pith. sign in

arxiv: 2605.22914 · v1 · pith:TJV4W3QOnew · submitted 2026-05-21 · 🌌 astro-ph.GA

No Blue without Red: Evolutionary Properties of Super-Early Galaxies

A. Ferrara , G. Rodighiero , S. Carniani , Z. Zhang , M. Kohandel , B. Das This is my paper

Pith reviewed 2026-05-25 05:49 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords super-early galaxiesAttenuation-Free Modeldust attenuationradiation-driven outflowsJWST observationshigh-redshift galaxiesRed Monster phaseBlue Monster phase
0
0 comments X

The pith

Super-early galaxies transition from dust-obscured red phases to UV-bright blue phases as outflows clear central dust.

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

The paper applies the Attenuation-Free Model to a sample of 32 spectroscopically confirmed galaxies at z greater than 10. In this framework radiation-driven outflows move dust outward from galaxy centers, lowering effective attenuation and allowing UV light to escape more freely. Galaxies therefore begin in a reddened state before becoming bluer once the central regions are cleared. The derived properties include halo masses around 10 to the 10.7 solar masses, star formation efficiencies of 0.01 to 0.05, and frequent super-Eddington conditions that drive the outflows. The red source EGS-z11-R0 at z=11.45 is presented as an example caught in the obscured stage of this sequence.

Core claim

Within the Attenuation-Free Model, in which radiation-driven outflows redistribute dust to large galactic radii thereby reducing effective attenuation, the 32 super-early galaxies reside in massive halos with log M/Msun approximately 10.7, show moderate star formation efficiencies 0.01 less than or equal to epsilon star less than or equal to 0.05, and frequently reach super-Eddington conditions that trigger powerful outflows. This leads to a proposed evolutionary sequence from a dust-obscured Red Monster phase to a UV-bright Blue Monster phase as outflows clear central regions, with the red galaxy EGS-z11-R0 at z=11.45 interpreted as observed during the obscured phase. Compact sources with r

What carries the argument

The Attenuation-Free Model, in which radiation-driven outflows redistribute dust to large galactic radii thereby reducing effective attenuation.

If this is right

  • Galaxies in massive halos with moderate star formation efficiency frequently reach super-Eddington conditions that drive powerful outflows.
  • The observed diversity in UV properties of z greater than 10 galaxies arises from different stages in the dust-clearing evolutionary sequence.
  • Compact sources with effective radius less than or equal to 150 pc are difficult to reconcile within the model and may instead be AGN-dominated.
  • Future JWST and ALMA observations can test the predicted dust distributions and outflow properties.

Where Pith is reading between the lines

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

  • If the sequence holds, UV-selected surveys will miss a population of still-obscured red galaxies at high redshift.
  • Outflow velocity measurements in additional sources could directly correlate with the degree of blue appearance.
  • The same dust-redistribution mechanism may operate at slightly lower redshifts and shape the visibility of galaxies during reionization.

Load-bearing premise

Radiation-driven outflows are the dominant process that redistributes dust and controls effective attenuation in these super-early galaxies.

What would settle it

A large population of compact red galaxies at z greater than 10 whose dust and emission properties cannot be explained by AGN activity would contradict the model's account of the observed UV diversity.

Figures

Figures reproduced from arXiv: 2605.22914 by A. Ferrara, B. Das, G. Rodighiero, M. Kohandel, S. Carniani, Z. Zhang.

Figure 1
Figure 1. Figure 1: Predicted redshift evolution of the effective galaxy radius, re (eq. 1), for different values of the halo circular velocities, vc, as shown by the legend. The data points represent our super-early galaxy sample presented in Tab. 1 along with the references. Open points indicate up￾per limits. Also shown are the best-fit curves and 1σ errors (shaded region) to high-z galaxy data from Shibuya et al. (2015) a… view at source ↗
Figure 2
Figure 2. Figure 2: Attenuation-Free Model (AFM) predictions for the UV luminosity function at z ≃ 11 (left panel) and z ≃ 12 (right) compared to available JWST data. The model is well fitted by a double-power law (red curve) of the form ϕ(MUV) = ϕ∗[10(1+α)x + 10(1+β)x ] −1 , where x = −0.4(M∗ − MUV), with parameters shown in the panels. Data points are taken from Donnan et al. (2024); Finkelstein et al. (2023); Casey et al. … view at source ↗
Figure 3
Figure 3. Figure 3: The comoving star formation rate density evolu￾tion predicted by AFM (blue line) is compared with avail￾able data and other models (lines) in the literature. Data are taken from McLeod et al. (2023); Adams et al. (2024); Harikane et al. (2024); Whitler et al. (2023); P´erez-Gonz´alez et al. (2025); Chemerynska et al. (2024); Madau & Dickinson (2014); Harikane et al. (2022); Mason et al. (2023); Sun & Furla… view at source ↗
Figure 4
Figure 4. Figure 4: Properties of super-early galaxies predicted by AFM. For the 17 extended galaxies (ordered according to their redshift, shown on the top axis) in the sample we show the instantaneous star formation efficiency (top left panel), spin parameter (top right), halo mass (middle left), stellar age (middle right), outflow outer radius in units of the effective radius (bottom left), metallicity (bottom right). Data… view at source ↗
Figure 5
Figure 5. Figure 5: Sketch of the possible evolutionary path leading to the formation of a Blue Monster in the Attenuation-Free Model (AFM), based on the detailed study of GS-z14-0 at z = 14.18 presented in Ferrara (2024b). The values of the lookback time and of the SFR are only indicative, as they depend on the properties of individual galaxies, as discussed in the text. 3.1.4. Stellar ages Our predictions on the stellar age… view at source ↗
Figure 6
Figure 6. Figure 6: Evolutionary path of super-early galaxies shown in the redshift - circular velocity (proxy for halo mass) plane. The green lines (bottom to top) are the tracks of galaxies whose star formation activity starts at z∗ = 9, 10, .., 25, respectively. Also shown are stellar mass isocountours (blue dotted). As the circular velocity, halo and stellar mass increase with time the galaxy accumulates dust and becomes … view at source ↗
read the original abstract

