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REVIEW 2 major objections 7 minor 81 references

Unravelling Turbulence and Magnetic Fields in Galaxy Clusters with SKA and XRISM

T0 review · 2 major / 7 minor · reviewed 2026-07-08 · glm-5.2

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Pith's one-line read X-ray and radio together crack open cluster turbulence physics

desk verdict Solid framework chapter for the SKA science book; the XRISM-SKA synergy concept is real but the quantitative claims about η_acc are limited by the unconstrained turbulence scale L. read the letter →

arxiv 2607.06346 v1 pith:5KZZDVE7 submitted 2026-07-07 astro-ph.HE astro-ph.GA

Kohei Kurahara , Takuya Akahori , Amit Seta , Kosuke Nishiwaki , Kazuhiro Nakazawa , Yuki Omiya , Daisuke Ito , Kosei Sakai This is my paper · ORCID
classification astro-ph.HEastro-ph.GA
keywords galaxyclustersintraclustermediumturbulencemagneticfieldscosmicraysFaradayrotationmeasuresynchrotronemissionturbulentdynamo
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

This paper proposes that combining XRISM's X-ray measurements of turbulent gas velocities with SKA's radio measurements of magnetic fields and synchrotron emission will, for the first time, allow direct observational determination of two fundamental efficiencies in galaxy clusters: how efficiently turbulence amplifies magnetic fields (η_B) and how efficiently it accelerates cosmic-ray electrons (η_acc). The core argument rests on a set of equations showing that once four quantities are independently measured — gas density and turbulent velocity dispersion from X-rays, plus magnetic field strength from Faraday rotation measures and synchrotron luminosity from radio — both efficiencies are fully constrained. Neither facility alone can do this: radio observations alone cannot separate magnetic field strength from cosmic-ray electron density, and X-ray observations alone cannot probe non-thermal components. The paper demonstrates the framework using the Coma cluster, finding magnetic field amplification efficiency of roughly 10% and electron acceleration efficiency of roughly 0.003% for a characteristic turbulence scale of 20 kpc. The paper also reviews recent XRISM results on merger geometry and velocity structure functions in clusters like Coma, Abell 3667, and Centaurus, and surveys new radio structures discovered by SKA pathfinders including mega-halos, radio bridges, and head-tail galaxies, arguing that these phenomena are all manifestations of turbulence coupling to magnetic fields and particle acceleration.

What carries the argument

The load-bearing equations are (15) and (18). Equation (15) gives η_B = B²/(4πρσ_v²), requiring B from radio RM, ρ and σ_v from X-ray. Equation (18) gives η_acc as a function of synchrotron luminosity, gas density, turbulent velocity, magnetic field, and the characteristic turbulence scale L. The turbulence scale L enters linearly in η_acc and is the most uncertain parameter.

What would settle it

If dense RM grids from SKA and velocity dispersion maps from XRISM, applied to a well-observed cluster like Coma, fail to produce physically plausible (i.e., η_B < 1 and η_acc < 1) and mutually consistent efficiency values for any reasonable choice of L, the decomposition framework would be called into question.

Watch

Extended reading notes

Core claim

The central mechanism is a decomposition of the turbulent energy budget in the intracluster medium into two observationally accessible efficiencies. The turbulent energy density is U_turb = (1/2)ρσ_v², measured by XRISM. The magnetic field amplification efficiency η_B = B²/(4πρσ_v²) is then determined once B is independently measured from SKA rotation measure grids. The electron acceleration efficiency η_acc depends on the synchrotron luminosity L(ν), the emitting volume V, the same turbulent energy quantities, and linearly on the characteristic turbulence scale L. The paper shows that the degeneracy between B and cosmic-ray electron density n_CRe that has plagued radio-only analyses is打破 by

Load-bearing premise

The framework assumes the characteristic turbulence scale L is known or can be reasonably assumed, but L is among the most uncertain quantities in cluster physics: XRISM's narrow field of view cannot trace the full turbulent velocity field, and L enters the electron acceleration efficiency linearly, so a factor-of-ten error in L produces a factor-of-ten error in η_acc.

