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arxiv: 2606.25096 · v1 · pith:AUEN2HHLnew · submitted 2026-06-23 · 🌌 astro-ph.CO · astro-ph.GA

An SKA-Low RM Grid for constraining the origin of cosmic magnetism

Shane P. O'Sullivan , Franco Vazza , Ettore Carretti , Valentina Vacca , Francesca Loi This is my paper

Pith reviewed 2026-06-25 22:48 UTC · model grok-4.3

classification 🌌 astro-ph.CO astro-ph.GA
keywords SKA-Lowrotation measureFaraday rotationcosmic magnetismpolarized sourcesRM gridmetre-wavelength radio
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The pith

SKA-Low will produce more than 50,000 rotation measures at 0.05 rad/m² precision across 10,000 square degrees.

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

The paper models the counts of metre-wavelength polarized radio sources to forecast the rotation-measure grid that SKA-Low can deliver. The resulting density reaches at least an order of magnitude above existing grids, yielding over 50,000 RMs for a representative 10,000 deg² survey. These measurements carry enough precision and sky coverage to compare directly against cosmological magnetohydrodynamic simulations and thereby test competing pictures of how cosmic magnetic fields first arose and grew. The same data set can be partially validated already during early science verification observations.

Core claim

Modeling the polarized source counts as N(>P) ∼ 5 (P/100 μJy)^{-0.75} deg^{-2} shows that SKA-Low can generate the leading RM grid of the SKA era, delivering more than 50,000 RMs at ∼0.05 rad/m² precision for a 10,000 deg² survey in ∼3,200 hours and up to 100,000 RMs when wide-area and all-sky data are combined.

What carries the argument

The power-law extrapolation of metre-wavelength polarized source counts that sets the expected RM grid density at SKA-Low flux thresholds.

If this is right

  • At least tenfold increase in RM grid density relative to the current best metre-wavelength surveys.
  • Direct comparison of observed RMs with cosmological MHD simulations to constrain magnetic-field seeding and amplification mechanisms.
  • Up to 100,000 m-λ RMs detectable across the full observable sky when wide-area and all-sky data sets are merged.
  • Early verification possible with AA* data yielding ∼2.6 RMs per square degree at a 240 μJy threshold.

Where Pith is reading between the lines

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

  • A grid of this size and precision could separate primordial-seeding from astrophysical-amplification scenarios by mapping field strength on the largest cosmic scales.
  • Repeated observations over time could track the redshift evolution of magnetized structures in the circumgalactic and intergalactic media.
  • The same data would furnish a dense foreground screen for correcting Faraday rotation in future 21-cm intensity-mapping experiments.

Load-bearing premise

The adopted power-law form and normalization of polarized source counts continue to hold at the faint polarized intensities reached by SKA-Low.

What would settle it

A direct measurement of the surface density of polarized sources at 10–50 μJy that lies more than a factor of two away from the extrapolated power law.

Figures

Figures reproduced from arXiv: 2606.25096 by Ettore Carretti, Francesca Loi, Franco Vazza, Shane P. O'Sullivan, Valentina Vacca.

Figure 1
Figure 1. Figure 1: Left: Cumulative polarized-source number counts: updated T-RECS polarization (blue), LOFAR deep field polarized source counts from Piras et al. (2024) (red), LoTSS DR2 RM Grid counts (green), power￾law fit to model between 0.1 and 10 mJy (orange). Right: Euclidean-normalised source counts: T-RECS total intensity (grey points), LOFAR total intensity deep field counts from Mandal et al. (2021) (grey line), p… view at source ↗
Figure 2
Figure 2. Figure 2: Left panels: projected average dark matter overdensity along the line of sight, for a simulated integration up to 𝑧 = 0.1 (top) or up to 𝑧 = 2 (lower panel). Central and right panels: integrated RM up to 𝑧 = 0.1 or 𝑧 = 2, for our fiducial model comprising a primordial magnetic field model (𝑛𝐵 = −1 spectrum with 0.37 nG normalisation, Section 4.1) with an astrophysical seeding by galaxy processes (central p… view at source ↗
Figure 3
Figure 3. Figure 3: The RRM(𝑧) distribution from the LoTSS DR2 RM Grid, for 0 < 𝑧 < 1 (left) and 𝑧 > 1 (right). One can clearly see the sharp fall-off in the number of data points beyond 𝑧 = 1, which are crucial for constraining the origin of cosmic magnetism and the strength of primodial magnetic fields (Section 4). formation-related processes ( [PITH_FULL_IMAGE:figures/full_fig_p010_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Left: Observational data from the LoTSS DR2 RM Grid of |ΔRRM(Δ𝑧)| of non-physical pairs. A linear fit to the data gives a slope of ∼0.3, however the data remain consistent with a flat behaviour. The median |ΔRM(Δ𝑧)| are shown for six bins with equal numbers of sources per bin (57), with their bootstrap errors and the interquartile range (IQR). Right: Simulated |ΔRRM(Δ𝑧)| for the baseline (primordial+astrop… view at source ↗
read the original abstract

