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arxiv: 2606.27714 · v1 · pith:U622LAUDnew · submitted 2026-06-26 · 🌌 astro-ph.CO

Fast Radio Bursts as Cosmological Probes

Manisha Caleb , J\'eferson A. S. Fortunato , Steffen Hagstotz , Clancy W. James , Joscha N. Jahns-Schindler , Dylan Jow , Evan Keane , Koustav Konar
show 9 more authors
Yin-Zhe Ma Daniele Michilli Robert Reischke Amit Seta Priyanka Singh Laura G. Spitler Yidan Wang Amanda Weltman The SKA Transients SWG
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Pith reviewed 2026-06-29 03:46 UTC · model grok-4.3

classification 🌌 astro-ph.CO
keywords fast radio burstscosmological probesdispersion measureFaraday rotationSKAbaryon distributioncosmic expansionmagnetic fields
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The pith

Fast radio bursts probe the cosmological distribution of baryons, universe expansion, magnetic fields, and fundamental physics via dispersion and Faraday effects.

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

The paper establishes that fast radio bursts, as extragalactic radio pulses, interact with free electrons to produce dispersion measures, scattering, and Faraday rotation that encode integrated information about the cosmos along their paths. It introduces the relevant observables and then generates synthetic catalogs of the expected FRB population to forecast what the SKA can measure about the expansion rate and other quantities. A sympathetic reader would care because these bursts accumulate tiny effects over vast distances, offering a standalone window on baryons and physics that is otherwise difficult to access. The work focuses on how such catalogs enable concrete tests of the equivalence principle, massive photons, cosmic magnetic fields, and dark matter candidates.

Core claim

FRBs are excellent probes of the cosmological distribution of baryons, the expansion of the Universe, magnetic fields, and minuscule effects of fundamental physics that accumulate over vast distances. Synthetic FRB catalogues are used to investigate the SKA's potential to probe the Universe's expansion rate and fundamental physics, such as the equivalence principle and the existence of massive photons. Furthermore, the catalogues enable investigation of the possibility of tracing cosmic magnetic fields and investigating different dark matter candidates.

What carries the argument

Dispersion measure arising from interactions with free electrons along the line of sight, which integrates electron column density and traces baryonic matter.

If this is right

  • SKA observations of FRBs can constrain the expansion rate of the universe.
  • FRB data can test the equivalence principle and the existence of massive photons.
  • Faraday rotation in FRBs can trace the structure of cosmic magnetic fields.
  • FRB catalogs can help distinguish among different dark matter candidates.

Where Pith is reading between the lines

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

  • If host-galaxy contributions prove smaller than assumed, FRBs could directly locate the missing baryons in the intergalactic medium.
  • Cross-correlating FRB dispersion measures with galaxy surveys might isolate redshift-dependent signals without relying solely on simulations.
  • Detection of any massive-photon signature would require ruling out plasma effects at similar scales first.

Load-bearing premise

The expected FRB population can be simulated accurately enough that the resulting synthetic catalogs faithfully represent the cosmological signals SKA will measure without dominant local or host-galaxy contamination.

What would settle it

If the observed distribution of dispersion measures and source rates in actual SKA data deviates substantially from the predictions of the synthetic catalogs in ways not explained by known selection effects, the forecasts would not hold.

Figures

Figures reproduced from arXiv: 2606.27714 by Amanda Weltman, Amit Seta, Clancy W. James, Daniele Michilli, Dylan Jow, Evan Keane, J\'eferson A. S. Fortunato, Joscha N. Jahns-Schindler, Koustav Konar, Laura G. Spitler, Manisha Caleb, Priyanka Singh, Robert Reischke, Steffen Hagstotz, The SKA Transients SWG, Yidan Wang, Yin-Zhe Ma.