Editorial extensions

If this is right

  • If both η_B and η_acc can be measured across a sample of clusters at different merger stages, it becomes possible to test whether turbulent dynamo saturation at a few percent of turbulent kinetic energy — a prediction from MHD simulations — holds observationally.
  • The framework could resolve the long-standing question of whether radio halos originate from turbulent re-acceleration of electrons or from hadronic secondary production, since the two scenarios predict different relationships between η_acc and turbulent energy.
  • Spatially resolved maps of η_B and η_acc within individual clusters would reveal whether magnetic field amplification and particle acceleration are co-spatial or spatially offset, testing the assumption that a single turbulent cascade drives both processes.
  • The comparison of cooling and acceleration timescales (Figure 5) offers an independent constraint on the turbulence injection scale, potentially closing the loop on the L-dependence that limits the efficiency estimates.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • The linear dependence of η_acc on L means that even order-of-magnitude progress on all other measurements will not yield a precise efficiency unless L is independently constrained. The paper's own Figure 4 shows η_acc varying by two orders of magnitude across L = 2–200 kpc. This suggests the framework's practical power may be limited until wide-field X-ray velocity mapping (beyond XRISM's 3 arcmin
  • The emerging correlation between X-ray turbulent velocity and radio emission intensity mentioned in Section 4, if confirmed with a larger sample, could itself serve as an empirical calibrator for L, effectively using the radio–turbulence correlation to break the L-degeneracy from within the same dataset.
  • If the Coma cluster's velocity structure function genuinely deviates from Kolmogorov scaling (as suggested in Section 2.2), the standard turbulent cascade picture used to derive the efficiency equations may need modification, since those equations assume energy dissipation at rate ~σ_v³/L without accounting for non-Kolmogorov spectral slopes.
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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit.

Referee Report

2 major / 7 minor

Summary. This chapter proposes a research framework for combining XRISM X-ray velocity measurements of ICM turbulence with SKA radio observations (synchrotron emission and Faraday RM grids) to jointly constrain magnetic field amplification efficiency (eta_B) and cosmic-ray electron acceleration efficiency (eta_acc) in galaxy clusters. The core formalism (Eqs. 10–18) follows Botteon et al. (2022) and is standard. The paper provides a representative application to the Coma cluster (Figure 4) and discusses observational feasibility with SKA. The physics is correctly applied and the synergy motivation is well-argued. However, the headline claim of 'direct observational determination' of eta_acc is overstated because the characteristic turbulence scale L — on which eta_acc depends linearly (Eq. 18) — remains model-dependent, and the proposed method to constrain L (Section 4.3) is itself partially circular. These issues are addressable by toning claims and adding discussion, not by fundamental restructuring.

Significance. The paper identifies a genuine and timely observational synergy between XRISM and SKA, and the central equations (15) and (18) correctly show how joint X-ray plus radio data constrain eta_B and eta_acc. The eta_B derivation (Eq. 15) is genuinely parameter-free once B, rho, and sigma_v are measured. The feasibility calculations for SKA-Mid (Section 5, Table 1) are concrete and useful. The VSF formalism in Section 2.2, while simplified, is correctly presented with appropriate caveats. The paper would benefit from more precise framing of what is and is not 'directly determined,' but the overall framework is a legitimate contribution to the SKA science case.

