., et al. 2017, RMxAA, 53, 385

    2017

  24. [24]

    A., Shapley, A

    Fetherolf, T., Reddy, N. A., Shapley, A. E., et al. 2020, MNRAS, 498, 5009 —. 2021, MNRAS, 508, 1431 —. 2023, MNRAS, 518, 4214

    2020

  25. [25]

    Fitzpatrick, E. L. 1999, PASP, 111, 63

    1999

  26. [26]

    L., & Massa, D

    Fitzpatrick, E. L., & Massa, D. 2009, ApJ, 699, 1209 F¨orster Schreiber, N. M., Genzel, R., Bouch´e, N., et al. 2009, ApJ, 706, 1364

    2009

  27. [27]

    A., Faisst, A., et al

    Fudamoto, Y ., Oesch, P. A., Faisst, A., et al. 2020, A&A, 643, A4 Gim´enez-Arteaga, C., Brammer, G. B., Marchesini, D., et al. 2022, ApJS, 263, 17

    2020

  28. [28]

    1999, MNRAS, 306, 843 20

    Glazebrook, K., Blake, C., Economou, F., Lilly, S., & Colless, M. 1999, MNRAS, 306, 843 20

    1999

  29. [29]

    Wolff, M. J. 2003, ApJ, 594, 279

    2003

  30. [30]

    M., van Hoof, P

    Gunasekera, C. M., van Hoof, P. A. M., Chatzikos, M., & Ferland, G. J. 2023, Research Notes of the American Astronomical Society, 7, 246

    2023

  31. [31]

    M., et al

    Guo, Y ., Rafelski, M., Faber, S. M., et al. 2016, ApJ, 833, 37

    2016

  32. [32]

    E., Brammer, G

    Heintz, K. E., Brammer, G. B., Watson, D., et al. 2025, A&A, 693, A60

    2025

  33. [33]

    F., Kereˇs, D., O˜norbe, J., et al

    Hopkins, P. F., Kereˇs, D., O˜norbe, J., et al. 2014, MNRAS, 445, 581

    2014

  34. [34]

    K., Matsuda, Y ., et al

    Iwata, I., Inoue, A. K., Matsuda, Y ., et al. 2009, ApJ, 692, 1287

    2009

  35. [35]

    E., Sanders, R

    Jeong, M.-S., Shapley, A. E., Sanders, R. L., et al. 2020, ApJL, 902, L16

    2020

  36. [36]

    D., Rodighiero, G., et al

    Kashino, D., Silverman, J. D., Rodighiero, G., et al. 2013, ApJL, 777, L8

    2013

  37. [37]

    1998, ARA&A, 36, 189

    Kennicutt, Robert C., J. 1998, ARA&A, 36, 189

    1998

  38. [38]

    C., Tamblyn, P., & Congdon, C

    Kennicutt, Jr., R. C., Tamblyn, P., & Congdon, C. E. 1994, ApJ, 435, 22

    1994

  39. [39]

    2013, ApJ, 771, 62

    Kreckel, K., Groves, B., Schinnerer, E., et al. 2013, ApJ, 771, 62

    2013

  40. [40]

    2013, ApJL, 775, L16

    Kriek, M., & Conroy, C. 2013, ApJL, 775, L16

    2013

  41. [41]

    Leitherer, C., & Heckman, T. M. 1995, ApJS, 96, 9

    1995

  42. [42]

    C., & Faisst, A

    Leitherer, C., Lee, J. C., & Faisst, A. 2019, AJ, 158, 192

    2019

  43. [43]

    E., et al

    Lorenz, B., Kriek, M., Shapley, A. E., et al. 2023, ApJ, 951, 29 —. 2024, ApJ, 975, 187

    2023

  44. [44]

    A., Kriek, M., et al

    Lorenz, B., Suess, K. A., Kriek, M., et al. 2025, ApJL, 988, L20

    2025

  45. [45]

    2024, A&A, 691, A87

    Marques-Chaves, R., Schaerer, D., Vanzella, E., et al. 2024, A&A, 691, A87

    2024

  46. [46]

    F., & Ostriker, E

    McKee, C. F., & Ostriker, E. C. 2007, ARA&A, 45, 565

    2007

  47. [47]

    J., Dunlop, J

    McLure, R. J., Dunlop, J. S., Cullen, F., et al. 2018, MNRAS, 476, 3991

    2018

  48. [48]

    R., Heckman, T

    Meurer, G. R., Heckman, T. M., & Calzetti, D. 1999, ApJ, 521, 64

    1999

  49. [49]

    R., Wong, O

    Meurer, G. R., Wong, O. I., Kim, J. H., et al. 2009, ApJ, 695, 765

    2009

  50. [50]

    E., Shapley, A

    Mostardi, R. E., Shapley, A. E., Nestor, D. B., et al. 2013, ApJ, 779, 65

    2013

  51. [51]

    B., Shapley, A

    Nestor, D. B., Shapley, A. E., Steidel, C. C., & Siana, B. 2011, ApJ, 736, 18

    2011

  52. [52]

