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arxiv: 2606.29903 · v1 · pith:PSUUYZ4Hnew · submitted 2026-06-29 · 🌌 astro-ph.CO · astro-ph.GA

High-Redshift Signatures from the Cosmic Dawn and the Epoch of Reionization

Rennan Barkana , Oliver Basquette , Ankita Bera , Jennifer Yik Ham Chan , Pravabati Chingangbam , Hector Afonso G. Cruz , Saswata Dasgupta , Kanan K. Datta
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Anastasia Fialkov Sambit K. Giri Qin Han Ilian T. Iliev Bohua Li Teppei Minoda Shikhar Mittal Julian B. Mu\~noz Suvedha Suresh Naik Janakee Raste Aurel Schneider Sudipta Sikder Kinwah Wu Yidong Xu Bin Yue Meng Zhang Meng-Lin Zhao
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Pith reviewed 2026-06-30 05:33 UTC · model grok-4.3

classification 🌌 astro-ph.CO astro-ph.GA
keywords 21-cm signalCosmic DawnEpoch of ReionizationSKA-Lowprimordial black holesdark matterLambdaCDMhigh-redshift astrophysics
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The pith

The 21-cm signal from the Cosmic Dawn and Epoch of Reionization carries both standard signatures from the first stars and galaxies and exotic ones from new physics that SKA-Low can detect.

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

This chapter reviews the astrophysical and cosmological processes that shape the 21-cm signal at high redshifts. It covers contributions from first stars, galaxies and black holes within the standard LambdaCDM model as well as speculative effects from primordial black holes, modified dark matter, non-standard fluctuations or bright radio galaxies. The analysis places these signatures in the context of the sensitivity expected from SKA-Low in its AA* and AA4 configurations. A reader would care because detection of the signal would map the formation of the first luminous objects and could reveal physics beyond the standard cosmological framework.

Core claim

The chapter establishes that the 21-cm signal during Cosmic Dawn and the Epoch of Reionization is shaped by standard LambdaCDM sources including the first stars, galaxies and black holes as well as by exotic sources such as primordial black holes, modifications to the dark matter sector, non-standard primordial fluctuations or strongly emitting radio galaxies, and that both classes of signatures are potentially observable with SKA-Low.

What carries the argument

The 21-cm brightness temperature fluctuations from neutral hydrogen at high redshifts, modulated by heating, ionization and energy injection from the listed sources.

If this is right

  • Detection of standard signatures will constrain the properties and timing of the first stars and galaxies.
  • Detection of exotic signatures could indicate the existence of primordial black holes or non-standard dark matter.
  • Observations will refine the history of reionization and the thermal evolution of the intergalactic medium.
  • Absence of exotic signals will place upper limits on the abundance or strength of the new-physics sources considered.

Where Pith is reading between the lines

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

  • Confirmation of the standard signals would extend the tested timeline of structure formation to redshifts currently inaccessible to direct galaxy observations.
  • The 21-cm data could be combined with other high-redshift probes to reduce degeneracies between astrophysical and cosmological parameters.
  • If exotic signals appear, follow-up observations at different frequencies could help isolate the responsible mechanism.

Load-bearing premise

The SKA-Low telescope will reach its projected sensitivity in the AA* and AA4 configurations and the cited theoretical models accurately represent the relevant physics.

What would settle it

SKA-Low measurements that show no 21-cm fluctuations at the amplitudes or spectral shapes predicted by any of the standard or exotic models would falsify the detectability claims.

Figures

Figures reproduced from arXiv: 2606.29903 by Anastasia Fialkov, Ankita Bera, Aurel Schneider, Bin Yue, Bohua Li, Hector Afonso G. Cruz, Ilian T. Iliev, Janakee Raste, Jennifer Yik Ham Chan, Julian B. Mu\~noz, Kanan K. Datta, Kinwah Wu, Meng-Lin Zhao, Meng Zhang, Oliver Basquette, Pravabati Chingangbam, Qin Han, Rennan Barkana, Sambit K. Giri, Saswata Dasgupta, Shikhar Mittal, Sudipta Sikder, Suvedha Suresh Naik, Teppei Minoda, Yidong Xu.