The discovery of numerous luminous, super-early galaxies at $z>10$ by JWST has revealed a striking diversity in their ultraviolet (UV) properties, ranging from extremely blue, dust-poor systems to a smaller population of significantly reddened sources. We investigate the physical origin of this diversity within the framework of the Attenuation-Free Model (AFM), in which radiation-driven outflows redistribute dust to large galactic radii, reducing the effective attenuation. Applying the model to a sample of 32 spectroscopically confirmed super-early galaxies, we derive their key physical properties, including halo mass, star formation efficiency, metallicity, and outflow extent. We find that these systems reside in massive halos ($\log M/M_\odot \sim 10.7$) and exhibit moderate ($0.01 \lesssim \epsilon_* \lesssim 0.05$) star formation efficiencies, while frequently reaching super-Eddington conditions that trigger powerful outflows. Within this framework, we propose an evolutionary sequence in which galaxies transition from a dust-obscured ``Red Monster'' phase to a UV-bright ``Blue Monster'' phase as outflows clear their central regions. The recently confirmed red galaxy EGS-z11-R0 at $z=11.45$ is naturally interpreted as a system observed during this obscured phase. Compact ($r_e \lesssim 150$ pc) sources are instead difficult to reconcile within AFM; we speculate that their emission is dominated by an AGN. Our results provide a unified interpretation of super-early galaxy properties and highlight the key role of radiation-driven outflows in shaping galaxy evolution at cosmic dawn. Future observations with JWST and ALMA will be essential to test these predictions and further constrain the nature of the earliest galaxies.

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 / 2 minor

Summary. The manuscript applies the Attenuation-Free Model (AFM) to a sample of 32 spectroscopically confirmed super-early galaxies at z>10. It derives halo masses (log M/M_⊙ ~10.7), star-formation efficiencies (0.01 ≲ ε_* ≲ 0.05), metallicities, and outflow extents, then proposes an evolutionary sequence in which galaxies transition from a dust-obscured 'Red Monster' phase to a UV-bright 'Blue Monster' phase as radiation-driven outflows clear central dust. EGS-z11-R0 at z=11.45 is interpreted as observed during the obscured phase; compact sources (r_e ≲ 150 pc) are speculated to be AGN-dominated. The work claims this framework unifies the observed UV diversity and highlights outflows at cosmic dawn.

Significance. If the AFM framework and the proposed sequence are shown to be preferred over standard attenuation models, the results would offer a coherent physical picture for the diversity of JWST-detected z>10 galaxies and generate falsifiable predictions for future observations. The application to 32 objects and the explicit identification of testable observables constitute strengths. However, the significance is limited by the absence of quantitative model comparisons or dynamical validation.

major comments (2)
  1. [Results / Application of the model] Application of AFM to the 32-galaxy sample: halo masses and star-formation efficiencies are obtained inside the AFM from the same observational data later used to illustrate the red-to-blue sequence. This renders the evolutionary 'predictions' for individual objects (including EGS-z11-R0) quantities fitted within the model rather than independent tests, undermining the claim that the sequence is data-driven.
  2. [Discussion / Evolutionary sequence] Evolutionary sequence section: the assertion that radiation-driven outflows dominate dust redistribution and produce the observed UV diversity is presented without any quantitative comparison demonstrating that AFM reproduces the UV slopes or colors of the sample better than conventional screen or clumpy-dust attenuation models. No dynamical simulation or timescale calculation is supplied to show that the red-to-blue transition occurs on the required ~10–100 Myr timescales at z~11.
minor comments (2)
  1. The abstract states derived quantities without accompanying equations, error budgets, or data tables; the full manuscript should supply these (including explicit definitions of E_p or outflow extent) so that the central claims can be reproduced.
  2. Notation for star-formation efficiency (ε_*) and halo mass should be defined at first use and kept consistent with standard conventions in the high-z galaxy literature.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive comments on our manuscript. We address each major comment point by point below and indicate where revisions will be made.

read point-by-point responses

  1. Referee: [Results / Application of the model] Application of AFM to the 32-galaxy sample: halo masses and star-formation efficiencies are obtained inside the AFM from the same observational data later used to illustrate the red-to-blue sequence. This renders the evolutionary 'predictions' for individual objects (including EGS-z11-R0) quantities fitted within the model rather than independent tests, undermining the claim that the sequence is data-driven.

