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arxiv: 2606.17571 · v2 · pith:5SS7RGBNnew · submitted 2026-06-16 · 🌌 astro-ph.GA · astro-ph.CO

The Incidence of Large Ionized Bubbles at Redshift 13

Peter Ziwei Hu , Massimo Stiavelli , Colin Norman This is my paper

Pith reviewed 2026-06-27 00:33 UTC · model grok-4.3

classification 🌌 astro-ph.GA astro-ph.CO
keywords ionized bubblesreionizationhigh-redshift galaxiesUV luminosity functionJWSTLyα emittersz=13intergalactic medium
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The pith

JWST UV luminosity functions imply ionized bubbles of radius 2.5 cMpc occur at z=13 with surface density 1.33×10^{-2} arcmin^{-2} per Δz=1.

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

The paper calculates how often galaxy populations at redshift 13 produce large ionized bubbles using observed UV luminosity functions from JWST. It benchmarks against the bubble size needed for the Lyα source reported by Witstok et al. The central result is a surface density of about 0.013 such regions per square arcminute per unit redshift in the fiducial model. This matters because these bubbles influence when reionization begins, how Lyα light escapes, and the structure seen in 21 cm maps. The calculation treats bubbles as isolated, providing a lower bound on the incidence of ionized environments.

Core claim

We model the incidence of galaxy-driven ionized bubbles at z≈13 using JWST UV luminosity functions and take the Witstok et al. (2025) Lyα source as a benchmark for the relevant bubble scale of R ≥ 2.5 cMpc. For the fiducial case with UVLF from Donnan et al. 2024, f_esc=0.2, log ξ_ion=25.5, f_duty=1, and C=3, the sky surface density Σ≥2.5 is ≃ 1.33×10^{-2} arcmin^{-2} per Δz=1. Bubbles are treated as independent spheres, making this a conservative baseline. We conclude that Witstok-sized regions are plausible in UVLF-calibrated galaxy-driven models, though the specific source may require unusual conditions.

What carries the argument

The sky surface density Σ≥2.5 of independent ionized spheres with comoving radius R ≥ 2.5 cMpc, computed by integrating the bubble production rate over the UV luminosity function using fixed ionizing parameters.

Load-bearing premise

The model assumes fixed uniform values for the ionizing escape fraction, efficiency, duty cycle, and clumping factor across the entire galaxy population at z≈13 with no redshift evolution or scatter.

What would settle it

A direct count of Lyα emitters or large ionized regions at z=13 showing a surface density substantially different from 1.33×10^{-2} arcmin^{-2} per unit redshift would test whether the fiducial parameters correctly predict the incidence.

Figures

Figures reproduced from arXiv: 2606.17571 by Colin Norman, Massimo Stiavelli, Peter Ziwei Hu.