Understanding the origin and evolution of cosmic magnetic fields is a key science goal for the SKAO. Recent advances in metre-wavelength (m-$\lambda$) Faraday rotation measure (RM) grids are enabling precision probes of cosmic magnetism, with implications extending to early-Universe physics, AGN feedback, and the magnetized circumgalactic medium. Here we model the m-$\lambda$ polarized source counts to predict an RM Grid density with SKA-Low of $N(>P) \sim 5 ({P}/{100{\rm \mu Jy}})^{-0.75}\,\, {\rm deg}^{-2} $, where $P$ is the polarized intensity detection threshold. This represents at least an order of magnitude improvement over the current state-of-the-art. For a representative wide-area SKA-Low AA4 survey covering 10,000 deg$^2$ in $\sim$3,200 hours, we predict more than 50,000 RMs. Coupled with an expected RM precision of $\sim$0.05 rad/m$^2$, SKA-Low promises to produce the leading RM Grid survey for constraining the origin of cosmic magnetism in the SKA era. These predictions can be partially tested during the Science Verification phase using the AA* Sky Model data. For example, at a nominal detection threshold of 240~$\mu$Jy/beam (8 times the noise in Stokes $Q$ and $U$), we expect $\sim$2.6 RMs/deg$^2$ (5x the current best m-$\lambda$ RM Grid density). Combining both wide-area and all-sky data, SKA-Low could detect up to 100,000 m-$\lambda$ RMs across its observable sky. Finally, we demonstrate new constraints on the origin of cosmic magnetism by comparing cosmological MHD simulations with the LOFAR m-$\lambda$ RMs, and highlight the transformative advances an SKA-Low RM Grid will enable for precision studies of cosmic magnetism.

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 / 1 minor

Summary. The manuscript models meter-wavelength polarized source counts to predict an SKA-Low RM grid density of N(>P) ~ 5 (P/100 μJy)^{-0.75} deg^{-2}. For a 10,000 deg² AA4 survey it forecasts >50,000 RMs at ~0.05 rad/m² precision (an order-of-magnitude gain), illustrates partial tests with AA* data, and demonstrates current constraints on cosmic magnetism by comparing LOFAR RMs with cosmological MHD simulations.

Significance. If the source-count model holds, the predicted RM grid would materially advance precision studies of cosmic magnetism, enabling tighter constraints on early-Universe fields, AGN feedback, and the magnetized CGM. The LOFAR–MHD comparison already supplies a concrete, falsifiable demonstration of the method.

major comments (2)
  1. [Abstract] Abstract: the headline prediction (>50,000 RMs over 10,000 deg²) is obtained by integrating the quoted power-law N(>P) ~ 5 (P/100 μJy)^{-0.75} deg^{-2} down to the survey threshold. The functional form and normalization are stated to come from 'modeling' but the abstract (and, on the information supplied, the methods) supplies neither the input catalogs, fitting procedure, nor any cross-check against existing deep m-λ polarized catalogs at P ≲ 100 μJy. Without these, the integrated density and the 'order of magnitude improvement' claim cannot be assessed.
  2. [Abstract] Abstract: no error bars, sensitivity tests, or alternative slope/normalization scenarios are reported for the source-count integral. A plausible flattening or change in normalization below current detection limits would shift the predicted RM count by a factor of several, directly affecting the central quantitative claim.
minor comments (1)
  1. [Abstract] The statement that predictions 'can be partially tested during the Science Verification phase using the AA* Sky Model data' is left at a high level; a short quantitative example (e.g., expected number of sources at the quoted 240 μJy threshold) would strengthen the claim.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their careful and constructive review. We address each major comment below and commit to revisions that will strengthen the presentation of the source-count model.

read point-by-point responses

  1. Referee: [Abstract] Abstract: the headline prediction (>50,000 RMs over 10,000 deg²) is obtained by integrating the quoted power-law N(>P) ~ 5 (P/100 μJy)^{-0.75} deg^{-2} down to the survey threshold. The functional form and normalization are stated to come from 'modeling' but the abstract (and, on the information supplied, the methods) supplies neither the input catalogs, fitting procedure, nor any cross-check against existing deep m-λ polarized catalogs at P ≲ 100 μJy. Without these, the integrated density and the 'order of magnitude improvement' claim cannot be assessed.