    Authors: We agree that the halo masses, star-formation efficiencies, and other parameters are derived by fitting the AFM to the observed properties of each galaxy. The evolutionary sequence is therefore an interpretive framework that organizes these model-derived quantities into a physical picture consistent with the observed UV diversity, rather than a set of independent predictions. In the revised manuscript we will explicitly clarify this distinction in the discussion, rephrase claims about the sequence to emphasize its model-guided nature, and stress that future observations are required to test the framework. revision: yes

  2. Referee: [Discussion / Evolutionary sequence] Evolutionary sequence section: the assertion that radiation-driven outflows dominate dust redistribution and produce the observed UV diversity is presented without any quantitative comparison demonstrating that AFM reproduces the UV slopes or colors of the sample better than conventional screen or clumpy-dust attenuation models. No dynamical simulation or timescale calculation is supplied to show that the red-to-blue transition occurs on the required ~10–100 Myr timescales at z~11.

    Authors: We acknowledge that the current manuscript contains no direct quantitative comparisons of AFM predictions against standard attenuation models and provides no dynamical simulations or explicit timescale calculations. Such analyses lie beyond the scope of this work. In revision we will expand the discussion to include a qualitative assessment of how AFM expectations align with the observed UV slopes in the sample, supply order-of-magnitude timescale estimates derived from the model parameters, and explicitly note the absence of full dynamical validation as a limitation to be addressed in future studies. revision: partial

Circularity Check

0 steps flagged

No significant circularity; derivation applies external framework to data without self-referential reduction

full rationale

The paper takes the Attenuation-Free Model (AFM) as an input framework, applies it to derive halo masses, star-formation efficiencies, and outflow extents for the 32-galaxy sample, and then interprets an evolutionary red-to-blue sequence within that framework. No equation or derivation step is shown in which a claimed prediction or first-principles result is mathematically identical to a fitted parameter or to the input data by construction. The AFM itself is presented as a pre-existing model rather than derived here, and no self-citation chain is invoked to establish uniqueness or to forbid alternatives. The central claims remain conditional on the AFM assumption and are therefore model-dependent rather than tautological.

Axiom & Free-Parameter Ledger

2 free parameters · 1 axioms · 0 invented entities

The central claim rests on the pre-existing Attenuation-Free Model plus two fitted quantities (halo mass and star-formation efficiency) extracted from the 32-galaxy sample; no new entities are postulated.

free parameters (2)
  • halo mass log M/M_sun = ~10.7
    Derived for the sample and stated as ~10.7
  • star formation efficiency epsilon_* = 0.01-0.05
    Moderate range 0.01 to 0.05 derived within the model
axioms (1)
  • domain assumption Radiation-driven outflows redistribute dust to large galactic radii, thereby reducing effective attenuation
    This is the defining premise of the Attenuation-Free Model invoked for all interpretations

pith-pipeline@v0.9.0 · 5863 in / 1284 out tokens · 24670 ms · 2026-05-25T05:49:09.650585+00:00 · methodology

discussion (0)

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

Reference graph

Works this paper leans on

85 extracted references · 85 canonical work pages · 9 internal anchors

  1. [1]

    J., Conselice, C

    Adams, N. J., Conselice, C. J., Ferreira, L., et al. 2023, MNRAS, 518, 4755, doi: 10.1093/mnras/stac3347

    work page doi:10.1093/mnras/stac3347 2023

  2. [2]

    J., Conselice, C

    Adams, N. J., Conselice, C. J., Austin, D., et al. 2024, ApJ, 965, 169, doi: 10.3847/1538-4357/ad2a7b ´Alvarez-M´ arquez, J., Colina, L., Crespo-Gomez, A., et al. 2026, arXiv e-prints, arXiv:2602.02323, doi: 10.48550/arXiv.2602.02323

    work page doi:10.3847/1538-4357/ad2a7b 2024

  3. [3]

    W., Poole, G

    Angel, P. W., Poole, G. B., Ludlow, A. D., et al. 2016, MNRAS, 459, 2106, doi: 10.1093/mnras/stw737

    work page doi:10.1093/mnras/stw737 2016

  4. [4]

    J., & Scott, P

    Asplund, M., Grevesse, N., Sauval, A. J., & Scott, P. 2009, Annual Review of Astronomy and Astrophysics, 47, 481–522, doi: 10.1146/annurev.astro.46.060407.145222

    work page doi:10.1146/annurev.astro.46.060407.145222 2009

  5. [5]