Figure 1
Figure 1. Figure 1: Bubble age versus ionizing photon rate at z ≈ 13. Left: radius-hybrid rendering, with low-radius bubbles summarized by median radius heatmap and the largest bubbles shown individually. Right: number density heatmap of the same population [PITH_FULL_IMAGE:figures/full_fig_p005_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Global neutral hydrogen fraction as a function of redshift. The solid black curve shows the volume-weighted neutral fraction from our bubble-growth simulation, while the dashed red curve indicates the value inferred from the cumulative ionizing photon budget. Colored observational constraints are overlaid for comparison and grouped by probe: damping-wing constraints from GRBs, individual quasars, stacked q… view at source ↗
Figure 3
Figure 3. Figure 3: Slices through the ionization field at different redshifts, showing the progression from isolated ionized regions to widespread overlap. From top-left to bottom-right, redshifts decrease as z = 15, 13, 11, 9, 8, 7. the ionization field at several redshifts. At early times, the IGM is dominated by neutral hydrogen, punctu- [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Merged BSD diagnostics at z ≈ 13 with redshift evolution. Top row: (a) simulation bubble size distribution at z ≈ 13 compared with analytic prescriptions; (b) contribution to the ionized volume, dQHII/d ln R, with age-distribution overlays at selected radii. Bottom row: Redshift evolution of (c) BSD and (d) ionized-volume contribution per logarithmic radius bin. The red reference line marks R = 2.5 cMpc. t… view at source ↗
Figure 5
Figure 5. Figure 5: Source-level probability of producing a Witstok-sized bubble, R ≥ 2.5 cMpc, near z = 13, calibrated from the simulated source population in a fixed-age slice around the adopted source age. Panel (a) maps probability in the fesc–log ξion plane, and panel (b) compresses the same dependence into the combined emissivity shift S at fixed observed UV luminosity and source-age assumption. Panels (c)–(f) show one-… view at source ↗
Figure 6
Figure 6. Figure 6: Bubble size distributions at z ≈ 13 across parameter groups. Each panel varies one ingredient around the fiducial Donnan UVLF model, shown in black and labeled as baseline. Panels (a)–(d) vary Mlim, fesc, ξion, and the clumping factor C. Panels (e) and (f) vary the duty cycle for a representative subset fduty ∈ {0.2, 0.4, 0.6, 0.8} on top of the C. T. Donnan et al. (2024) and R. J. Bouwens et al. (2021) UV… view at source ↗
Figure 7
Figure 7. Figure 7: Merger/percolation diagnostics. Panel (a) shows 10 bubble growth histories in a merger-enabled catalog overlaid on the volume-normalized density of merger events in redshift and radius. Panel (b) shows the merger-event rate density with per-snapshot estimates and a moving average. Panel (c) compares the probability that merger events produce or preserve a Witstok-sized region, R ≥ 2.5 cMpc, with and withou… view at source ↗
Figure 8
Figure 8. Figure 8: Component decomposition of the Method-2 analytic BSD at z ≃ 13. The seed BSD ψ1(R) from Eq. (A6) is broken into N-fold multiplicity contributions ψN (R) from Eq. (A8) and overlaid on the simulation measurement, isolating which source populations and overlap regimes control the high-R tail. B. FULL PARAMETER SUITE AND SUPPLEMENTARY DIAGNOSTICS [PITH_FULL_IMAGE:figures/full_fig_p018_8.png] view at source ↗
read the original abstract

Ionized bubbles around the first galaxies link early galaxy growth, ionizing photon escape, intergalactic-medium topology, Ly{\alpha} visibility, 21 cm structure, and the timing of reionization. With JWST now constraining both the abundance of luminous galaxies at $z\gtrsim 10$ and rare Ly$\alpha$ emitters deep in the neutral era, it is timely to ask how often galaxy populations produce large ionized environments. We model the incidence of galaxy-driven ionized bubbles at $z\approx 13$ using JWST UV luminosity functions, taking the Ly$\alpha$ source reported by Witstok et al. (2025) as a benchmark for the relevant bubble scale. We quantify the incidence of regions with comoving radius $R\ge 2.5$ cMpc through the sky surface density $\Sigma_{\ge 2.5}$ at $z\approx 13$. For our fiducial case (UVLF from Donnan et al. 2024 with $f_{\mathrm{esc}}=0.2$, $\log\xi_{\mathrm{ion}}=25.5$, $f_{\mathrm{duty}}=1$, and $C=3$), we find $\Sigma_{\ge 2.5}\simeq 1.33\times 10^{-2}$ arcmin$^{-2}$ per $\Delta z=1$. Because bubbles are treated as independent spheres with random source positions and no union of overlaps, this is a conservative baseline for the abundance of connected ionized environments. We conclude that Witstok-sized regions are plausible in UVLF-calibrated galaxy-driven models. This is a population-level statement, however, and the specific Witstok source may still require unusual effective ionizing efficiency, recent fading or burstiness, or a non-stellar ionizing contribution.