    Authors: We agree that the abstract is too concise and that the methods section would benefit from greater explicitness on this point. In revision we will (i) expand the abstract to state the principal input catalogs and the fitting approach used to obtain the quoted power-law parameters, (ii) add a short methods subsection that tabulates the catalogs, describes the fitting procedure, and reports the cross-checks performed against existing deep m-λ polarized fields, and (iii) note that the AA* Sky Model data provide a partial validation at 240 μJy. These changes will allow readers to assess the integrated density and the order-of-magnitude claim directly. revision: yes

  2. Referee: [Abstract] Abstract: no error bars, sensitivity tests, or alternative slope/normalization scenarios are reported for the source-count integral. A plausible flattening or change in normalization below current detection limits would shift the predicted RM count by a factor of several, directly affecting the central quantitative claim.

    Authors: We accept this criticism. The revised manuscript will include (i) formal uncertainties on the fitted slope and normalization propagated through the integral, (ii) a sensitivity analysis showing the range of predicted RM counts when the slope is varied by ±0.1 and the normalization by ±30 %, and (iii) an explicit discussion of the possible impact of a flattening below ~100 μJy. These results will be added both to the abstract (as a parenthetical range) and to a new paragraph in the main text. revision: yes

Circularity Check

0 steps flagged

No significant circularity in the derivation chain

full rationale

The paper states it models the m-λ polarized source counts to obtain the density formula N(>P) ~ 5 (P/100 μJy)^{-0.75} deg^{-2} and then integrates that model to forecast RM counts for SKA-Low. This is a forward-model prediction rather than a fitted parameter or self-referential definition. No load-bearing self-citations, uniqueness theorems, or reductions of the headline prediction (>50,000 RMs) to the input data by construction appear in the abstract or quoted sections. The extrapolation assumption is an external modeling choice, not a circular step.

Axiom & Free-Parameter Ledger

2 free parameters · 1 axioms · 0 invented entities

The forecasts rest on an empirical power-law model of polarized source counts whose parameters are not derived from first principles in the abstract; no new physical entities are introduced.

free parameters (2)
  • normalization constant 5
    Sets the overall scale of the source count power law; appears chosen to match current m-λ data.
  • power-law index -0.75
    Determines how steeply counts rise at fainter fluxes; taken from the modeling.
axioms (1)
  • domain assumption Polarized source counts follow a single unbroken power law down to SKA-Low thresholds
    Invoked when extrapolating the quoted N(>P) formula to 100 μJy and below.

pith-pipeline@v0.9.1-grok · 5916 in / 1490 out tokens · 10695 ms · 2026-06-25T22:48:53.436835+00:00 · methodology

discussion (0)

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Reference graph

Works this paper leans on

90 extracted references · 9 linked inside Pith

  1. [1]

    T. M. C. Abbott et al. , 239 0 (2): 0 18, Dec. 2018. doi:10.3847/1538-4365/aae9f0

    doi:10.3847/1538-4365/aae9f0 2018

  2. [2]

    Abitbol et al

    M. Abitbol et al. , 2025 0 (8): 0 034, Aug. 2025. doi:10.1088/1475-7516/2025/08/034

    doi:10.1088/1475-7516/2025/08/034 2025

  3. [3]

    Ade et al

    P. Ade et al. Journal of Cosmology and Astroparticle Physics, 2019 0 (2): 0 056, Feb. 2019. doi:10.1088/1475-7516/2019/02/056

    doi:10.1088/1475-7516/2019/02/056 2019

  4. [4]

    Agazie et al

    G. Agazie et al. The Astrophysical Journal Letters, 951 0 (1): 0 L8, June 2023. ISSN 2041-8205. doi:10.3847/2041-8213/acdac6. URL https://dx.doi.org/10.3847/2041-8213/acdac6. Publisher: The American Astronomical Society

    doi:10.3847/2041-8213/acdac6 2023

  5. [5]

    Alonso-L \'o pez et al

    D. Alonso-L \'o pez et al. , 705: 0 A143, Jan. 2026. doi:10.1051/0004-6361/202556287

    doi:10.1051/0004-6361/202556287 2026

  6. [6]