major comments (2)
  1. §4.2, Eqs. (15) and (18), and abstract: The abstract states that the synergy 'will allow for the first direct, multi-wavelength comparison' and Section 4.2 states that 'all quantities entering Eqs. (15) and (18) can be constrained observationally,' enabling 'direct estimates of both eta_B and eta_acc.' While eta_B (Eq. 15) is indeed directly determined from observables (B, rho, sigma_v), eta_acc (Eq. 18) depends linearly on the characteristic turbulence scale L, which is not directly measured but assumed. Figure 4 demonstrates that varying L from 2 to 200 kpc shifts eta_acc by two orders of magnitude. The paper acknowledges this ('once L and V are assumed'), but the headline language of 'direct observational determination' is inconsistent with this sensitivity. Recommend revising the abstract and Section 4.2 to state that eta_B is directly constrained while eta_acc remains modeldependent
  2. §4.3: The proposed method for constraining L by comparing the electron cooling timescale t_cool to the turbulent re-acceleration timescale t_acc has a circularity issue. The re-acceleration timescale t_acc depends on L itself (through the eddy turnover time and the Mach number dependence in the re-acceleration model, e.g., Brunetti and Lazarian 2016). Thus one is solving for L from an equation that already contains L as input, mediated by model assumptions about turbulent energy coupling to particles. This should be acknowledged explicitly, and the claim that this comparison 'can potentially provide constraints on the characteristic turbulence scale' should be qualified as model-dependent rather than independent.
minor comments (7)
  1. §2.2: The VSF analysis neglects cosmic variance and systematic uncertainties, as the authors acknowledge. The velocity dispersions (350.5 and 228.9 km/s for alpha = -11/3 and -8) are compared to the observed ~200 km/s, but no error bars or confidence intervals are provided on the model curves in Figure 2. Adding even approximate uncertainties would clarify whether the steeper slope is genuinely preferred.
  2. Figure 2: The caption should state the source of the observed VSF data points (Coma cluster XRISM observations) and clarify whether the data are from Xrism Collaboration et al. (2025b).
  3. §2: The phrase 'some cluster' (regarding XRISM measurements of ~200 km/s turbulent width) is vague. Specify which cluster is being referenced.
  4. §4.2: The representative values for Coma (sigma_v = 217 km/s, n_e = 3.4e-3 cm^-3, 0.1 Jy at 144 MHz) should cite their sources explicitly, particularly the flux density estimate from LoTSS data.
  5. §5.1, Eq. (19): The spectral index convention should be clarified — the exponent (alpha - 1) in the (1+z) K-correction term assumes a specific sign convention for alpha. A brief note would help readers verify the calculation.
  6. References: Several references appear to be from 2025-2026 (e.g., Xrism Collaboration et al. 2025a,b; Vazza and Brunetti 2026). Confirm these are correctly cited and that publication details are final.
  7. §1.4: The statement 'collision time ~10 Gyr' for cosmic-ray protons should specify the assumed target density, as this value depends on the ICM density.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for a careful and constructive report. Both major comments are well-taken and will be addressed in the revised manuscript. The core issue — that η_B is directly determined from observables while η_acc retains a model-dependent sensitivity to the characteristic turbulence scale L — is a genuine limitation of the framework as currently framed, and we will revise the language accordingly. We also acknowledge the circularity concern in Section 4.3 and will qualify the relevant claims.

read point-by-point responses

  1. Referee: §4.2, Eqs. (15) and (18), and abstract: The headline language of 'direct observational determination' is inconsistent with the sensitivity of η_acc to the assumed turbulence scale L. Recommend revising the abstract and Section 4.2 to state that η_B is directly constrained while η_acc remains model-dependent.

    Authors: The referee is correct. Equation (15) shows that η_B is determined directly from observables (B from RM, ρ and σ_v from X-ray), with no free parameters. Equation (18), however, depends linearly on L, and Figure 4 demonstrates that varying L from 2 to 200 kpc shifts η_acc by two orders of magnitude. The current language in the abstract ('first direct, multi-wavelength comparison') and in Section 4.2 ('direct estimates of both η_B and η_acc') does not adequately distinguish between these two cases. We will revise the abstract to state that the synergy enables direct determination of η_B and model-dependent constraints on η_acc. In Section 4.2, we will replace 'direct estimates of both η_B and η_acc' with language that explicitly states η_B is directly constrained from observables, while η_acc depends on the assumed turbulence scale L and is therefore model-dependent. We will also add a sentence emphasizing the order-of-magnitude sensitivity illustrated in Figure 4. revision: yes

  2. Referee: §4.3: The proposed method for constraining L by comparing t_cool to t_acc has a circularity issue, since t_acc itself depends on L. The claim that this comparison 'can potentially provide constraints on the characteristic turbulence scale' should be qualified as model-dependent rather than independent.

    Authors: We agree with this assessment. The re-acceleration timescale t_acc in the Brunetti & Lazarian (2016) framework depends on the eddy turnover time, which is itself proportional to L/σ_v, and on the turbulent Mach number, which also involves L through the sound speed ratio. Thus, using the condition t_cool ≈ t_acc to solve for L is indeed circular in the strict sense: L appears on both sides of the equation, mediated by model assumptions about how turbulent energy couples to particles. We will revise Section 4.3 to acknowledge this circularity explicitly. Specifically, we will qualify the statement that the comparison 'can potentially provide constraints on the characteristic turbulence scale' by noting that this is not an independent measurement of L but rather a self-consistency check within the re-acceleration model: given the model framework, the observed spectral cutoff frequency and measured turbulent velocity together select a preferred L, but the result is contingent on the assumed form of the turbulent re-acceleration model. We will also add a brief discussion of this limitation alongside the existing caveat sentence ('These estimates rely on several physical assumptions and simplified treatments'). revision: yes