    2025, arXiv e-prints, arXiv:2511.07542, doi: 10.48550/arXiv.2511.07542

    Atek, H., Chisholm, J., Kokorev, V., et al. 2025, arXiv e-prints, arXiv:2511.07542, doi: 10.48550/arXiv.2511.07542

    work page doi:10.48550/arxiv.2511.07542 2025

  6. [6]

    J., Adams, N

    Austin, D., Conselice, C. J., Adams, N. J., et al. 2024, arXiv e-prints, arXiv:2404.10751, doi: 10.48550/arXiv.2404.10751

    work page doi:10.48550/arxiv.2404.10751 2024

  7. [7]

    J., Stefanon, M., Brammer, G., et al

    Bouwens, R. J., Stefanon, M., Brammer, G., et al. 2022, arXiv e-prints, arXiv:2211.02607, doi: 10.48550/arXiv.2211.02607

    work page doi:10.48550/arxiv.2211.02607 2022

  8. [8]

    S., Dekel, A., Kolatt, T

    Bullock, J. S., Dekel, A., Kolatt, T. S., et al. 2001, ApJ, 555, 240, doi: 10.1086/321477

    work page doi:10.1086/321477 2001

  9. [9]

    J., Saxena, A., Cameron, A

    Bunker, A. J., Saxena, A., Cameron, A. J., et al. 2023, arXiv e-prints, arXiv:2302.07256, doi: 10.48550/arXiv.2302.07256

    work page doi:10.48550/arxiv.2302.07256 2023

  10. [10]

    2024, Nature, 633, 318, doi: 10.1038/s41586-024-07860-9

    Carniani, S., Hainline, K., D’Eugenio, F., et al. 2024, Nature, 633, 318, doi: 10.1038/s41586-024-07860-9

    work page doi:10.1038/s41586-024-07860-9 2024

  11. [11]

    Intense and extended CIII] emission suggests a strong outflow in JADES-GS-z14-0

    Carniani, S., Jakobsen, P., Venturi, G., et al. 2026, Intense and extended CIII] emission suggests a strong outflow in JADES-GS-z14-0. https://arxiv.org/abs/2604.11899

    work page internal anchor Pith review Pith/arXiv arXiv 2026

  12. [12]

    M., Akins, H

    Casey, C. M., Akins, H. B., Shuntov, M., et al. 2023, arXiv e-prints, arXiv:2308.10932, doi: 10.48550/arXiv.2308.10932

    work page doi:10.48550/arxiv.2308.10932 2023

  13. [13]

    2023, ApJL, 948, L14, doi: 10.3847/2041-8213/accea5 16Ferrara et al

    Castellano, M., Fontana, A., Treu, T., et al. 2023, ApJL, 948, L14, doi: 10.3847/2041-8213/accea5 16Ferrara et al

    work page doi:10.3847/2041-8213/accea5 2023

  14. [14]

    2024, arXiv e-prints, arXiv:2403.10238, doi: 10.48550/arXiv.2403.10238

    Castellano, M., Napolitano, L., Fontana, A., et al. 2024, arXiv e-prints, arXiv:2403.10238, doi: 10.48550/arXiv.2403.10238

    work page doi:10.48550/arxiv.2403.10238 2024

  15. [15]

    2025, A&A, 704, A158, doi: 10.1051/0004-6361/202555082

    Castellano, M., Fontana, A., Merlin, E., et al. 2025, A&A, 704, A158, doi: 10.1051/0004-6361/202555082

    work page doi:10.1051/0004-6361/202555082 2025

  16. [16]

    J., et al

    Chemerynska, I., Atek, H., Furtak, L. J., et al. 2024, MNRAS, 531, 2615, doi: 10.1093/mnras/stae1260

    work page doi:10.1093/mnras/stae1260 2024

  17. [17]

    2005, SSRv, 116, 625, doi: 10.1007/s11214-005-3592-0

    Ciardi, B., & Ferrara, A. 2005, SSRv, 116, 625, doi: 10.1007/s11214-005-3592-0

    work page doi:10.1007/s11214-005-3592-0 2005

  18. [18]

    A., Wyithe, J

    Correa, C. A., Wyithe, J. S. B., Schaye, J., & Duffy, A. R. 2015, MNRAS, 450, 1521, doi: 10.1093/mnras/stv697

    work page doi:10.1093/mnras/stv697 2015

  19. [19]

    J., McLure, R

    Cullen, F., McLeod, D. J., McLure, R. J., et al. 2024, MNRAS, 531, 997, doi: 10.1093/mnras/stae1211

    work page doi:10.1093/mnras/stae1211 2024

  20. [20]

    2023, Nature Astronomy, doi: 10.1038/s41550-023-01918-w

    Curtis-Lake, E., Carniani, S., Cameron, A., et al. 2023, Nature Astronomy, doi: 10.1038/s41550-023-01918-w

    work page doi:10.1038/s41550-023-01918-w 2023

  21. [21]