    Amaral, T

    A. Amaral, T. Vernstrom, and B. M. Gaensler. Monthly Notices of the Royal Astronomical Society, 503 0 (2): 0 2913, 2021. doi:10.1093/mnras/stab564. URL http://arxiv.org/abs/2102.11312v2. Publisher: Cornell University Library

    doi:10.1093/mnras/stab564 2021

  7. [7]

    C. S. Anderson et al. Monthly Notices of the Royal Astronomical Society, 533 0 (4): 0 4068--4080, Oct. 2024. doi:10.1093/mnras/stae1954

    doi:10.1093/mnras/stae1954 2024

  8. [8]

    Beck and B

    R. Beck and B. M. Gaensler . New Astron. Rev., 48: 0 1289--1304, Dec. 2004. doi:10.1016/j.newar.2004.09.013

    doi:10.1016/j.newar.2004.09.013 2004

  9. [9]

    P. N. Best et al. , 523 0 (2): 0 1729--1755, Aug. 2023. doi:10.1093/mnras/stad1308

    doi:10.1093/mnras/stad1308 2023

  10. [10]

    Blunier and A

    J. Blunier and A. Neronov. Astronomy and Astrophysics, 691: 0 A34, March 2024. doi:10.1051/0004-6361/202450138. URL http://arxiv.org/abs/2403.13418. arXiv: 2403.13418

    doi:10.1051/0004-6361/202450138 2024

  11. [11]

    B \"o ckmann et al

    K. B \"o ckmann et al. Astronomy and Astrophysics, 678: 0 A56, August 2023. doi:10.1051/0004-6361/202346777. URL http://arxiv.org/abs/2308.11391. arXiv: 2308.11391

    doi:10.1051/0004-6361/202346777 2023

  12. [12]

    Bonaldi et al

    A. Bonaldi et al. Monthly Notices of the Royal Astronomical Society, 482 0 (1): 0 2--19, January 2019. ISSN 0035-8711, 1365-2966. doi:10.1093/mnras/sty2603. URL http://arxiv.org/abs/1805.05222. arXiv:1805.05222 [astro-ph]

    Pith/arXiv arXiv doi:10.1093/mnras/sty2603 2019

  13. [13]

    Bonaldi et al

    A. Bonaldi et al. Monthly Notices of the Royal Astronomical Society, 524 0 (1): 0 993--1007, July 2023. ISSN 0035-8711, 1365-2966. doi:10.1093/mnras/stad1913. URL http://arxiv.org/abs/2305.10175. arXiv:2305.10175 [astro-ph]

    doi:10.1093/mnras/stad1913 2023

  14. [14]

    Bondarenko, A

    K. Bondarenko, A. Boyarsky, A. Sokolenko, and I. Vovk. arXiv e-prints, page arXiv:2404.17402, April 2024. doi:10.48550/arXiv.2404.17402. URL http://arxiv.org/abs/2404.17402. arXiv: 2404.17402

    doi:10.48550/arxiv.2404.17402 2024

  15. [15]

    Booth et al

    M. Booth et al. arXiv e-prints, art. arXiv:2407.01413, July 2024. doi:10.48550/arXiv.2407.01413

    doi:10.48550/arxiv.2407.01413 2024

  16. [16]

    Botteon et al

    A. Botteon et al. , 499 0 (1): 0 L11--L15, Dec. 2020. doi:10.1093/mnrasl/slaa142

    doi:10.1093/mnrasl/slaa142 2020

  17. [17]

    Brandenburg, O

    A. Brandenburg, O. Iarygina, E. I. Sfakianakis, and R. Sharma. Journal of Cosmology and Astroparticle Physics, 2024 0 (12): 0 057, August 2024. doi:10.1088/1475-7516/2024/12/057. URL https://doi.org/10.1088/1475-7516/2024/12/057. Publication Title: arXiv e-prints ADS Bibcode: 2024arXiv240817413B

    doi:10.1088/1475-7516/2024/12/057 2024

  18. [18]

    Carretti and F

    E. Carretti and F. Vazza . Universe, 11 0 (5): 0 164, May 2025. doi:10.3390/universe11050164

    doi:10.3390/universe11050164 2025

  19. [19]

    Carretti et al

    E. Carretti et al. Monthly Notices of the Royal Astronomical Society, 512 0 (1): 0 945, 2022. doi:10.1093/mnras/stac384. URL http://arxiv.org/abs/2202.04607v1. Publisher: Cornell University Library

    doi:10.1093/mnras/stac384 2022

  20. [21]

    Carretti et al

    E. Carretti et al. , 518 0 (2): 0 2273--2286, Jan. 2023. doi:10.1093/mnras/stac2966

    doi:10.1093/mnras/stac2966 2023

  21. [22]