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 / 0 minor

Summary. The paper calculates the incidence of galaxy-driven ionized bubbles with comoving radius R ≥ 2.5 cMpc at z ≈ 13 by integrating the Donnan et al. (2024) UV luminosity function above the luminosity threshold set by fiducial parameters (f_esc = 0.2, log ξ_ion = 25.5, f_duty = 1, C = 3). Under the independent-sphere approximation with random source positions, it reports a surface density Σ_≥2.5 ≃ 1.33 × 10^{-2} arcmin^{-2} per Δz = 1 and concludes that Witstok-sized regions are plausible in UVLF-calibrated models, while noting that the specific observed source may require additional factors such as burstiness.

Significance. If the central calculation holds, the work supplies a quantitative, population-level baseline for the abundance of large ionized regions at z ≈ 13 that directly connects recent JWST UVLF constraints to IGM topology, Lyα visibility, and the timing of reionization. The explicit conservative treatment via non-overlapping spheres strengthens its utility as a reference point for interpreting rare high-redshift Lyα emitters.

major comments (2)
  1. [Abstract (fiducial case)] Abstract (fiducial case): The reported Σ_≥2.5 is obtained by integrating the UVLF above the minimum galaxy luminosity that produces R = 2.5 cMpc when the ionizing photon rate is computed with the fixed values f_esc = 0.2, log ξ_ion = 25.5, f_duty = 1 and the recombination rate with C = 3. Because the bright-end UVLF slope at z ≈ 13 is steep, this integral is exponentially sensitive to small shifts in these parameters, yet the manuscript presents only the single fiducial point with no sensitivity tests, scatter, or error propagation.
  2. [Abstract] Abstract: The conclusion that Witstok-sized regions are plausible rests on this single fiducial surface density. Without quantifying the plausible range of Σ_≥2.5 under reasonable variations of the four free parameters (consistent with lower-redshift constraints), the robustness of the population-level claim cannot be assessed.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their careful reading of the manuscript and for identifying the need to assess sensitivity to the model parameters. We agree that this strengthens the robustness of the population-level claim and will revise the manuscript accordingly.

read point-by-point responses

  1. Referee: [Abstract (fiducial case)] The reported Σ_≥2.5 is obtained by integrating the UVLF above the minimum galaxy luminosity that produces R = 2.5 cMpc when the ionizing photon rate is computed with the fixed values f_esc = 0.2, log ξ_ion = 25.5, f_duty = 1 and the recombination rate with C = 3. Because the bright-end UVLF slope at z ≈ 13 is steep, this integral is exponentially sensitive to small shifts in these parameters, yet the manuscript presents only the single fiducial point with no sensitivity tests, scatter, or error propagation.

    Authors: We agree that the steep bright-end slope renders the integral sensitive to the adopted parameters and that presenting only the fiducial case limits evaluation of robustness. In the revised manuscript we will add a new section (or appendix) that quantifies Σ_≥2.5 for plausible variations of f_esc, log ξ_ion, f_duty and C drawn from lower-redshift constraints. This will include a table of resulting surface densities and a brief discussion of the range. revision: yes

  2. Referee: [Abstract] The conclusion that Witstok-sized regions are plausible rests on this single fiducial surface density. Without quantifying the plausible range of Σ_≥2.5 under reasonable variations of the four free parameters (consistent with lower-redshift constraints), the robustness of the population-level claim cannot be assessed.

    Authors: We concur that an explicit range under parameter variations will better support the population-level statement. The revised version will provide this quantification, allowing direct assessment of how Σ_≥2.5 changes across the adopted parameter space while retaining the fiducial result as the baseline case motivated by typical values at lower redshift. revision: yes

Circularity Check

0 steps flagged

No significant circularity; standard model evaluation using external UVLF

full rationale

The paper computes Σ_≥2.5 by integrating the external Donnan et al. (2024) UVLF above the luminosity threshold set by the explicitly chosen fiducial parameters f_esc=0.2, log ξ_ion=25.5, f_duty=1 and C=3 in the standard bubble-radius relation. This is a direct model evaluation, not a derivation that reduces to its own inputs by construction. No self-citations are load-bearing, no parameters are fitted within the paper and then relabeled as predictions, and the result is presented as a population-level plausibility check rather than an independent first-principles claim. The derivation chain is self-contained against the stated external inputs and assumptions.

