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arxiv: 2605.16924 · v1 · pith:7CE6SBY5new · submitted 2026-05-16 · 🌌 astro-ph.GA · astro-ph.CO

Magnetised CGM Gas at z~1 revealed by SPICE-RACS

Sunil Malik , S. P. O'Sullivan , A. J. M. Thomson , C. S. Anderson , C. Van Eck , L. Rudnick , Amit Seta , B. M. Gaensler
show 12 more authors
Y. K. Ma Takuya Akahori D. Alonso-L\'opez M. Br\"uggen E. Carretti S. W. Duchesne T. J. Galvin G. Heald O. Hlinka A. Khadir S. A. Mao R. Omae
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Pith reviewed 2026-05-19 20:53 UTC · model grok-4.3

classification 🌌 astro-ph.GA astro-ph.CO
keywords Faraday rotation measureMg II absorberscircumgalactic mediummagnetic fieldshigh-redshift galaxiesSPICE-RACSDESI
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The pith

Quasar sightlines through Mg II absorbers at z~1 show excess Faraday rotation dispersion indicating magnetized circumgalactic gas.

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

The study compares rotation measures from thousands of quasars, splitting the sample into those with intervening Mg II absorbers tracing foreground galaxies and a control set without absorbers. After subtracting the Milky Way contribution and restricting to low-contamination sightlines, the absorber group displays a clear excess in the scatter of the remaining rotation measures. This excess reaches 4.13 rad m^{-2} at 4.5 sigma significance for a median absorber redshift near 1.14. The signal corresponds to model-dependent magnetic field strengths of 0.4 to 0.8 microgauss spanning projected distances of 20 to 150 kiloparsecs. The result shows that substantial magnetization of galaxy halos was already in place by redshift 1.

Core claim

In this foreground-cleaned sample, Mg II sightlines exhibit a 4.5σ excess in the residual RM dispersion of 4.13 ± 0.91 rad m^{-2} relative to the control sample, at a median absorber redshift of z∼1.14. This implies model-dependent CGM magnetic field strengths of ∼0.4 - 0.8 μG over projected radii of 20 - 150 kpc. This indicates that substantial CGM magnetisation was already established by z∼1.

What carries the argument

Excess residual Faraday rotation measure dispersion between Mg II absorber sightlines and control sightlines after Galactic subtraction and Milky Way HI/Hα cuts.

If this is right

  • Substantial magnetic fields of 0.4-0.8 microgauss already exist in the CGM at redshifts around 1.
  • Magnetic field amplification in galaxy halos must occur early enough to reach these strengths by z~1.
  • Projected radii of 20-150 kpc are magnetized, providing a new benchmark for halo field models.
  • Future RM surveys can track the redshift evolution of CGM magnetization directly.

Where Pith is reading between the lines

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

  • Extending the same RM comparison to higher-redshift absorbers would test when CGM magnetization first appears.
  • Matching the RM excess against galaxy simulations could distinguish between seeding and dynamo amplification mechanisms.
  • Applying the method to other absorber species might reveal whether magnetization depends on galaxy mass or environment.

Load-bearing premise

The measured excess in residual RM dispersion is produced by magnetized gas in the circumgalactic medium of the foreground galaxies rather than by residual contamination or selection effects.

What would settle it

A larger or cleaner sample in which Mg II absorber sightlines show no excess residual RM dispersion relative to matched controls would falsify the CGM magnetization claim.

Figures

Figures reproduced from arXiv: 2605.16924 by A. J. M. Thomson, A. Khadir, Amit Seta, B. M. Gaensler, C. S. Anderson, C. Van Eck, D. Alonso-L\'opez, E. Carretti, G. Heald, L. Rudnick, M. Br\"uggen, O. Hlinka, R. Omae, S. A. Mao, S. P. O'Sullivan, Sunil Malik, S. W. Duchesne, Takuya Akahori, T. J. Galvin, Y. K. Ma.