    2024, ApJ, 972, 156

    Neufeld, C., van Dokkum, P., Asali, Y ., et al. 2024, ApJ, 972, 156

    2024

  53. [53]

    G., Weiner, B

    Noeske, K. G., Weiner, B. J., Faber, S. M., et al. 2007, ApJL, 660, L43

    2007

  54. [54]

    2009, A&A, 499, 69

    Noll, S., Pierini, D., Cimatti, A., et al. 2009, A&A, 499, 69

    2009

  55. [55]

    J., Shapley, A., Steidel, C

    Pahl, A. J., Shapley, A., Steidel, C. C., Chen, Y ., & Reddy, N. A. 2021, MNRAS, 505, 2447

    2021

  56. [56]

    J., Shapley, A., Reddy, N

    Pahl, A. J., Shapley, A., Reddy, N. A., et al. 2026, ApJ, 996, 37 P´erez-Gonz´alez, P. G., Barro, G., Annunziatella, M., et al. 2023, ApJL, 946, L16

    2026

  57. [57]

    2022, ApJ, 928, 71

    Papovich, C. 2022, ApJ, 928, 71

    2022

  58. [58]

    H., Kriek, M., Brammer, G

    Price, S. H., Kriek, M., Brammer, G. B., et al. 2014, ApJ, 788, 86

    2014

  59. [59]

    A., Erb, D

    Reddy, N. A., Erb, D. K., Pettini, M., Steidel, C. C., & Shapley, A. E. 2010, ApJ, 712, 1070

    2010

  60. [60]

    A., Pettini, M., Steidel, C

    Reddy, N. A., Pettini, M., Steidel, C. C., et al. 2012, ApJ, 754, 25

    2012

  61. [61]

    A., Steidel, C

    Reddy, N. A., Steidel, C. C., Fadda, D., et al. 2006, ApJ, 644, 792

    2006

  62. [62]

    A., Kriek, M., Shapley, A

    Reddy, N. A., Kriek, M., Shapley, A. E., et al. 2015, ApJ, 806, 259

    2015

  63. [63]

    A., Oesch, P

    Reddy, N. A., Oesch, P. A., Bouwens, R. J., et al. 2018, ApJ, 853, 56

    2018

  64. [64]

    A., Shapley, A

    Reddy, N. A., Shapley, A. E., Kriek, M., et al. 2020, ApJ, 902, 123

    2020

  65. [65]

    A., Topping, M

    Reddy, N. A., Topping, M. W., Shapley, A. E., et al. 2022, ApJ, 926, 31

    2022

  66. [66]

    A., Shapley, A

    Reddy, N. A., Shapley, A. E., Sanders, R. L., et al. 2026, ApJ, 999, 15

    2026

  67. [67]

    A., Topping, M

    Rezaee, S., Reddy, N. A., Topping, M. W., et al. 2023, MNRAS, 526, 1512

    2023

  68. [68]

    2020, ARA&A, 58, 529

    Salim, S., & Narayanan, D. 2020, ARA&A, 58, 529

    2020

  69. [69]

    L., Shapley, A

    Sanders, R. L., Shapley, A. E., Kriek, M., et al. 2016, ApJ, 816, 23

    2016

  70. [70]

    L., Shapley, A

    Sanders, R. L., Shapley, A. E., Topping, M. W., et al. 2025, ApJ, 989, 209

    2025

  71. [71]

    2017, ApJ, 847, 76

    Santini, P., Fontana, A., Castellano, M., et al. 2017, ApJ, 847, 76

    2017

  72. [72]

    2015, ApJ, 800, 108

    Scoville, N., Faisst, A., Capak, P., et al. 2015, ApJ, 800, 108

    2015

  73. [73]

    Erb, D. K. 2006, ApJ, 651, 688

    2006

  74. [74]

    E., Steidel, C

    Shapley, A. E., Steidel, C. C., Strom, A. L., et al. 2016, ApJL, 826, L24

    2016

  75. [75]

    Shapley, R.L

    Shapley, A. E., Sanders, R. L., Topping, M. W., et al. 2024, arXiv e-prints, arXiv:2407.00157 —. 2025, ApJ, 980, 242

    work page arXiv 2024

  76. [76]

    A., Shapley, A

    Shivaei, I., Reddy, N. A., Shapley, A. E., et al. 2015, ApJ, 815, 98

    2015

  77. [77]

    C., Feldmann, R., et al

    Sparre, M., Hayward, C. C., Feldmann, R., et al. 2017, MNRAS, 466, 88

    2017

  78. [78]

    S., Steinhardt, C

    Speagle, J. S., Steinhardt, C. L., Capak, P. L., & Silverman, J. D. 2014, ApJS, 214, 15

    2014

  79. [79]

    R., & Eldridge, J

    Stanway, E. R., & Eldridge, J. J. 2018, MNRAS, 479, 75

    2018

  80. [80]

    C., Bogosavljevi´c, M., Shapley, A

    Steidel, C. C., Bogosavljevi´c, M., Shapley, A. E., et al. 2018, ApJ, 869, 123

    2018

Showing first 80 references.

This paper was first reviewed by grok-4.3 on June 29, 2026.