Axiom & Free-Parameter Ledger

4 free parameters · 2 axioms · 0 invented entities

The incidence calculation rests on four chosen parameters (f_esc, ξ_ion, f_duty, C) taken as constant, the Donnan et al. 2024 UVLF as an external input, and the assumption that bubbles remain isolated spheres. No new entities are postulated.

free parameters (4)
  • f_esc = 0.2
    Ionizing photon escape fraction set to 0.2 for the fiducial run; directly scales bubble size.
  • log ξ_ion = 25.5
    Ionizing efficiency set to 25.5; converts UV luminosity to ionizing photon rate.
  • f_duty = 1
    Duty cycle set to 1; assumes continuous star formation.
  • C = 3
    Clumping factor set to 3; affects recombination rate inside bubbles.
axioms (2)
  • domain assumption Bubbles can be treated as independent, non-overlapping spheres with random source positions.
    Explicitly stated in abstract as the basis for the conservative baseline.
  • domain assumption The UV luminosity function from Donnan et al. 2024 accurately represents the galaxy population at z≈13.
    Used as the direct input for source abundance.

pith-pipeline@v0.9.1-grok · 5866 in / 1798 out tokens · 40688 ms · 2026-06-27T00:33:33.510360+00:00 · methodology

discussion (0)

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Works this paper leans on

54 extracted references · 54 canonical work pages · 16 internal anchors

  1. [1]

    Planck 2018 results. VI. Cosmological parameters

    , keywords =. doi:10.1051/0004-6361/201833910 , archiveprefix =. 1807.06209 , primaryclass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201833910

  2. [2]

    doi:10.1051/0004-6361/201936630 , archiveprefix =

    , keywords =. doi:10.1051/0004-6361/201936630 , archiveprefix =. 1908.09856 , primaryclass =

    work page doi:10.1051/0004-6361/201936630 1908

  3. [3]

    The Growth of HII Regions During Reionization

    , keywords =. doi:10.1086/423025 , archiveprefix =. astro-ph/0403697 , primaryclass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/423025

  4. [4]

    2007, MNRAS, 382, 1415, doi: 10.1111/j.1365-2966.2007.12487.x

    , keywords =. doi:10.1111/j.1365-2966.2007.11489.x , archiveprefix =. astro-ph/0610094 , primaryclass =

    work page doi:10.1111/j.1365-2966.2007.11489.x 2007

  5. [5]

    Simulations and Analytic Calculations of Bubble Growth During Hydrogen Reionization

    , keywords =. doi:10.1086/509597 , archiveprefix =. astro-ph/0604177 , primaryclass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/509597

  6. [6]

    Reionization Through the Lens of Percolation Theory

    , keywords =. doi:10.1093/mnras/stw104 , archiveprefix =. 1511.01521 , primaryclass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stw104

  7. [7]

    The Distribution of Bubble Sizes During Reionization

    , keywords =. doi:10.1093/mnras/stw1542 , archiveprefix =. 1511.01506 , primaryclass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stw1542

  8. [8]

    Bubble size statistics during reionization from 21-cm tomography

    , keywords =. doi:10.1093/mnras/stx2539 , archiveprefix =. 1706.00665 , primaryclass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stx2539