    2018, PhR, 780, 1, doi: 10.1016/j.physrep.2018.10.002

    Dayal, P., & Ferrara, A. 2018, PhR, 780, 1, doi: 10.1016/j.physrep.2018.10.002

    work page doi:10.1016/j.physrep.2018.10.002 2018

  22. [22]

    2022, MNRAS, 512, 989, doi: 10.1093/mnras/stac537

    Dayal, P., Ferrara, A., Sommovigo, L., et al. 2022, MNRAS, 512, 989, doi: 10.1093/mnras/stac537

    work page doi:10.1093/mnras/stac537 2022

  23. [23]

    2023, MNRAS, 523, 3201, doi: 10.1093/mnras/stad1557

    Li, Z. 2023, MNRAS, 523, 3201, doi: 10.1093/mnras/stad1557

    work page doi:10.1093/mnras/stad1557 2023

  24. [24]

    T., McLure, R

    Donnan, C. T., McLure, R. J., Dunlop, J. S., et al. 2024, arXiv e-prints, arXiv:2403.03171, doi: 10.48550/arXiv.2403.03171

    work page doi:10.48550/arxiv.2403.03171 2024

  25. [25]

    Spectroscopic confirmation of a large and luminous galaxy with weak emission lines at $\mathbf{z = 13.53}$

    Donnan, C. T., McLeod, D. J., McLure, R. J., et al. 2026, arXiv e-prints, arXiv:2601.11515, doi: 10.48550/arXiv.2601.11515

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2601.11515 2026

  26. [26]

    2024, arXiv e-prints, arXiv:2412.01623, doi: 10.48550/arXiv.2412.01623

    Dottorini, D., Calabr` o, A., Pentericci, L., et al. 2024, arXiv e-prints, arXiv:2412.01623, doi: 10.48550/arXiv.2412.01623

    work page doi:10.48550/arxiv.2412.01623 2024

  27. [27]

    A., & Macci` o, A

    Dutton, A. A., & Macci` o, A. V. 2014, MNRAS, 441, 3359, doi: 10.1093/mnras/stu742

    work page doi:10.1093/mnras/stu742 2014

  28. [28]

    2024a, A&A, 684, A207, doi: 10.1051/0004-6361/202348321 —

    Ferrara, A. 2024a, A&A, 684, A207, doi: 10.1051/0004-6361/202348321 —. 2024b, A&A, 689, A310, doi: 10.1051/0004-6361/202450944

    work page doi:10.1051/0004-6361/202348321

  29. [29]

    2025a, A&A, 694, A215, doi: 10.1051/0004-6361/202452368

    Ferrara, A., Carniani, S., di Mascia, F., et al. 2025a, A&A, 694, A215, doi: 10.1051/0004-6361/202452368

    work page doi:10.1051/0004-6361/202452368

  30. [30]

    2025b, The Open Journal of Astrophysics, 8, 125, doi: 10.33232/001c.143600

    Ferrara, A., Giavalisco, M., Pentericci, L., et al. 2025b, The Open Journal of Astrophysics, 8, 125, doi: 10.33232/001c.143600

    work page doi:10.33232/001c.143600

  31. [31]

    2023, MNRAS, 522, 3986, doi: 10.1093/mnras/stad1095

    Ferrara, A., Pallottini, A., & Dayal, P. 2023, MNRAS, 522, 3986, doi: 10.1093/mnras/stad1095

    work page doi:10.1093/mnras/stad1095 2023

  32. [32]

    2025c, A&A, 694, A286, doi: 10.1051/0004-6361/202452707

    Ferrara, A., Pallottini, A., & Sommovigo, L. 2025c, A&A, 694, A286, doi: 10.1051/0004-6361/202452707

    work page doi:10.1051/0004-6361/202452707

  33. [33]

    2022, MNRAS, 512, 58, doi: 10.1093/mnras/stac460

    Ferrara, A., Sommovigo, L., Dayal, P., et al. 2022, MNRAS, 512, 58, doi: 10.1093/mnras/stac460

    work page doi:10.1093/mnras/stac460 2022

  34. [34]

    L., Leung, G

    Finkelstein, S. L., Leung, G. C. K., Bagley, M. B., et al. 2023, arXiv e-prints, arXiv:2311.04279, doi: 10.48550/arXiv.2311.04279 —. 2024, ApJL, 969, L2, doi: 10.3847/2041-8213/ad4495

    work page doi:10.48550/arxiv.2311.04279 2023

  35. [35]

    2023, ApJL, 943, L27, doi: 10.3847/2041-8213/acb5f2

    Travascio, A. 2023, ApJL, 943, L27, doi: 10.3847/2041-8213/acb5f2

    work page doi:10.3847/2041-8213/acb5f2 2023

  36. [36]