Circularity Check

0 steps flagged · score 1.0 of 10

No significant circularity: the framework is a forward-modeling proposal with externally measured inputs, not a derivation that reduces to its own outputs.

full rationale

The paper proposes a synergistic observational framework combining XRISM velocity dispersion measurements with SKA radio/RM data. The central equations (15) and (18) are straightforward algebraic definitions: η_B = B²/(4πρσ_v²) and η_acc = ξL(ν)(1+B²_CMB/B²)/(V · ½ρσ³_v/L). These are not derived from their own outputs — each input (ρ, σ_v from X-ray; B, L(ν) from radio; L, V, ξ assumed) is independently measured or assumed. The B ≈ 4.7 μG from Bonafede et al. (2010) is an external RM-based measurement, not a quantity the paper itself fits and then re-predicts. The §4.3 timescale comparison (t_cool vs t_acc) does involve L on both sides, but the paper explicitly flags this as a consistency check ('can potentially provide constraints'), not a first-principles derivation or a prediction. The paper is appropriately cautious throughout ('once L and V are assumed'; 'these estimates rely on several physical assumptions'). The concern about L being model-dependent is a correctness/uncertainty issue, not circularity: the paper does not claim to derive L from an equation that already contains L as a fitted input. No self-citation chain is load-bearing for the central framework — the key equations are attributed to Botteon et al. (2022), an independent external paper. The Seta et al. self-citations appear in supporting contexts (magnetic field structure functions, dynamo theory) and do not form a circular derivation chain. This is a proposal chapter, not a results paper claiming parameter-free predictions.

Assumptions & free parameters 5 free parameters · 4 assumptions · 0 invented entities

No new particles, forces, fields, or entities are postulated.

free parameters (5)
  • Turbulence injection scale ℓ_inj = 1 Mpc
    Assumed in §2.2 for Coma VSF modeling; not independently measured
  • Turbulence dissipation scale ℓ_dis = 1 kpc
    Assumed in §2.2 for Coma VSF modeling; not independently measured
  • Characteristic turbulence scale L = 2, 20, 200 kpc (illustrative)
    Free parameter in Eqs. (12) and (18); η_acc depends linearly on L
  • Spectral slope α = -11/3 and -8 (illustrative)
    Assumed in §2.2 VSF modeling; compared to observations
  • Line-of-sight emissivity scale L_z = 1 Mpc
    Gaussian window function parameter in §2.2, assumed for simplicity
assumptions (4)
  • domain assumption ICM turbulence follows a power-law cascade describable by P(k) ∝ k^(-α)
    Invoked throughout §1.2 and §2.2; standard in turbulence theory but unverified for ICM at all scales
  • domain assumption Magnetic field amplification saturates at a few percent of turbulent kinetic energy
    §1.3, citing Ryu et al. 2008 and Seta et al. 2020; simulation-based, not observationally confirmed
  • domain assumption Turbulent re-acceleration is the primary mechanism for radio halo formation
    §1.4; the paper frames its framework around this model, though alternatives (hadronic) are mentioned
  • standard math RM is proportional to ∫ n_e B_∥ dl
    Standard Faraday rotation physics; used in §4.1

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Cite this review

Pith. "Pith review of Unravelling Turbulence and Magnetic Fields in Galaxy Clusters with SKA and XRISM." pith.science (2026). https://pith.science/paper/5KZZDVE7

@misc{pith2026260706346,
  author       = {Pith},
  title        = {Pith review of: Unravelling Turbulence and Magnetic Fields in Galaxy Clusters with SKA and XRISM},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/5KZZDVE7}},
  note         = {Machine review of arXiv:2607.06346}
}
abstract