    Carretti et al

    E. Carretti et al. Astronomy and Astrophysics, 693: 0 A208, Jan. 2025. doi:10.1051/0004-6361/202451333

    doi:10.1051/0004-6361/202451333 2025

  22. [23]

    Dietl et al

    J. Dietl et al. Astronomy and Astrophysics, 691: 0 A286, January 2024. doi:10.1051/0004-6361/202449354. URL http://arxiv.org/abs/2401.17281. arXiv: 2401.17281

    doi:10.1051/0004-6361/202449354 2024

  23. [24]

    , 662: 0 A112, June 2022

    Euclid Collaboration et al. , 662: 0 A112, June 2022. doi:10.1051/0004-6361/202141938

    doi:10.1051/0004-6361/202141938 2022

  24. [25]

    B. M. Gaensler et al. The polarisation sky survey of the universe's magnetism (possum): Science goals and survey description, May 2025. URL http://arxiv.org/abs/2505.08272. arXiv:2505.08272 [astro-ph]

    arXiv 2025

  25. [26]

    J. E. Geach et al. Nature, 621 0 (7979): 0 483--486, September 2023. ISSN 1476-4687. doi:10.1038/s41586-023-06346-4. URL https://www.nature.com/articles/s41586-023-06346-4. Publisher: Nature Publishing Group

    doi:10.1038/s41586-023-06346-4 2023

  26. [27]

    Y. A. Gordon et al. The Astrophysical Journal Supplement Series, 267 0 (2): 0 37, 2023. doi:10.3847/1538-4365/acda30. URL http://arxiv.org/abs/2303.12830v1. Publisher: Cornell University Library

    doi:10.3847/1538-4365/acda30 2023

  27. [28]

    Govoni et al

    F. Govoni et al. Science, 364 0 (6444): 0 981--984, June 2019. doi:10.1126/science.aat7500

    doi:10.1126/science.aat7500 2019

  28. [29]

    Gupta et al

    N. Gupta et al. Publications of the Astronomical Society of Australia, 41: 0 e027, March 2024. doi:10.1017/pasa.2024.25. URL http://arxiv.org/abs/2403.14235. arXiv: 2403.14235

    doi:10.1017/pasa.2024.25 2024

  29. [30]

    Hackstein et al

    S. Hackstein et al. Monthly Notices of the Royal Astronomical Society, 475 0 (2): 0 2519, 2018. doi:10.1093/mnras/stx3354. URL http://arxiv.org/abs/1710.01353v2. Publisher: Cornell University Library

    Pith/arXiv arXiv doi:10.1093/mnras/stx3354 2018

  30. [31]

    M. J. Hardcastle et al. Astronomy and Astrophysics, 678, October 2023. ISSN 14320746. doi:10.1051/0004-6361/202347333. arXiv: 2309.00102 Publisher: EDP Sciences

    doi:10.1051/0004-6361/202347333 2023

  31. [32]

    M. J. Hardcastle et al. , 539 0 (2): 0 1856--1878, May 2025. doi:10.1093/mnras/staf622

    doi:10.1093/mnras/staf622 2025

  32. [33]

    Heald et al

    G. Heald et al. Galaxies, 8 0 (3): 0 53, 2020. doi:10.3390/galaxies8030053. URL http://arxiv.org/abs/2006.03172v1. Publisher: Cornell University Library

    doi:10.3390/galaxies8030053 2020

  33. [34]

    Heesen et al

    V. Heesen et al. Astronomy & Astrophysics, 670: 0 L23, Feb. 2023. ISSN 0004-6361, 1432-0746. doi:10.1051/0004-6361/202346008. URL https://www.aanda.org/10.1051/0004-6361/202346008

    doi:10.1051/0004-6361/202346008 2023

  34. [35]

    Hoeft et al

    M. Hoeft et al. , 654: 0 A68, Oct. 2021. doi:10.1051/0004-6361/202039725

    doi:10.1051/0004-6361/202039725 2021

  35. [36]

    Hutschenreuter et al

    S. Hutschenreuter et al. Astronomy and Astrophysics, 657: 0 A43, 2022. doi:10.1051/0004-6361/202140486. URL http://arxiv.org/abs/2102.01709v1. Publisher: Cornell University Library

    doi:10.1051/0004-6361/202140486 2022

  36. [37]

    Ivezi \'c et al

    Z . Ivezi \'c et al. , 873 0 (2): 0 111, Mar. 2019. doi:10.3847/1538-4357/ab042c

    doi:10.3847/1538-4357/ab042c 2019

  37. [38]