    2024, ApJ, 960, 56, doi: 10.3847/1538-4357/ad0b7e

    Harikane, Y., Nakajima, K., Ouchi, M., et al. 2024, ApJ, 960, 56, doi: 10.3847/1538-4357/ad0b7e

    work page doi:10.3847/1538-4357/ad0b7e 2024

  37. [37]

    2022, ApJS, 259, 20, doi: 10.3847/1538-4365/ac3dfc

    Harikane, Y., Ono, Y., Ouchi, M., et al. 2022, ApJS, 259, 20, doi: 10.3847/1538-4365/ac3dfc

    work page doi:10.3847/1538-4365/ac3dfc 2022

  38. [38]

    2023, ApJS, 265, 5, doi: 10.3847/1538-4365/acaaa9

    Harikane, Y., Ouchi, M., Oguri, M., et al. 2023, ApJS, 265, 5, doi: 10.3847/1538-4365/acaaa9

    work page doi:10.3847/1538-4365/acaaa9 2023

  39. [39]

    K., Ellis, R

    Harikane, Y., Inoue, A. K., Ellis, R. S., et al. 2025, ApJ, 980, 138, doi: 10.3847/1538-4357/ad9b2c

    work page doi:10.3847/1538-4357/ad9b2c 2025

  40. [40]

    G., Alvarez-Marquez, J., et al

    Harikane, Y., Perez-Gonzalez, P. G., Alvarez-Marquez, J., et al. 2026, arXiv e-prints, arXiv:2601.21833, doi: 10.48550/arXiv.2601.21833

    work page doi:10.48550/arxiv.2601.21833 2026

  41. [41]

    Y.-Y., Abdurro’uf, Coe, D., et al

    Hsiao, T. Y.-Y., Abdurro’uf, Coe, D., et al. 2023, arXiv e-prints, arXiv:2305.03042, doi: 10.48550/arXiv.2305.03042

    work page doi:10.48550/arxiv.2305.03042 2023

  42. [42]

    J., Saxena, A., et al

    Katz, H., Cameron, A. J., Saxena, A., et al. 2025, The Open Journal of Astrophysics, 8, 104, doi: 10.33232/001c.142570

    work page doi:10.33232/001c.142570 2025

  43. [43]

    2025, A&A, 704, A39, doi: 10.1051/0004-6361/202555499

    Kohandel, M., Pallottini, A., & Ferrara, A. 2025, A&A, 704, A39, doi: 10.1051/0004-6361/202555499

    work page doi:10.1051/0004-6361/202555499 2025

  44. [44]

    A., Taylor, A

    Kokorev, V., Ch´ avez Ortiz,´O. A., Taylor, A. J., et al. 2025, arXiv e-prints, arXiv:2504.12504, doi: 10.48550/arXiv.2504.12504

    work page doi:10.48550/arxiv.2504.12504 2025

  45. [45]

    Leung, G. C. K., Bagley, M. B., Finkelstein, S. L., et al. 2023, ApJL, 954, L46, doi: 10.3847/2041-8213/acf365

    work page doi:10.3847/2041-8213/acf365 2023

  46. [46]

    C., et al

    Li, Z., Dekel, A., Sarkar, K. C., et al. 2023, arXiv e-prints, arXiv:2311.14662, doi: 10.48550/arXiv.2311.14662

    work page doi:10.48550/arxiv.2311.14662 2023

  47. [47]

    Impact of primordial black holes on the formation of the first stars and galaxies

    Liu, B., & Bromm, V. 2023, arXiv e-prints, arXiv:2312.04085, doi: 10.48550/arXiv.2312.04085 L´ opez-Corredoira, M., & Guti´ errez, C. M. 2026, MNRAS, doi: 10.1093/mnras/stag089 Macci` o, A. V., Dutton, A. A., van den Bosch, F. C., et al. 2007, MNRAS, 378, 55, doi: 10.1111/j.1365-2966.2007.11720.x

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2312.04085 2023

  48. [48]

    2014, Annual Review of Astronomy and Astrophysics, 52, 415, doi: 10.1146/annurev-astro-081811-125615

    Madau, P., & Dickinson, M. 2014, ARA&A, 52, 415, doi: 10.1146/annurev-astro-081811-125615

    work page internal anchor Pith review doi:10.1146/annurev-astro-081811-125615 2014

  49. [49]

    2024, Nature, 627, 59, doi: 10.1038/s41586-024-07052-5

    Maiolino, R., Scholtz, J., Witstok, J., et al. 2024, Nature, 627, 59, doi: 10.1038/s41586-024-07052-5

    work page doi:10.1038/s41586-024-07052-5 2024

  50. [50]

    2026, arXiv e-prints, arXiv:2602.02322, doi: 10.48550/arXiv.2602.02322

    Marques-Chaves, R., ´Alvarez-M´ arquez, J., Colina, L., et al. 2026, arXiv e-prints, arXiv:2602.02322, doi: 10.48550/arXiv.2602.02322

    work page doi:10.48550/arxiv.2602.02322 2026

  51. [51]