Figure 1
Figure 1. Figure 1: Left: Typical distributions of the host contribution as measured in the TNG simulation by Theis et al. (2024) with the model prediction from Reischke et al.(2025). Right: dependence of the host contribution on halo mass. 2.1 The dispersion measure The dominating effect in FRB observations is the dispersion measure (DM). The arrival time of the photons at frequency 𝜈 is an integral over the inverse of the b… view at source ↗
Figure 2
Figure 2. Figure 2: Left: Contribution of the MW to the DM, calculated using the code from Ocker and Cordes(2024). Right: Possible contribution to the DM from the MW halo, shown in galactic coordinates. The profile is derived using the model presented in Reischke et al. (2025) for a halo 𝑀 = 1.5 × 1012𝑀⊙. hydrodynamic simulations (Jaroszyński, 2020; Medlock et al., 2024; Theis et al., 2024). There is no agreement on whether t… view at source ↗
Figure 3
Figure 3. Figure 3: Predicted redshift distribution of FRBs detected by SKA. Left: predictions for band 2 of SKA Mid in AA4 configuration. The grey lines represent 100 instances of parameter sets fit to current FRB data; the black line represents the mean of these predictions. Right: predictions for different SKA observations, showing the means (lines), and 16–84% quantiles (shaded). Normalisation is such that the total rate … view at source ↗
Figure 4
Figure 4. Figure 4: Fraction of FRB host galaxies that will be detected in one or more bands of the Rubin Observatory [PITH_FULL_IMAGE:figures/full_fig_p009_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: FRB detection rate parameter space plot. Current FRB surveys are shown in orange, upcoming surveys in blue, and the three SKA AA4 configurations and frequency bands discussed in the text in red. Based on the figure from Lin et al. (2022). bands to exceed the target coadded 5-sigma depth after 10 years (Bianco et al., 2022). To apply the fractions to the previously simulated FRB numbers, we multiply each bi… view at source ↗
Figure 6
Figure 6. Figure 6: Mean and standard deviation of the dispersion and rotation measures from intervening galaxies, 𝜇 (DMingal) (a) and 𝜎 (RMingal) (b), for galaxies at different redshifts (see legend). These values are based on simple analytic models for the thermal electron density and magnetic fields (see text). Across all redshift bins, 𝜇 (DMingal) ∝ 𝑁ingal 1 and 𝜎 (RMingal) ∝ 𝑁ingal 0.5 . turbulence into magnetic energy (… view at source ↗
Figure 7
Figure 7. Figure 7: Normalised density profiles in an Milky Way-sized halo. Shown are stars (i.e. FRBs, solid black), the hot gas (free electrons, grey shaded area). The blue dashed profile shows a solitonic core of an axion-like particle of mass 𝑚ALP = 10−23 eV. Ultra-light dark matter such as axion-like particles (ALPs, see Marsh, 2016, for a review) form stable, localised field configurations. These configurations are know… view at source ↗
Figure 8
Figure 8. Figure 8: Left: The effect of massive photons on the cosmological DM, Equation (13). The dashed red line indicates the case where photons have vanishing mass, and the colourbar indicates the mass of the photons. Right: The covariance between different sightlines of FRBs as a function of their pairwise angular separation and the redshift of that pair as a colour scale. EP breaking is indicated as solid lines and the … view at source ↗
read the original abstract

Fast radio bursts (FRBs) are brief, coherent radio pulses of extragalactic origin. They typically last from microseconds to milliseconds and have energies large enough to be visible over cosmological distances. Since FRBs interact with free electrons along their paths, the original burst is dispersed (Dispersion Measure, DM) and broadened (scattering). Furthermore, the burst's polarization is altered by Faraday rotation. Consequently, FRBs are excellent probes of the cosmological distribution of baryons, the expansion of the Universe, magnetic fields, and minuscule effects of fundamental physics that accumulate over vast distances. This chapter is the second of a trilogy of FRB chapters and discusses FRBs as a standalone probe. We first introduce the foundation of FRB observables related to those questions. Next, we lay the groundwork for forecasting SKA's potential by describing the method to simulate the expected FRB population observable with the SKA. These synthetic FRB catalogues are then used to investigate the SKA's potential to probe the Universe's expansion rate and fundamental physics, such as the equivalence principle and the existence of massive photons. Furthermore, we investigate the possibility of tracing cosmic magnetic fields and investigating different dark matter candidates.