    Jedamzik and L

    K. Jedamzik and L. Pogosian. Physical Review Letters, 125 0 (18): 0 181302, 2020. doi:10.1103/PhysRevLett.125.181302. URL http://arxiv.org/abs/2004.09487v2. Publisher: Cornell University Library

    doi:10.1103/physrevlett.125.181302 2020

  38. [39]

    Johnston-Hollitt et al

    M. Johnston-Hollitt et al. Advancing Astrophysics with the Square Kilometre Array (AASKA14), astro-ph.CO: 0 92, 2015. doi:10.22323/1.215.0092. URL http://arxiv.org/abs/1506.00808v1. Publisher: Cornell University Library

    Pith/arXiv arXiv doi:10.22323/1.215.0092 2015

  39. [40]

    J. P. Leahy. Monthly Notices of the Royal Astronomical Society, 226 0 (2): 0 433--446, 1987. doi:10.1093/mnras/226.2.433. URL https://doi.org/10.1093/mnras/226.2.433

    doi:10.1093/mnras/226.2.433 1987

  40. [41]

    Lin et al

    J. Lin et al. RAS Techniques and Instruments, 3 0 (1): 0 737--747, November 2024. doi:10.1093/rasti/rzae051. URL https://doi.org/10.1093/rasti/rzae051. Publication Title: arXiv e-prints ADS Bibcode: 2024arXiv241103931L

    doi:10.1093/rasti/rzae051 2024

  41. [42]

    Loi et al

    F. Loi et al. , 485 0 (4): 0 5285--5293, June 2019. doi:10.1093/mnras/stz350

    doi:10.1093/mnras/stz350 2019

  42. [43]

    Loi et al

    F. Loi et al. In Advancing Astrophysics with the SKA -- II (AASKAII). 2026. arXiv search: Report number AASKAII/Loi01

    2026

  43. [44]

    V. H. Mahatma et al. Monthly Notices of the Royal Astronomical Society, 502 0 (1): 0 273, 2021. doi:10.1093/mnras/staa3980. URL http://arxiv.org/abs/2012.11990v1. Publisher: Cornell University Library

    doi:10.1093/mnras/staa3980 2021

  44. [45]

    Mandal et al

    S. Mandal et al. Astronomy and Astrophysics, 648: 0 A5, April 2021. ISSN 0004-6361. doi:10.1051/0004-6361/202039998. URL https://ui.adsabs.harvard.edu/abs/2021A&A...648A...5M. ADS Bibcode: 2021A&A...648A...5M

    doi:10.1051/0004-6361/202039998 2021

  45. [46]

    M. Mevius . RMextract: Ionospheric Faraday Rotation calculator . Astrophysics Source Code Library, record ascl:1806.024, June 2018

    2018

  46. [47]

    Migkas, F

    K. Migkas, F. Pacaud, T. Tuominen, and N. Aghanim. Astronomy & Astrophysics, 698: 0 A270, June 2025. ISSN 0004-6361, 1432-0746. doi:10.1051/0004-6361/202554944. URL https://www.aanda.org/10.1051/0004-6361/202554944

    doi:10.1051/0004-6361/202554944 2025

  47. [49]

    Mtchedlidze et al

    S. Mtchedlidze et al. The Astrophysical Journal, 977 0 (1): 0 128, June 2024. doi:10.3847/1538-4357/ad8dc5. URL http://arxiv.org/abs/2406.16230. arXiv: 2406.16230

    doi:10.3847/1538-4357/ad8dc5 2024

  48. [50]

    F. Naokawa. Universal profile for cosmic birefringence tomography with radio galaxies, April 2025. URL http://arxiv.org/abs/2504.06709. arXiv:2504.06709 [astro-ph]

    arXiv 2025

  49. [51]

    Neronov and I

    A. Neronov and I. Vovk. Science, 328 0 (5974): 0 73, 2010. doi:10.1126/science.1184192. URL http://arxiv.org/abs/1006.3504v1. Publisher: Cornell University Library

    Pith/arXiv arXiv doi:10.1126/science.1184192 2010

  50. [52]

    Neronov, A

    A. Neronov, A. R. Pol, C. Caprini, and D. Semikoz. Physical Review D, 103 0 (4), February 2021. ISSN 24700029. doi:10.1103/PhysRevD.103.L041302. Publisher: American Physical Society

    doi:10.1103/physrevd.103.l041302 2021

  51. [53]