Figure 1
Figure 1. Figure 1: All-sky map of the Galactic neutral hydrogen (Hi) col￾umn density from the HI4PI survey, overlaid with the clean RRM sample (757 sources). Positive and negative RRMs are shown with red and blue circles, respectively, with the circle size proportional to |RRM|. Sky coverage of the sources is limited in declination by the SPICE-RACS upper limit of ∼ +49◦ and the lower limit of −18◦ is from DESI. In addition,… view at source ↗
Figure 2
Figure 2. Figure 2: CDF of |RRM| for the subsamples with and without foreground Mg ii absorbers. 3. Results 3.1. RRM Excess in Mg ii absorbers To demonstrate the statistical difference between the RRM distributions of the subsamples with and without Mg ii ab￾sorbers, we plot the cumulative distribution function (CDF) of |RRM| in [PITH_FULL_IMAGE:figures/full_fig_p003_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Map of the RRM excess for various cutoff limits of Hi column density and Hα intensities to illustrate the varia￾tion of σExcess. We retain excess values when both subsamples (with and without Mg II absorbers) contain a minimum of 100 sightlines. The vertical green and horizontal blue lines mark the thresholds Hi = 3.5 × 1020 cm−2 and Hα = 1.0 R, respectively, adopted to compute the values reported in the t… view at source ↗
read the original abstract

Magnetic fields are expected to permeate the circumgalactic medium (CGM) of galaxies, yet direct constraints at high redshift remain limited by the lack of high-quality Faraday rotation measure (RM) data. Using the RMs from SPICE-RACS DR2 combined with the DESI DR1 quasar catalogue, we compile the largest sample to date of 2483 quasar sightlines with associated RMs, including 612 with intervening Mg II absorbers tracing foreground galaxies and 1871 control sightlines without Mg II absorbers. After subtracting the Galactic RM contribution and restricting the analysis to sightlines with low Milky Way HI column density and H$\alpha$ intensity, we obtain a foreground-cleaned sample of 757 quasars (191 Mg II / 566 control) spanning redshifts $0.13<z<3.45$. In this foreground-cleaned sample, Mg II sightlines exhibit a $4.5\sigma$ excess in the residual RM dispersion of $4.13 \pm 0.91~\mathrm{rad\,m^{-2}}$ relative to the control sample, at a median absorber redshift of $z\sim1.14$. This implies model-dependent CGM magnetic field strengths of $\sim0.4 - 0.8\, \mu$G over projected radii of $20 - 150$ kpc. This indicates that substantial CGM magnetisation was already established by $z\sim1$, enabling new constraints on the growth and amplification of magnetic fields in galaxy halos over cosmic time.

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 / 3 minor

Summary. The manuscript reports a 4.5σ excess in residual Faraday rotation measure (RM) dispersion of 4.13 ± 0.91 rad m^{-2} for 191 quasar sightlines with intervening Mg II absorbers (median z ∼ 1.14) relative to 566 control sightlines in a foreground-cleaned sample of 757 quasars drawn from SPICE-RACS DR2 and DESI DR1. After Galactic RM subtraction and cuts on low Milky Way HI column density and Hα intensity, this excess is interpreted as arising from magnetized circumgalactic medium (CGM) gas, implying model-dependent magnetic field strengths of ∼0.4–0.8 μG over projected radii of 20–150 kpc and indicating substantial CGM magnetisation already in place by z ∼ 1.

Significance. If robust, the result would offer one of the largest-sample constraints to date on CGM magnetic fields at intermediate redshift using a direct statistical comparison of RM dispersions. The compilation of 2483 sightlines from public catalogs is a clear strength that enables the reported excess to be measured with quoted significance. The model dependence of the B-field conversion is appropriately flagged in the abstract, so the primary advance is the detection of the residual dispersion difference rather than a model-independent field measurement.

major comments (2)
  1. [§3] §3 (foreground subtraction and sample cleaning): The Galactic RM subtraction procedure together with the specific thresholds applied for Milky Way HI column density and Hα intensity cuts are described, but no quantitative robustness tests (e.g., results with alternative RM foreground maps or varying cut values) or explicit error propagation details for the residual dispersion are provided. Because the central 4.5σ excess claim rests on these steps fully removing non-CGM contributions, such tests are required to demonstrate that the 4.13 ± 0.91 rad m^{-2} difference cannot be produced by residual Galactic or other foreground variance.
  2. [§4] §4 (statistical comparison): The foreground-cleaned Mg II (191) and control (566) subsamples are stated to span 0.13 < z < 3.45, yet no table or figure directly compares their redshift distributions, impact-parameter sampling, or quasar intrinsic properties, nor reports a statistical test (e.g., KS p-value) confirming they are drawn from the same parent population. Any mismatch in these observables would undermine the attribution of the excess specifically to magnetized gas at the absorber redshifts rather than selection effects.
minor comments (3)
  1. [Abstract] Abstract: The quoted significance and excess value are clear, but a one-sentence reference to the exact cuts or the section containing the foreground-cleaning details would improve immediate context for readers.
  2. [Discussion] Discussion: The range of CGM B-field strengths (0.4–0.8 μG) is presented as model-dependent; adding a short paragraph or table showing how the conversion varies with the assumed electron density and path length would make the model assumptions more transparent.
  3. Notation: Ensure consistent use of “residual RM dispersion” versus “RM dispersion” throughout; a brief definition in the methods would eliminate any ambiguity for readers unfamiliar with the exact subtraction steps.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive and positive assessment of our manuscript. We appreciate the recognition that our work provides one of the largest-sample constraints on CGM magnetic fields at intermediate redshift. We address each major comment point by point below, agreeing where additional material is needed to strengthen the robustness of the analysis and outlining the specific revisions we will make.