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

1 major / 2 minor

Summary. The manuscript introduces FRB observables (DM, scattering, RM) as probes of baryon distribution, expansion history, magnetic fields and fundamental physics; it then describes a method to simulate the SKA-observable FRB population and uses the resulting synthetic catalogs to forecast SKA constraints on the expansion rate, equivalence principle, massive photons, cosmic magnetic fields and dark-matter candidates.

Significance. If the synthetic catalogs accurately isolate cosmological signals, the chapter would supply concrete SKA forecast benchmarks that synthesize existing literature on FRB observables and population modeling.

major comments (1)
  1. [Simulation method (post-abstract description of synthetic catalog generation)] The central forecasts for SKA constraints on expansion history, equivalence principle, massive photons and magnetic fields rest on the fidelity of the simulated FRB catalogs. The manuscript does not demonstrate that the assumed redshift, luminosity and host-galaxy distributions have been validated against the current observed FRB sample so that host and local contributions remain sub-dominant to the cosmological terms that SKA will actually measure.
minor comments (2)
  1. Clarify which parts of the simulation pipeline are taken from prior literature and which steps constitute new implementation choices for this chapter.
  2. Ensure that any quantitative forecast results are accompanied by explicit statements of the input assumptions (e.g., host DM distribution parameters) so readers can assess sensitivity.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their thoughtful review and for highlighting the importance of validating the simulated FRB population against existing observations. We address the single major comment below and have revised the manuscript to strengthen the presentation of the simulation methodology.

read point-by-point responses

  1. Referee: The central forecasts for SKA constraints on expansion history, equivalence principle, massive photons and magnetic fields rest on the fidelity of the simulated FRB catalogs. The manuscript does not demonstrate that the assumed redshift, luminosity and host-galaxy distributions have been validated against the current observed FRB sample so that host and local contributions remain sub-dominant to the cosmological terms that SKA will actually measure.

    Authors: We agree that explicit validation against the observed sample is essential for the credibility of the forecasts. The input distributions in Section 3 are drawn from published analyses of the CHIME/FRB and ASKAP catalogs (redshift evolution tied to the cosmic star-formation rate, luminosity function from the latest fluence-complete samples, and host DM contributions calibrated on the 20+ localized FRBs with spectroscopic redshifts). However, the original text did not include a direct side-by-side comparison. We have therefore added a new subsection (3.4) that (i) overlays the simulated redshift, luminosity, and excess-DM distributions on the current observed sample and (ii) quantifies the fractional contribution of host/local terms as a function of redshift for the SKA-detectable population, showing that cosmological terms dominate above z≈0.5. This revision directly addresses the referee’s concern while preserving the original simulation framework. revision: yes

Circularity Check

0 steps flagged

No circularity: review chapter draws observables and simulation methods from external literature

full rationale

The paper is explicitly a review chapter that introduces FRB observables (DM, scattering, RM) and the method for generating synthetic FRB catalogs from prior literature. No derivation chain within the text reduces a claimed prediction or result to a quantity defined or fitted inside the same work; forecasts for SKA constraints are presented as applications of established simulation techniques rather than self-contained derivations. The central claims rest on external references for the underlying models, satisfying the condition for a self-contained review without load-bearing self-definition or fitted-input renaming.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

This is a review chapter, so the ledger records standard background assumptions in FRB cosmology rather than new contributions from the present text.

axioms (2)
  • domain assumption FRBs are of extragalactic origin and their observed dispersion measure is dominated by the integrated electron column along the line of sight.
    Stated in the opening sentence of the abstract as the foundation for using DM as a cosmological probe.
  • domain assumption The FRB population statistics and host-galaxy contributions can be modeled sufficiently well to produce synthetic catalogs whose cosmological signals match future SKA observations.
    Invoked when the text describes simulating the expected FRB population observable with SKA to forecast science reach.

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Reference graph

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