    Neronov, F

    A. Neronov, F. Vazza, S. Mtchedlidze, and E. Carretti. Revision of upper bound on volume-filling intergalactic magnetic fields with lofar, December 2024. URL http://arxiv.org/abs/2412.14825. arXiv:2412.14825 [astro-ph]

    arXiv 2024

  52. [54]

    Oppermann et al

    N. Oppermann et al. Astronomy and Astrophysics, 575: 0 1--25, March 2015. ISSN 14320746. doi:10.1051/0004-6361/201423995. arXiv: 1404.3701 Publisher: EDP Sciences

    Pith/arXiv arXiv doi:10.1051/0004-6361/201423995 2015

  53. [55]

    S. P. O'Sullivan et al. Monthly Notices of the Royal Astronomical Society, 475 0 (3): 0 4263--4277, April 2018. ISSN 13652966. doi:10.1093/MNRAS/STY171. arXiv: 1801.02452 Publisher: Oxford University Press

    Pith/arXiv arXiv doi:10.1093/mnras/sty171 2018

  54. [57]

    S. P. O'Sullivan et al. , 495 0 (3): 0 2607--2619, May 2020. doi:10.1093/mnras/staa1395

    doi:10.1093/mnras/staa1395 2020

  55. [58]

    S. P. O'Sullivan et al. Monthly Notices of the Royal Astronomical Society, 519 0 (4): 0 5723--5742, 2023. doi:10.1093/mnras/stac3820. URL https://doi.org/10.1093/mnras/stac3820. arXiv: 2301.07697v1

    doi:10.1093/mnras/stac3820 2023

  56. [59]

    Paoletti and F

    D. Paoletti and F. Finelli . JCAP, 2019 0 (11): 0 028, Nov. 2019. doi:10.1088/1475-7516/2019/11/028

    doi:10.1088/1475-7516/2019/11/028 2019

  57. [60]

    Pavi c evi \'c et al

    M. Pavi c evi \'c et al. Physical Review Letters, January 2025. doi:10.1103/77rd-vkpz. URL https://doi.org/10.1103/77rd-vkpz. Publication Title: arXiv e-prints ADS Bibcode: 2025arXiv250106299P

    doi:10.1103/77rd-vkpz 2025

  58. [61]

    Pell \'o et al

    R. Pell \'o et al. In J. J. Bryant, K. Motohara, and J. R. D. Vernet, editors, Ground-based and Airborne Instrumentation for Astronomy X, volume 13096, page 1309615. International Society for Optics and Photonics, SPIE, 2024. doi:10.1117/12.3019047. URL https://doi.org/10.1117/12.3019047

    doi:10.1117/12.3019047 2024

  59. [62]

    G. V. Pignataro et al. Astronomy & Astrophysics, 682: 0 A105, February 2024. ISSN 0004-6361, 1432-0746. doi:10.1051/0004-6361/202346243. URL https://www.aanda.org/10.1051/0004-6361/202346243

    doi:10.1051/0004-6361/202346243 2024

  60. [63]

    G. V. Pignataro et al. Detection of magnetic fields in superclusters of galaxies, March 2025. URL http://arxiv.org/abs/2503.08765. arXiv:2503.08765 [astro-ph]

    arXiv 2025

  61. [64]

    Piras et al

    S. Piras et al. Astronomy and Astrophysics, 687: 0 A267, June 2024. doi:10.1051/0004-6361/202349085. URL http://arxiv.org/abs/2406.08346. arXiv: 2406.08346

    doi:10.1051/0004-6361/202349085 2024

  62. [65]

    , 594: 0 A19, Sept

    Planck Collaboration et al. , 594: 0 A19, Sept. 2016. doi:10.1051/0004-6361/201525821

    doi:10.1051/0004-6361/201525821 2016

  63. [66]

    V. P. Pomakov et al. Monthly Notices of the Royal Astronomical Society, 515 0 (1): 0 256--270, September 2022. ISSN 13652966. doi:10.1093/mnras/stac1805. arXiv: 2208.01336 Publisher: Oxford University Press

    doi:10.1093/mnras/stac1805 2022

  64. [67]

    Ramesh, D

    R. Ramesh, D. Nelson, V. Heesen, and M. Br \"u ggen. Monthly Notices of the Royal Astronomical Society, 526 0 (4): 0 5483, May 2023. doi:10.1093/mnras/stad3104. URL http://arxiv.org/abs/2305.11214. arXiv: 2305.11214

    doi:10.1093/mnras/stad3104 2023

  65. [68]