    A., Trenti, M., & Treu, T

    Mason, C. A., Trenti, M., & Treu, T. 2023, MNRAS, 521, 497, doi: 10.1093/mnras/stad035 Super-early galaxies17

    work page doi:10.1093/mnras/stad035 2023

  52. [52]

    2025, arXiv e-prints, arXiv:2503.18850, doi: 10.48550/arXiv.2503.18850

    Matteri, A., Ferrara, A., & Pallottini, A. 2025, arXiv e-prints, arXiv:2503.18850, doi: 10.48550/arXiv.2503.18850

    work page doi:10.48550/arxiv.2503.18850 2025

  53. [53]

    J., Donnan, C

    McLeod, D. J., Donnan, C. T., McLure, R. J., et al. 2023, arXiv e-prints, arXiv:2304.14469, doi: 10.48550/arXiv.2304.14469

    work page doi:10.48550/arxiv.2304.14469 2023

  54. [54]

    A search for the first galaxies across $>0.6$ deg$^2$ of JWST imaging: new evidence for a rapid decline in star-formation activity at $z>12$

    McLeod, D. J., Dunlop, J. S., McLure, R. J., et al. 2026, A search for the first galaxies across>0.6 deg 2 of JWST imaging: new evidence for a rapid decline in star-formation activity atz >12. https://arxiv.org/abs/2604.16666

    work page internal anchor Pith review Pith/arXiv arXiv 2026

  55. [55]

    A., Leja, J., et al

    Mitsuhashi, I., Suess, K. A., Leja, J., et al. 2025, arXiv e-prints, arXiv:2510.13240, doi: 10.48550/arXiv.2510.13240

    work page doi:10.48550/arxiv.2510.13240 2025

  56. [56]

    C., & White, S

    Mo, H., van den Bosch, F. C., & White, S. 2010, Galaxy Formation and Evolution, doi: 10.1017/CBO9780511807244

    work page doi:10.1017/cbo9780511807244 2010

  57. [57]

    M., Finkelstein, S

    Morales, A. M., Finkelstein, S. L., Leung, G. C. K., et al. 2024, The Astrophysical Journal Letters, 964, L24, doi: 10.3847/2041-8213/ad2de4

    work page doi:10.3847/2041-8213/ad2de4 2024

  58. [58]

    2024, ApJ, 963, 9, doi: 10.3847/1538-4357/ad1404

    Morishita, T., Stiavelli, M., Chary, R.-R., et al. 2024, ApJ, 963, 9, doi: 10.3847/1538-4357/ad1404

    work page doi:10.3847/1538-4357/ad1404 2024

  59. [59]

    P., Oesch, P

    Naidu, R. P., Oesch, P. A., van Dokkum, P., et al. 2022, Two Remarkably Luminous Galaxy Candidates at z≈11−13 Revealed by JWST, arXiv, doi: 10.48550/ARXIV.2207.09434

    work page doi:10.48550/arxiv.2207.09434 2022

  60. [60]

    P., Oesch, P

    Naidu, R. P., Oesch, P. A., Brammer, G., et al. 2025, arXiv e-prints, arXiv:2505.11263, doi: 10.48550/arXiv.2505.11263

    work page doi:10.48550/arxiv.2505.11263 2025

  61. [61]

    2024, ApJ, 975, 238, doi: 10.3847/1538-4357/ad7d0b

    Nakazato, Y., Ceverino, D., & Yoshida, N. 2024, ApJ, 975, 238, doi: 10.3847/1538-4357/ad7d0b

    work page doi:10.3847/1538-4357/ad7d0b 2024

  62. [62]

    2024, arXiv e-prints, arXiv:2412.07598, doi: 10.48550/arXiv.2412.07598

    Nakazato, Y., & Ferrara, A. 2024, arXiv e-prints, arXiv:2412.07598, doi: 10.48550/arXiv.2412.07598

    work page doi:10.48550/arxiv.2412.07598 2024

  63. [63]

    2025, ApJ, 989, 75, doi: 10.3847/1538-4357/ade706 P´ erez-Gonz´ alez, P

    Napolitano, L., Castellano, M., Pentericci, L., et al. 2025, ApJ, 989, 75, doi: 10.3847/1538-4357/ade706 P´ erez-Gonz´ alez, P. G.,¨Ostlin, G., Costantin, L., et al. 2025, arXiv e-prints, arXiv:2503.15594, doi: 10.48550/arXiv.2503.15594 Planck Collaboration, Ade, P. A. R., Aghanim, N., et al. 2014, A&A, 571, A16, doi: 10.1051/0004-6361/201321591 P´ erez-G...

    work page doi:10.3847/1538-4357/ade706 2025

  64. [64]

    JWST Spectroscopic Insights Into the Diversity of Galaxies in the First 500 Myr: Short-Lived Snapshots Along a Common Evolutionary Pathway

    Roberts-Borsani, G., Oesch, P., Ellis, R., et al. 2025, arXiv e-prints, arXiv:2508.21708, doi: 10.48550/arXiv.2508.21708