This chapter proposes a research framework to quantitatively investigate non-thermal components in the Intracluster Medium (ICM) of galaxy clusters, which are critical ingredients for governing energy transport, structure formation, and particle acceleration. Turbulence, primarily driven by cluster mergers, is the leading mechanism for re-accelerating cosmic ray electrons (forming radio halos) and amplifying magnetic fields (via the turbulent dynamo). Observational understanding of both the turbulence and magnetic fields is rapidly evolving: the high-resolution X-ray spectrometer XRISM is directly measuring the velocity properties of the thermal ICM, providing insights into the kinetic energy of turbulence. Concurrently, high-sensitivity low-frequency radio observations, including SKA pathfinders, are mapping non-thermal components and magnetic structures through diffuse synchrotron emission and high-density Faraday Rotation Measure (RM) grids. The synergy between XRISM and SKA offers a decisive paradigm shift. XRISM's velocity maps, with its high energy resolution (<7 eV FWHM), combined with SKA-Mid's capability to deliver high-resolution RM grids ($\sim 100$--$200~\rm deg^{-2}$) and high-dynamic-range imaging, will allow for the first direct, multi-wavelength comparison of the turbulent energy properties (from X-ray) and the magnetic field properties (from radio). This joint analysis will validate Magnetohydrodynamic (MHD) simulation predictions, clarify the process of turbulent energy cascade and decay, and ultimately lead to a comprehensive understanding of the co-evolution of turbulence, magnetic fields, and cosmic rays in the largest laboratories of the Universe.

Figures

Figures reproduced from arXiv: 2607.06346 by the authors.

Figure 1
Figure 1. Conceptual illustration of the time evolution of the turbulent velocity power spectrum driven by a galaxy cluster merger. The elapsed time is normalised by the eddy turnover time at the injection scale, 𝑡0. Turbulent energy is injected at large scales and cascades through an inertial range before reaching the dissipation scale, which marks the onset of the turnover of the spectrum. At smaller scales, the power decre… view at source ↗
Figure 2
Figure 2. Observed velocity structure function (VSF) of the Coma cluster (blue points) compared with model predictions derived from projected three-dimensional turbulent power spectra. The orange and green curves show models with spectral slopes of 𝛼 = −11/3 (Kolmogorov-like) and 𝛼 = −8, respectively, assuming ℓinj = 1 Mpc and ℓdis = 1 kpc. dissipation scales are 350.5 km s−1 for 𝛼 = −11/3 and 228.9 km s−1 for 𝛼 = −8. Since t… view at source ↗
Figure 3
Figure 3. Various newly discovered radio structures identified with SKA pathfinder observations. All color images show the high-resolution LOFAR LoTSS DR3 data, while the contours represent smoothed radio intensity distributions after subtraction of compact sources in the corresponding fields. Scale bars are shown in the upper-right corners of the panels. (Left) A megahalo in ZwCl 0634.1+4750. (Center) A radio bridge connecti… view at source ↗
Figures from the paper (2 more)
Figure 4
Figure 4. Figure 4: Estimated electron acceleration efficiency, 𝜂acc, and magnetic field amplification efficiency, 𝜂𝐵, as functions of the assumed magnetic field strength in the Coma cluster. The shaded region indicates the 1𝜎 confidence interval of the central magnetic-field strength est…
Figure 5
Figure 5. Figure 5: Comparison between the radiative cooling timescale of cosmic-ray electrons, 𝑡cool, and the turbulent acceleration timescale, 𝑡acc, for the Coma cluster. The shaded region indicates the 1𝜎 confidence interval of the central magnetic-field strength estimated by Bonafede …

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Reference graph

Works this paper leans on

81 extracted references · 81 canonical work pages

  1. [1]

    Residual Gas Motions in the Intracluster Medium and Bias in Hydrostatic Measurements of Mass Profiles of Clusters

    Residual Gas Motions in the Intracluster Medium and Bias in Hydrostatic Measurements of Mass Profiles of Clusters. , keywords =. doi:10.1088/0004-637X/705/2/1129 , archivePrefix =. 0903.4895 , primaryClass =

    work page Pith review arXiv doi:10.1088/0004-637x/705/2/1129

  2. [2]

    and Jones, T

    Turbulence and vorticity in Galaxy clusters generated by structure formation. , keywords =. doi:10.1093/mnras/stw2351 , archivePrefix =. 1609.03558 , primaryClass =

    work page Pith review arXiv doi:10.1093/mnras/stw2351

  3. [3]

    The Matryoshka Run. II. Time-dependent Turbulence Statistics, Stochastic Particle Acceleration, and Microphysics Impact in a Massive Galaxy Cluster. , keywords =. doi:10.1088/0004-637X/800/1/60 , archivePrefix =. 1409.3576 , primaryClass =

    work page Pith review arXiv doi:10.1088/0004-637x/800/1/60

  4. [4]