    C. J. Riseley et al. Publications of the Astronomical Society of Australia, 37: 0 e029, 2020. doi:10.1017/pasa.2020.20. URL http://arxiv.org/abs/2005.09266v1. Publisher: Cornell University Library

    doi:10.1017/pasa.2020.20 2020

  66. [69]

    Sanati et al

    M. Sanati et al. Astronomy and Astrophysics, 690: 0 A59, October 2024. ISSN 0004-6361. doi:10.1051/0004-6361/202449822. URL https://ui.adsabs.harvard.edu/abs/2024A&A...690A..59S. Publisher: EDP ADS Bibcode: 2024A&A...690A..59S

    doi:10.1051/0004-6361/202449822 2024

  67. [70]

    D. H. Schnitzeler. Monthly Notices of the Royal Astronomical Society: Letters, 409 0 (1), November 2010. ISSN 17453933. doi:10.1111/j.1745-3933.2010.00957.x

    doi:10.1111/j.1745-3933.2010.00957.x 2010

  68. [71]

    Sobey et al

    C. Sobey et al. , 661: 0 A87, May 2022. doi:10.1051/0004-6361/202142636

    doi:10.1051/0004-6361/202142636 2022

  69. [72]

    J. M. Stil, M. Krause, R. Beck, and A. R. Taylor. The Astrophysical Journal, 693 0 (2): 0 1392, 2009. doi:10.1088/0004-637X/693/2/1392. URL http://arxiv.org/abs/0810.2303v1

    Pith/arXiv arXiv doi:10.1088/0004-637x/693/2/1392 2009

  70. [73]

    J. M. Stil , A. R. Taylor , and C. Sunstrum . ApJ, 726: 0 4, Jan. 2011. doi:10.1088/0004-637X/726/1/4

    doi:10.1088/0004-637x/726/1/4 2011

  71. [74]

    Stuardi et al

    C. Stuardi et al. Astronomy and Astrophysics, 638: 0 A48, 2020. doi:10.1051/0004-6361/202037635. URL http://arxiv.org/abs/2004.05169v1. Publisher: Cornell University Library

    doi:10.1051/0004-6361/202037635 2020

  72. [75]

    Tanimura et al

    H. Tanimura et al. Astronomy and Astrophysics, 637: 0 A41, 2020 a . doi:10.1051/0004-6361/201937158. URL http://arxiv.org/abs/1911.09706v1. Publisher: Cornell University Library

    doi:10.1051/0004-6361/201937158 2020

  73. [76]

    Tanimura et al

    H. Tanimura et al. Astronomy and Astrophysics, 643, November 2020 b . ISSN 14320746. doi:10.1051/0004-6361/202038521. arXiv: 2011.05343 Publisher: EDP Sciences

    doi:10.1051/0004-6361/202038521 2020

  74. [77]

    A. R. Taylor, J. M. Stil, and C. Sunstrum. Astrophysical Journal, 702 0 (2): 0 1230--1236, 2009. ISSN 15384357. doi:10.1088/0004-637X/702/2/1230. Publisher: Institute of Physics Publishing

    doi:10.1088/0004-637x/702/2/1230 2009

  75. [78]

    Unger and G

    M. Unger and G. R. Farrar . , 970 0 (1): 0 95, July 2024. doi:10.3847/1538-4357/ad4a54

    doi:10.3847/1538-4357/ad4a54 2024

  76. [79]

    Vacca et al

    V. Vacca et al. , 691: 0 A334, Nov. 2024. doi:10.1051/0004-6361/202349095

    doi:10.1051/0004-6361/202349095 2024

  77. [80]

    Vacca et al

    V. Vacca et al. In Advancing Astrophysics with the SKA -- II (AASKAII). 2026. arXiv search: Report number AASKAII/Vacca02

    2026

  78. [81]

    C. L. Van Eck et al. Astronomy and Astrophysics, 613, May 2018. ISSN 14320746. doi:10.1051/0004-6361/201732228. arXiv: 1801.04467 Publisher: EDP Sciences

    Pith/arXiv arXiv doi:10.1051/0004-6361/201732228 2018

  79. [82]

    C. L. Van Eck et al. The Astrophysical Journal Supplement Series, 267 0 (2): 0 28, May 2023. doi:10.3847/1538-4365/acda24. URL http://arxiv.org/abs/2305.16607. arXiv: 2305.16607

    doi:10.3847/1538-4365/acda24 2023

  80. [83]

    R. J. van Weeren et al. , 215 0 (1): 0 16, Feb. 2019. doi:10.1007/s11214-019-0584-z

    doi:10.1007/s11214-019-0584-z 2019

Showing first 80 references.