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arxiv: 2604.24835 · v1 · submitted 2026-04-27 · 🌌 astro-ph.CO · hep-ph

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JWST Constraints on Primordial Magnetic Fields

Malcolm Fairbairn , Mar\'ia Olalla Olea-Romacho , Juan Urrutia , Ville Vaskonen
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Pith reviewed 2026-05-07 17:56 UTC · model grok-4.3

classification 🌌 astro-ph.CO hep-ph
keywords pmfsfieldsmagneticprimordialreionisationabundanceactingapprox
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The pith

JWST UV luminosity function calibration of reionization history bounds primordial magnetic fields to √<B²> < 0.27 nG (n_B=-2) and < 0.18 nG (n_B=2) at 95% CL by ruling out double reionization at z≈24.

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

Primordial magnetic fields are weak magnetic fields thought to have existed since the Big Bang. They exert a Lorentz force on charged gas particles, helping tiny clumps collapse into the first galaxies earlier than they otherwise would. The authors model how this extra early structure speeds up reionization—the process that made the universe transparent again. Using JWST measurements of early galaxies to fix the reionization timeline, they find that strong fields produce two separate reionization episodes, one at very high redshift. This double episode would leave a signature in the cosmic microwave background that is not observed, so the fields cannot be too strong.

Core claim

strong PMFs induce a characteristic double reionisation at z ≈ 24 that is incompatible with CMB measurements of the optical depth, yielding √<B²> < 0.27 nG and < 0.18 nG for n_B = -2 and n_B = 2 respectively at 95% CL using Planck priors on τ.

Load-bearing premise

The reionisation history is accurately calibrated solely with the UV luminosity function from JWST data, and the modeled boost to low-mass halo abundance from the Lorentz force on baryons contains no significant unaccounted systematics or alternative explanations.

Figures

Figures reproduced from arXiv: 2604.24835 by Juan Urrutia, Malcolm Fairbairn, Mar\'ia Olalla Olea-Romacho, Ville Vaskonen.

Figure 1
Figure 1. Figure 1: FIG. 1. UVLFs for CDM best fit (black dashed) and for the view at source ↗
Figure 2
Figure 2. Figure 2: FIG. 2. Posteriors from the UVLF fit. The contours show the view at source ↗
Figure 4
Figure 4. Figure 4: FIG. 4. Posteriors the reionization fit for view at source ↗
Figure 3
Figure 3. Figure 3: FIG. 3. Reionisation histories varying the PMF strength view at source ↗
Figure 5
Figure 5. Figure 5: FIG. 5. Same as Fig view at source ↗
read the original abstract

Primordial magnetic fields (PMFs) enhance small-scale structure formation through the Lorentz force acting on baryons, boosting the abundance of low-mass halos and their hosted galaxies. We show that the reionisation history calibrated with the UV luminosity function (UVLF) provides stringent bounds: strong PMFs induce a characteristic double reionisation at $z \approx 24$ that is incompatible with CMB measurements of the optical depth, yielding $\sqrt{\left\langle B^2 \right\rangle} < 0.27\,{\rm nG}$ and $< 0.18\,{\rm nG}$ for $n_B = -2$ and $n_B = 2$ respectively at $95\%\,{\rm CL}$ using Planck priors on $\tau$. This establishes early galaxy observables as among the most sensitive probes of PMFs in Gaussian, non-helical scenarios.

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.

Axiom & Free-Parameter Ledger

2 free parameters · 3 axioms · 0 invented entities

The claim rests on standard cosmological modeling of reionization and the Lorentz-force effect of PMFs on baryons; no new entities are postulated, but several domain assumptions are required.

free parameters (2)
  • n_B
    Magnetic field power spectrum index; fixed to discrete values -2 and 2 rather than fitted continuously.
  • B amplitude
    Field strength amplitude; the quantity being bounded rather than fitted, but its effect is modeled through halo abundance.
axioms (3)
  • domain assumption Standard Lambda-CDM cosmology governs structure formation and reionization
    Invoked throughout the modeling of halo abundance and reionization history.
  • domain assumption PMFs are Gaussian and non-helical
    Explicitly stated as the scenario under which the bounds apply.
  • domain assumption UV luminosity function from JWST accurately traces the reionization photon budget
    Used to calibrate the reionization history that is then compared to CMB τ.

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