    Characteristic Lengths of Magnetic Field in Magnetohydrodynamic Turbulence

    Characteristic Lengths of Magnetic Field in Magnetohydrodynamic Turbulence. , keywords =. doi:10.1088/0004-637X/705/1/L90 , archivePrefix =. 0908.0610 , primaryClass =

    work page Pith review arXiv doi:10.1088/0004-637x/705/1/l90

  5. [5]

    , keywords =

    A comparison of cosmological codes: properties of thermal gas and shock waves in large-scale structures. , keywords =. doi:10.1111/j.1365-2966.2011.19546.x , archivePrefix =. 1106.2159 , primaryClass =

    work page doi:10.1111/j.1365-2966.2011.19546.x 2011

  6. [6]

    Toward a Theory of Interstellar Turbulence. II. Strong Alfvenic Turbulence. , keywords =. doi:10.1086/175121 , adsurl =

    work page doi:10.1086/175121

  7. [7]

    Resolved magnetic dynamo action in the simulated intracluster medium

    Resolved magnetic dynamo action in the simulated intracluster medium. , keywords =. doi:10.1093/mnras/stx2830 , archivePrefix =. 1711.02673 , primaryClass =

    work page Pith review arXiv doi:10.1093/mnras/stx2830

  8. [8]

    Vorticity, Shocks and Magnetic Fields in Subsonic, ICM-like Turbulence

    Vorticity, Shocks, and Magnetic Fields in Subsonic, ICM-like Turbulence. , keywords =. doi:10.1088/0004-637X/810/2/93 , archivePrefix =. 1507.08737 , primaryClass =

    work page Pith review arXiv doi:10.1088/0004-637x/810/2/93

Show all 81 references
  1. [9]

    , keywords =

    Turbulent heating in galaxy clusters brightest in X-rays. , keywords =. doi:10.1038/nature13830 , archivePrefix =. 1410.6485 , primaryClass =

    doi arXiv

  2. [10]

    , keywords =

    Shaken Snow Globes: Kinematic Tracers of the Multiphase Condensation Cascade in Massive Galaxies, Groups, and Clusters. , keywords =. doi:10.3847/1538-4357/aaaa1b , archivePrefix =. 1709.06564 , primaryClass =

    doi arXiv

  3. [11]

    , keywords =

    The intracluster magnetic field power spectrum in Abell 2255. , keywords =. doi:10.1051/0004-6361:20065964 , archivePrefix =. astro-ph/0608433 , primaryClass =

    doi arXiv

  4. [12]

    , keywords =

    Atomic data and spectral modeling constraints from high-resolution X-ray observations of the Perseus cluster with Hitomi. , keywords =. doi:10.1093/pasj/psx156 , archivePrefix =. 1712.05407 , primaryClass =

    doi arXiv

  5. [13]

    , keywords =

    XRISM Forecast for the Coma Cluster: Stormy, with a Steep Power Spectrum. , keywords =. doi:10.3847/2041-8213/add2f6 , archivePrefix =. 2504.20928 , primaryClass =

    doi arXiv

  6. [14]

    The Radio Galaxy Messier 87 , year = 1999, editor =

    Cluster Turbulence. The Radio Galaxy Messier 87 , year = 1999, editor =. doi:10.1007/BFb0106425 , adsurl =

    1999 doi

  7. [15]

    , keywords =

    Cosmic Rays and Radio Halos in Galaxy Clusters: New Constraints from Radio Observations. , keywords =. doi:10.1086/524037 , archivePrefix =. 0710.0801 , primaryClass =

    doi arXiv

  8. [16]

    , keywords =

    On the Connection between Turbulent Motions and Particle Acceleration in Galaxy Clusters. , keywords =. doi:10.3847/2041-8213/aa7c1a , archivePrefix =. 1705.02341 , primaryClass =

    doi arXiv

  9. [17]

    arXiv e-prints , keywords =

    On the interpretation of XRISM X-ray measurements of turbulence in the intracluster medium: a comparison with cosmological simulations. arXiv e-prints , keywords =. doi:10.48550/arXiv.2507.04727 , archivePrefix =. 2507.04727 , primaryClass =

    doi

  10. [18]

    , keywords =

    Cluster Magnetic Fields. , keywords =. doi:10.1146/annurev.astro.40.060401.093852 , archivePrefix =. astro-ph/0110655 , primaryClass =

    doi

  11. [19]