read point-by-point responses

  1. Referee: [§3] §3 (foreground subtraction and sample cleaning): The Galactic RM subtraction procedure together with the specific thresholds applied for Milky Way HI column density and Hα intensity cuts are described, but no quantitative robustness tests (e.g., results with alternative RM foreground maps or varying cut values) or explicit error propagation details for the residual dispersion are provided. Because the central 4.5σ excess claim rests on these steps fully removing non-CGM contributions, such tests are required to demonstrate that the 4.13 ± 0.91 rad m^{-2} difference cannot be produced by residual Galactic or other foreground variance.

    Authors: We agree that quantitative robustness tests are essential to support the claim that the observed excess arises from the CGM rather than residual foregrounds. In the revised manuscript we will add a dedicated subsection (or appendix) presenting the following tests: (i) repetition of the full analysis using an independent Galactic RM map (e.g., Oppermann et al. 2015), (ii) variation of the Milky Way HI column-density and Hα intensity thresholds by ±20 % around the adopted values, and (iii) explicit propagation of uncertainties from the Galactic RM subtraction into the final residual dispersion error budget. These additions will directly address the referee’s concern and demonstrate that the 4.13 ± 0.91 rad m^{-2} excess remains statistically significant under reasonable variations of the foreground-cleaning procedure. revision: yes

  2. Referee: [§4] §4 (statistical comparison): The foreground-cleaned Mg II (191) and control (566) subsamples are stated to span 0.13 < z < 3.45, yet no table or figure directly compares their redshift distributions, impact-parameter sampling, or quasar intrinsic properties, nor reports a statistical test (e.g., KS p-value) confirming they are drawn from the same parent population. Any mismatch in these observables would undermine the attribution of the excess specifically to magnetized gas at the absorber redshifts rather than selection effects.

    Authors: We acknowledge that a direct statistical comparison of the two subsamples is required to exclude selection biases. In the revised manuscript we will insert a new figure that overlays the redshift, projected impact-parameter, and quasar-magnitude distributions for the Mg II and control samples. We will also report two-sample Kolmogorov-Smirnov p-values for each distribution, confirming that the samples are statistically consistent with being drawn from the same parent population. These additions will be placed in Section 4 and will strengthen the attribution of the excess RM dispersion to the intervening Mg II systems. revision: yes

Circularity Check

0 steps flagged

No significant circularity; central result is direct data comparison

full rationale

The paper performs an observational comparison of residual RM dispersion between Mg II absorber sightlines and a control sample after applying standard Galactic RM subtraction plus cuts on Milky Way HI column density and Hα intensity. The reported 4.5σ excess of 4.13 ± 0.91 rad m^{-2} is obtained by direct statistical differencing of the two subsamples in the foreground-cleaned data; it is not fitted to, defined in terms of, or predicted from the target CGM B-field value. The subsequent inference of model-dependent B-field strengths (∼0.4–0.8 μG) is a post-hoc interpretation using external scaling relations, not a closed loop that re-derives the input dispersion. No self-definitional steps, fitted-input predictions, or load-bearing self-citations appear in the derivation chain. The analysis is self-contained against external public catalogs and benchmarks.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

The central claim rests on the validity of the foreground-cleaning procedure and the physical model that converts observed RM dispersion into a CGM magnetic field strength; these steps introduce model assumptions not independently verified in the abstract.

free parameters (1)
  • RM-to-B conversion model parameters
    The quoted 0.4-0.8 μG range is obtained by assuming specific electron density and path-length values through the CGM; these are not measured in the paper but chosen from prior models.
axioms (1)
  • domain assumption Residual RM dispersion after Galactic subtraction originates from magnetized CGM gas associated with Mg II absorbers
    This interpretation is adopted once Milky Way contributions are removed and sightlines are restricted to low HI/Hα regions.

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