  9. [9]

    doi:10.3847/2041-8213/acade4 , archiveprefix =

    , keywords =. doi:10.3847/2041-8213/acade4 , archiveprefix =. 2211.05792 , primaryclass =

    work page doi:10.3847/2041-8213/acade4 2041

  10. [10]

    doi:10.3847/1538-4357/ad9b2c , archiveprefix =

    , keywords =. doi:10.3847/1538-4357/ad9b2c , archiveprefix =. 2406.18352 , primaryclass =

    work page doi:10.3847/1538-4357/ad9b2c

  11. [11]

    doi:10.3847/1538-3881/abf83e , archiveprefix =

    , keywords =. doi:10.3847/1538-3881/abf83e , archiveprefix =. 2102.07775 , primaryclass =

    work page doi:10.3847/1538-3881/abf83e

  12. [13]

    The Universe is Reionizing at z~7: Bayesian Inference of the IGM Neutral Fraction Using Ly$\alpha$ Emission from Galaxies

    , keywords =. doi:10.3847/1538-4357/aab0a7 , archiveprefix =. 1709.05356 , primaryclass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/aab0a7

  13. [14]

    and others , title =

    Tang, Mengtao and Hutchison, Thomas and Whitler, Luke and Endsley, Ryan and Stark, Daniel P. and others , title =. Monthly Notices of the Royal Astronomical Society , year =. doi:10.1093/mnras/stae2037 , archiveprefix =. 2403.03171 , primaryclass =

    work page doi:10.1093/mnras/stae2037

  14. [15]

    , keywords =

    , keywords =. doi:10.1093/mnras/stae1857 , archiveprefix =. 2306.05295 , primaryclass =

    work page doi:10.1093/mnras/stae1857

  15. [16]

    doi:10.3847/1538-4357/addc74 , archiveprefix =

    , keywords =. doi:10.3847/1538-4357/addc74 , archiveprefix =. 2410.01905 , primaryclass =

    work page doi:10.3847/1538-4357/addc74

  16. [17]

    doi:10.3847/1538-4357/ae486c , archiveprefix =

    , keywords =. doi:10.3847/1538-4357/ae486c , archiveprefix =. 2602.16706 , primaryclass =

    work page doi:10.3847/1538-4357/ae486c

  17. [18]

    Relatively Fast and Reasonably Furious: Evidence for Increased Burstiness in Smaller Halos at Cosmic Dawn

    , keywords =. doi:10.1093/mnras/stag415 , archiveprefix =. 2601.07912 , primaryclass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stag415

  18. [19]

    doi:10.1038/s41586-025-08779-5 , archiveprefix =

    , keywords =. doi:10.1038/s41586-025-08779-5 , archiveprefix =. 2408.16608 , primaryclass =

    work page doi:10.1038/s41586-025-08779-5

  19. [20]

    doi:10.3847/1538-4357/acaf50 , archiveprefix =

    , keywords =. doi:10.3847/1538-4357/acaf50 , archiveprefix =. 2210.04912 , primaryclass =

    work page doi:10.3847/1538-4357/acaf50

  20. [21]

    doi:10.1051/0004-6361/202554158 , archiveprefix =

    , keywords =. doi:10.1051/0004-6361/202554158 , archiveprefix =. 2503.05576 , primaryclass =

    work page doi:10.1051/0004-6361/202554158

  21. [22]

    doi:10.3847/1538-4357/adda45 , archiveprefix =

    , keywords =. doi:10.3847/1538-4357/adda45 , archiveprefix =. 2505.09097 , primaryclass =

    work page doi:10.3847/1538-4357/adda45

  22. [23]

    C., Schawinski, K., et al

    , keywords =. doi:10.1111/j.1365-2966.2009.14486.x , archiveprefix =. 0807.3963 , primaryclass =

    work page doi:10.1111/j.1365-2966.2009.14486.x 2009

  23. [24]

    2012, MNRAS, 427, 1266, doi: 10.1111/j.1365-2966.2012.22060.x

    , keywords =. doi:10.1111/j.1365-2966.2012.22114.x , archiveprefix =. 1209.2489 , primaryclass =

    work page doi:10.1111/j.1365-2966.2012.22114.x 2012

  24. [25]