    International Journal of Modern Physics D , keywords =

    Cosmic Rays in Galaxy Clusters and Their Nonthermal Emission. International Journal of Modern Physics D , keywords =. doi:10.1142/S0218271814300079 , archivePrefix =. 1401.7519 , primaryClass =

    doi arXiv

  12. [20]

    , keywords =

    A New Radio-X-Ray Probe of Galaxy Cluster Magnetic Fields. , keywords =. doi:10.1086/318896 , archivePrefix =. astro-ph/0011281 , primaryClass =

    doi arXiv

  13. [21]

    , keywords =

    Rotation measures of radio sources in hot galaxy clusters. , keywords =. doi:10.1051/0004-6361/200913665 , archivePrefix =. 1007.5207 , primaryClass =

    doi arXiv

  14. [22]

    , keywords =

    Rotation measure and synchrotron emission signatures in simulations of magnetized galactic discs. , keywords =. doi:10.1093/mnras/stac516 , archivePrefix =. 2203.04336 , primaryClass =

    doi arXiv

  15. [23]

    , keywords =

    Faraday rotation measure synthesis. , keywords =. doi:10.1051/0004-6361:20052990 , archivePrefix =. astro-ph/0507349 , primaryClass =

    doi arXiv

  16. [24]

    , keywords =

    Introduction to Faraday tomography and its future prospects. , keywords =. doi:10.1093/pasj/psac111 , archivePrefix =. 2303.07741 , primaryClass =

    doi arXiv

  17. [25]

    , keywords =

    Probing the magnetized gas distribution in galaxy groups and the cosmic web with POSSUM Faraday rotation measures. , keywords =. doi:10.1093/mnras/stae1954 , archivePrefix =. 2407.20325 , primaryClass =

    doi arXiv

  18. [26]

    Journal of Plasma Physics , keywords =

    MHD turbulence: a biased review. Journal of Plasma Physics , keywords =. doi:10.1017/S0022377822000721 , archivePrefix =. 2010.00699 , primaryClass =

    2010 doi arXiv

  19. [27]

    , keywords =

    AHKASH: a new Hybrid particle-in-cell code for simulations of astrophysical collisionless plasma. , keywords =. doi:10.1093/mnras/stae2188 , archivePrefix =. 2409.12151 , primaryClass =

    doi arXiv

  20. [28]

    , keywords =

    The Coma cluster magnetic field from Faraday rotation measures. , keywords =. doi:10.1051/0004-6361/200913696 , archivePrefix =. 1002.0594 , primaryClass =

    doi arXiv

  21. [29]

    The intra-cluster magnetic field power spectrum

    Sardinia Radio Telescope observations of Abell 194. The intra-cluster magnetic field power spectrum. , keywords =. doi:10.1051/0004-6361/201630349 , archivePrefix =. 1703.08688 , primaryClass =

    doi arXiv

  22. [30]

    Nature Astronomy , keywords =

    Suppressed effective viscosity in the bulk intergalactic plasma. Nature Astronomy , keywords =. doi:10.1038/s41550-019-0794-z , archivePrefix =. 1906.06346 , primaryClass =

    1906 doi arXiv

  23. [31]

    , keywords =

    Thermodynamic perturbations in the X-ray halo of 33 clusters of galaxies observed with Chandra ACIS. , keywords =. doi:10.1051/0004-6361/201526925 , archivePrefix =. 1510.08445 , primaryClass =

    doi arXiv

  24. [32]

    , keywords =

    Magnetic fields in the multiphase interstellar medium of the Milky Way: turbulent kinetic and magnetic energy density relation. , keywords =. doi:10.1093/mnras/staf520 , archivePrefix =. 2503.23634 , primaryClass =

    doi arXiv

  25. [33]

    , keywords =

    Dissecting nonthermal emission in the complex multiple-merger galaxy cluster Abell 2744: Radio and X-ray analysis. , keywords =. doi:10.1051/0004-6361/202141060 , archivePrefix =. 2104.05690 , primaryClass =

    doi arXiv

  26. [34]

    , keywords =

    MeerKAT view of the diffuse radio sources in Abell 3667 and their interactions with the thermal plasma. , keywords =. doi:10.1051/0004-6361/202142658 , archivePrefix =. 2111.06940 , primaryClass =

    doi arXiv

  27. [35]