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2508.21708 2025

  65. [65]

    D., Tacchella, S., et al

    Robertson, B., Johnson, B. D., Tacchella, S., et al. 2024, ApJ, 970, 31, doi: 10.3847/1538-4357/ad463d

    work page doi:10.3847/1538-4357/ad463d 2024

  66. [66]

    2023, MNRAS, 518, L19, doi: 10.1093/mnrasl/slac115

    Rodighiero, G., Bisigello, L., Iani, E., et al. 2023, MNRAS, 518, L19, doi: 10.1093/mnrasl/slac115

    work page doi:10.1093/mnrasl/slac115 2023

  67. [67]

    2026, arXiv e-prints, arXiv:2603.15841, doi: 10.48550/arXiv.2603.15841

    Rodighiero, G., Ferrara, A., Catone, M., et al. 2026, arXiv e-prints, arXiv:2603.15841, doi: 10.48550/arXiv.2603.15841

    work page doi:10.48550/arxiv.2603.15841 2026

  68. [68]

    The Early Maturity of High-Redshift Galaxies: Insights from sSFR, M/L and SFHs at z~7-14

    Santini, P., Castellano, M., Calabr` o, A., et al. 2025, arXiv e-prints, arXiv:2512.09139, doi: 10.48550/arXiv.2512.09139

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2512.09139 2025

  69. [69]

    Hitting the slopes: A spectroscopic view of UV continuum slopes of galaxies reveals a reddening at z > 9.5

    Saxena, A., Cameron, A. J., Katz, H., et al. 2024, arXiv e-prints, arXiv:2411.14532, doi: 10.48550/arXiv.2411.14532

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2411.14532 2024

  70. [70]

    2025, A&A, 697, A175, doi: 10.1051/0004-6361/202348804

    Scholtz, J., Maiolino, R., D’Eugenio, F., et al. 2025, A&A, 697, A175, doi: 10.1051/0004-6361/202348804

    work page doi:10.1051/0004-6361/202348804 2025

  71. [71]

    Semenov, V. A. 2026, arXiv e-prints, arXiv:2602.04950, doi: 10.48550/arXiv.2602.04950

    work page doi:10.48550/arxiv.2602.04950 2026

  72. [72]

    2015, ApJS, 219, 15, doi: 10.1088/0067-0049/219/2/15

    Shibuya, T., Ouchi, M., & Harikane, Y. 2015, ApJS, 219, 15, doi: 10.1088/0067-0049/219/2/15

    work page doi:10.1088/0067-0049/219/2/15 2015

  73. [73]

    S., & Dav´ e, R

    Somerville, R. S., & Dav´ e, R. 2015, ARA&A, 53, 51, doi: 10.1146/annurev-astro-082812-140951

    work page internal anchor Pith review doi:10.1146/annurev-astro-082812-140951 2015

  74. [74]

    S., Yung, L

    Somerville, R. S., Yung, L. Y. A., Lancaster, L., et al. 2025, MNRAS, 544, 3774, doi: 10.1093/mnras/staf1824

    work page doi:10.1093/mnras/staf1824 2025

  75. [75]

    2022, MNRAS, 513, 3122, doi: 10.1093/mnras/stac302

    Sommovigo, L., Ferrara, A., Pallottini, A., et al. 2022, MNRAS, 513, 3122, doi: 10.1093/mnras/stac302

    work page doi:10.1093/mnras/stac302 2022

  76. [76]

    Sun, G., & Furlanetto, S. R. 2016, MNRAS, 460, 417, doi: 10.1093/mnras/stw980

    work page doi:10.1093/mnras/stw980 2016

  77. [77]

    P., Mason, C

    Tang, M., Stark, D. P., Mason, C. A., et al. 2026, ApJ, 1001, 38, doi: 10.3847/1538-4357/ae4edb

    work page doi:10.3847/1538-4357/ae4edb 2026

  78. [78]

    P., Plat, A., et al

    Tang, M., Stark, D. P., Plat, A., et al. 2025, ApJ, 991, 217, doi: 10.3847/1538-4357/adfd57

    work page doi:10.3847/1538-4357/adfd57 2025

  79. [79]

    2026, arXiv e-prints, arXiv:2603.06409, doi: 10.48550/arXiv.2603.06409

    Tripodi, R., Napolitano, L., Pentericci, L., et al. 2026, arXiv e-prints, arXiv:2603.06409, doi: 10.48550/arXiv.2603.06409

    work page doi:10.48550/arxiv.2603.06409 2026

  80. [80]

    2023, The Astrophysical Journal Letters, 957, L34, doi: 10.3847/2041-8213/acfe07

    Wang, B., Fujimoto, S., Labb´ e, I., et al. 2023, The Astrophysical Journal Letters, 957, L34, doi: 10.3847/2041-8213/acfe07

    work page doi:10.3847/2041-8213/acfe07 2023

Showing first 80 references.