    Inhomogeneous recombinations during cosmic reionization

    , keywords =. doi:10.1093/mnras/stu377 , archiveprefix =. 1402.2298 , primaryclass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stu377

  25. [26]

    Implications for the Cosmic Reionization from the Optical Afterglow Spectrum of the Gamma-Ray Burst 050904 at z = 6.3

    , keywords =. doi:10.1093/pasj/58.3.485 , archiveprefix =. astro-ph/0512154 , primaryclass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/pasj/58.3.485

  26. [27]

    doi:10.1111/j.1365-2966.2010.17535.x , eprint =

    , keywords =. doi:10.1111/j.1365-2966.2010.16701.x , archiveprefix =. 1001.3415 , primaryclass =

    work page doi:10.1111/j.1365-2966.2010.16701.x 2010

  27. [28]

    Quantitative Constraints on the Reionization History from the IGM Damping Wing Signature in Two Quasars at z > 7

    , keywords =. doi:10.3847/1538-4357/aad6dc , archiveprefix =. 1802.06066 , primaryclass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/aad6dc

  28. [29]

    The Discovery of A Luminous Broad Absorption Line Quasar at A Redshift of 7.02

    , keywords =. doi:10.3847/2041-8213/aaf1d2 , archiveprefix =. 1810.11925 , primaryclass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/2041-8213/aaf1d2 2041

  29. [30]

    doi:10.1093/mnras/stac825 , archiveprefix =

    , keywords =. doi:10.1093/mnras/stac825 , archiveprefix =. 2112.04091 , primaryclass =

    work page doi:10.1093/mnras/stac825

  30. [31]

    doi:10.1093/mnras/staa505 , archiveprefix =

    , keywords =. doi:10.1093/mnras/staa505 , archiveprefix =. 1912.01050 , primaryclass =

    work page doi:10.1093/mnras/staa505 1912

  31. [32]

    doi:10.3847/1538-4357/ae232b , archiveprefix =

    , keywords =. doi:10.3847/1538-4357/ae232b , archiveprefix =. 2504.04683 , primaryclass =

    work page doi:10.3847/1538-4357/ae232b

  32. [33]

    Constraining the neutral fraction of hydrogen in the IGM at redshift 7.5

    , keywords =. doi:10.3847/1538-4357/ab1de7 , archiveprefix =. 1901.09001 , primaryclass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/ab1de7 1901

  33. [34]

    Inferences on the Timeline of Reionization at z~8 From the KMOS Lens-Amplified Spectroscopic Survey

    , keywords =. doi:10.1093/mnras/stz632 , archiveprefix =. 1901.11045 , primaryclass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stz632 1901

  34. [35]

    doi:10.1093/mnras/stac1963 , archiveprefix =

    , keywords =. doi:10.1093/mnras/stac1963 , archiveprefix =. 2111.14912 , primaryclass =

    work page doi:10.1093/mnras/stac1963

  35. [36]

    Model-independent evidence in favor of an end to reionization by z~6

    , keywords =. doi:10.1093/mnras/stu2449 , archiveprefix =. 1411.5375 , primaryclass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stu2449

  36. [37]

    doi:10.1093/mnras/staf1862 , archiveprefix =

    , keywords =. doi:10.1093/mnras/staf1862 , archiveprefix =. 2510.25829 , primaryclass =

    work page doi:10.1093/mnras/staf1862

  37. [38]

    doi:10.1038/s41586-024-07043-6 , archiveprefix =

    , keywords =. doi:10.1038/s41586-024-07043-6 , archiveprefix =. 2308.08540 , primaryclass =

    work page doi:10.1038/s41586-024-07043-6

  38. [39]

    doi:10.1038/s41586-024-07052-5 , archiveprefix =

    , keywords =. doi:10.1038/s41586-024-07052-5 , archiveprefix =. 2305.12492 , primaryclass =

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

  39. [40]