Figure 1
Figure 1. Figure 1: The 21-cm signal across cosmic epochs. The figure illustrates the evolution of the 21-cm signal from the Dark Ages through Cosmic Dawn to the end of the Epoch of Reionization, with reionization completed by 𝑧 ∼ 6. Top: The sky-averaged (global) 21-cm brightness temperature, 𝑇 𝑏, as a function of redshift (top x-axis)/frequency (bottom x-axis). The absorption trough at 𝑧 ∼ 17 reflects the onset of strong Ly… view at source ↗
Figure 2
Figure 2. Figure 2: The 21-cm power spectrum at 𝑧 ∼ 8 for different parameters in 𝑓★ − 𝑀h, 𝑓duty − 𝑀h and 𝑓esc − 𝑀h relations. Fiducial model: 𝜖0 = 0.13, 𝛾lo = 0.46, 𝛾hi = 0.82, 𝑀𝑝 = 2 × 1012 𝑀⊙, 𝑀turn = 5 × 108 𝑀⊙, 𝑀esc,0 = 1010 𝑀⊙, 𝑓esc,0 = 0.1 and 𝛼esc = 0.5. Model 1: 𝑀turn = 2 × 108 𝑀⊙ and 𝑀esc,0 = 3.2 × 109 𝑀⊙, others same to fiducial model. Model 2: 𝜖0 = 0.02 and 𝛾lo = 0.17, others same to fiducial model. Model 3: 𝜖0 = … view at source ↗
Figure 3
Figure 3. Figure 3: Forecasted Bayesian constraints on the Pop III IMF from the 21-cm power spectrum. We show the 21-cm power spectra simulated using the semi-numerical code 21cmSPACE for three candidate truncated power-law Pop III IMFs (different line colours), of the form 𝑑𝑁/𝑑𝑀 ∝ 𝑀−𝛼III , 𝑀 ∈ [𝑀min, 𝑀max]. Our bottom-heavy, fiducial and top-heavy IMFs correspond to the Sal, Int-1 and Top IMFs considered in Gessey-Jones et a… view at source ↗
Figure 4
Figure 4. Figure 4: Left: The 21-cm power spectrum in Cosmic Dawn, in the absence/presence of DCBHs. DCBHs abundance is normalized to ∼ 10−2 Mpc−3 at 𝑧 ∼ 10. Right: The 21-cm power spectrum in EoR, in the absence/presence of SMBHs. The SMBHs number density is normalized to be ∼ 2 × 10−3 Mpc−3 at 𝑧 ∼ 6. In all panels the filled regions refer to the SKA-low AA* uncertainties with 𝑡obs = 1080 hr and a bandwidth of 10 MHz. The un… view at source ↗
Figure 5
Figure 5. Figure 5: A depiction of how velocity-induced acoustic oscillations (VAOs) can be used to measure cosmic expansion. Left: The 21-cm power spectrum at 𝑧 = 13, 16, 22 computed with Zeus21 (Muñoz, 2023; Cruz et al., 2025) in the absence (dotted) and presence (solid) of dark matter-baryon relative velocities 𝑣cb. Including the streaming effects alter the spectral shape, leading to more pronounced acoustic features whose… view at source ↗
Figure 6
Figure 6. Figure 6: An estimate of the maximum 21-cm power spectrum from models with strongly-emitting radio galaxies, given current observational constraints (based on [PITH_FULL_IMAGE:figures/full_fig_p024_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Left: The 21 cm power spectra at 𝑧 ∼ 10 in the absence (black)/presence of DM annihilation (red) and decay (blue). Right: Similar to the left panel, however now the power spectra at 𝑘 = 0.05 Mpc−1 as functions of redshift are plotted. In all panels filled regions are SKA-AA* uncertainties for 𝑡obs = 1080 hr and bandwidth 10 MHz, calculated by 21cmSense, the left panel adopts moderate foreground removal mod… view at source ↗
Figure 8
Figure 8. Figure 8: The power spectrum evolution over redshift (left panel) and wavenumber (right panel). The shaded regions correspond to the error due to cosmic variance and instrumental noise (𝑡obs = 1000h, Δ ln 𝑘 = 0.5) with AA* (blue) and AA4 (green) layout of SKA-Low. particle energies correspond to higher minimum halo masses capable of hosting luminous sources. In this work, we adopt the WDM scenario as a representativ… view at source ↗
Figure 9
Figure 9. Figure 9: The 21 cm power spectra at different redshifts simulated for the featureless power law model (solid black), models with bump-like features (violet) and various EoR models (green). The shaded region is the 95% uncertainty estimated for SKA-AA4 using 21cmSense. 5.7 Other exotic signatures Topological defects such as superconducting cosmic strings are predicted by several different ex￾tensions to the standard… view at source ↗
read the original abstract

In this chapter, we provide a comprehensive overview of the astrophysical and cosmological processes that shape the 21-cm signal during Cosmic Dawn and the Epoch of Reionization. We investigate both standard and exotic signatures potentially observable with SKA-Low. Standard signatures are those expected within the $\Lambda$CDM framework, including contributions from the first stars, galaxies, and black holes. Exotic signatures are more speculative indicating new physics, such as primordial black holes, modifications to the dark matter sector, non-standard primordial fluctuations, or strongly emitting radio galaxies. The effects of these different sources or scenarios are evaluated in the context of the expected sensitivity of SKA-Low, considering the AA* and AA4 configurations. The chapter aims to provide an overview of the theoretical landscape of 21-cm signatures and to highlight how the forthcoming SKA-Low observations will improve our understanding of astrophysical processes at early times and may open the door towards new physics beyond the $\Lambda$CDM framework.

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

0 major / 0 minor

Summary. The manuscript is a review chapter providing a comprehensive overview of astrophysical and cosmological processes shaping the 21-cm signal during Cosmic Dawn and the Epoch of Reionization. It covers standard ΛCDM signatures from first stars, galaxies, and black holes, as well as exotic signatures from new physics (e.g., primordial black holes, modified dark matter, non-standard primordial fluctuations, or radio galaxies), and evaluates their detectability against SKA-Low sensitivity forecasts in the AA* and AA4 configurations.

Significance. If the literature summaries are accurate, the chapter offers a useful synthesis of the 21-cm theoretical landscape, highlighting how SKA-Low observations can constrain early-universe astrophysics and potentially test beyond-ΛCDM scenarios. It compiles existing models and sensitivity projections without introducing new derivations, which is appropriate for a review format.

Simulated Author's Rebuttal

0 responses · 0 unresolved

We thank the referee for their positive review of the manuscript and for recommending acceptance. We are pleased that the chapter is regarded as a useful synthesis of the theoretical 21-cm landscape and its detectability with SKA-Low.

Circularity Check

0 steps flagged

Review chapter presents no new derivations or self-referential predictions

full rationale

This is a review chapter that compiles and summarizes existing literature on 21-cm signals during Cosmic Dawn and Reionization, including standard and exotic signatures in the context of SKA-Low sensitivity. No original derivations, fitted parameters, or quantitative predictions are introduced within the paper itself; all content is framed as overviews of prior published models. Consequently, there are no load-bearing steps that reduce by construction to inputs defined in the paper, satisfying the default expectation of no significant circularity.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

This is a review paper that summarizes existing literature; it introduces no new free parameters, axioms, or invented entities of its own.

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