    , keywords =

    , keywords =. doi:10.1038/s41586-024-07227-0 , archiveprefix =. 2302.14155 , primaryclass =

    work page doi:10.1038/s41586-024-07227-0

  40. [41]

    doi:10.1093/mnras/stab3710 , archiveprefix =

    , keywords =. doi:10.1093/mnras/stab3710 , archiveprefix =. 2110.00584 , primaryclass =

    work page doi:10.1093/mnras/stab3710

  41. [42]

    doi:10.1093/mnras/staa1266 , archiveprefix =

    , keywords =. doi:10.1093/mnras/staa1266 , archiveprefix =. 1811.11192 , primaryclass =

    work page doi:10.1093/mnras/staa1266

  42. [43]

    doi:10.1093/mnras/stae839 , archiveprefix =

    , keywords =. doi:10.1093/mnras/stae839 , archiveprefix =. 2309.06475 , primaryclass =

    work page doi:10.1093/mnras/stae839

  43. [44]

    doi:10.1093/mnras/stad3605 , archiveprefix =

    , keywords =. doi:10.1093/mnras/stad3605 , archiveprefix =. 2310.01112 , primaryclass =

    work page doi:10.1093/mnras/stad3605

  44. [45]

    doi:10.1051/0004-6361/202345866 , archiveprefix =

    , keywords =. doi:10.1051/0004-6361/202345866 , archiveprefix =. 2301.02816 , primaryclass =

    work page doi:10.1051/0004-6361/202345866

  45. [46]

    , keywords =

    , keywords =. doi:10.1051/0004-6361/202347132 , archiveprefix =. 2306.04536 , primaryclass =

    work page doi:10.1051/0004-6361/202347132

  46. [47]

    doi:10.1093/mnras/stad2228 , archiveprefix =

    , keywords =. doi:10.1093/mnras/stad2228 , archiveprefix =. 2210.06504 , primaryclass =

    work page doi:10.1093/mnras/stad2228

  47. [48]

    doi:10.1051/0004-6361/202553820 , archiveprefix =

    , keywords =. doi:10.1051/0004-6361/202553820 , archiveprefix =. 2501.11702 , primaryclass =

    work page doi:10.1051/0004-6361/202553820

  48. [49]

    doi:10.3847/1538-4357/ad1e5f , archiveprefix =

    , keywords =. doi:10.3847/1538-4357/ad1e5f , archiveprefix =. 2309.05714 , primaryclass =

    work page doi:10.3847/1538-4357/ad1e5f

  49. [50]

    doi:10.3847/1538-4357/ab7cc9 , archiveprefix =

    , keywords =. doi:10.3847/1538-4357/ab7cc9 , archiveprefix =. 1907.13130 , primaryclass =

    work page doi:10.3847/1538-4357/ab7cc9 1907

  50. [51]

    doi:10.1038/s41550-023-01918-w , archiveprefix =

    Nature Astronomy , keywords =. doi:10.1038/s41550-023-01918-w , archiveprefix =. 2212.04568 , primaryclass =

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

  51. [52]

    doi:10.1051/0004-6361/202346159 , archiveprefix =

    , keywords =. doi:10.1051/0004-6361/202346159 , archiveprefix =. 2302.07256 , primaryclass =

    work page doi:10.1051/0004-6361/202346159

  52. [53]

    doi:10.1093/mnras/stac1046 , archiveprefix =

    , keywords =. doi:10.1093/mnras/stac1046 , archiveprefix =. 2108.03699 , primaryclass =

    work page doi:10.1093/mnras/stac1046

  53. [54]

    doi:10.1038/s41550-024-02397-3 , archiveprefix =

    Nature Astronomy , keywords =. doi:10.1038/s41550-024-02397-3 , archiveprefix =. 2403.10491 , primaryclass =

    work page doi:10.1038/s41550-024-02397-3

  54. [55]

    Cosmic Star Formation History

    , keywords =. doi:10.1146/annurev-astro-081811-125615 , archiveprefix =. 1403.0007 , primaryclass =

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