    , keywords =

    Galaxy clusters enveloped by vast volumes of relativistic electrons. , keywords =. doi:10.1038/s41586-022-05149-3 , archivePrefix =. 2209.13617 , primaryClass =

    doi arXiv

  28. [36]

    Science , keywords =

    A radio ridge connecting two galaxy clusters in a filament of the cosmic web. Science , keywords =. doi:10.1126/science.aat7500 , archivePrefix =. 1906.07584 , primaryClass =

    1906 doi arXiv

  29. [37]

    Nature Astronomy , keywords =

    Observations of a pre-merger shock in colliding clusters of galaxies. Nature Astronomy , keywords =. doi:10.1038/s41550-019-0798-8 , archivePrefix =. 1906.10285 , primaryClass =

    1906 doi arXiv

  30. [38]

    , keywords =

    Diffuse radio source candidate in CIZA J1358.9-4750. , keywords =. doi:10.1093/pasj/psac098 , archivePrefix =. 2208.04750 , primaryClass =

    doi arXiv

  31. [39]

    , keywords =

    Second-order Fermi Reacceleration Mechanisms and Large-Scale Synchrotron Radio Emission in Intracluster Bridges. , keywords =. doi:10.1103/PhysRevLett.124.051101 , archivePrefix =. 2001.07718 , primaryClass =

    2001 doi arXiv

  32. [40]

    Galaxies , keywords =

    Magnetism Science with the Square Kilometre Array. Galaxies , keywords =. doi:10.3390/galaxies8030053 , archivePrefix =. 2006.03172 , primaryClass =

    2006 doi arXiv

  33. [41]

    , keywords =

    Rotation measure structure functions with higher-order stencils as a probe of small-scale magnetic fluctuations and its application to the Small and Large Magellanic Clouds. , keywords =. doi:10.1093/mnras/stac2972 , archivePrefix =. 2206.13798 , primaryClass =

    doi arXiv

  34. [42]

    , keywords =

    Structure functions with higher-order stencils as a probe to separate small- and large-scale magnetic fields. , keywords =. doi:10.1093/mnras/stae1935 , archivePrefix =. 2408.04156 , primaryClass =

    doi arXiv

  35. [43]

    , keywords =

    The quiescent intracluster medium in the core of the Perseus cluster. , keywords =. doi:10.1038/nature18627 , archivePrefix =. 1607.04487 , primaryClass =

    doi arXiv

  36. [44]

    Journal of Plasma Physics , keywords =

    Dynamo theories. Journal of Plasma Physics , keywords =. doi:10.1017/S0022377819000539 , archivePrefix =. 1903.07829 , primaryClass =

    1903 doi arXiv

  37. [45]

    , keywords =

    XRISM Observations of the Prototypical Cold Front in A3667. , keywords =. doi:10.3847/2041-8213/ae2a28 , archivePrefix =. 2510.26405 , primaryClass =

    doi

  38. [46]

    , keywords =

    Indications of an offset merger in Abell 3667. , keywords =. doi:10.1051/0004-6361/202449992 , archivePrefix =. 2403.10150 , primaryClass =

    doi arXiv

  39. [47]

    , keywords =

    Comparing XRISM Cluster Velocity Dispersions with Predictions from Cosmological Simulations: Are Feedback Models Too Ejective?. , keywords =. doi:10.3847/2041-8213/ae100c , archivePrefix =. 2510.06322 , primaryClass =

    doi

  40. [48]

    , keywords =

    The interpretation of XRISM X-ray measurements of turbulence in the intracluster medium: A comparison with cosmological simulations. , keywords =. doi:10.1051/0004-6361/202556070 , archivePrefix =. 2507.04727 , primaryClass =

    doi

  41. [49]

    , keywords =

    The bulk motion of gas in the core of the Centaurus galaxy cluster. , keywords =. doi:10.1038/s41586-024-08561-z , archivePrefix =. 2502.08722 , primaryClass =

    doi arXiv

  42. [50]

    , keywords =

    A XRISM/Resolve View of the Dynamics in the Hot Gaseous Atmosphere of M87. , keywords =. doi:10.3847/1538-4357/ae2c5c , archivePrefix =. 2512.06596 , primaryClass =

    doi

  43. [51]

    , keywords =

    The relation between gas density and velocity power spectra in galaxy clusters: High-resolution hydrodynamic simulations and the role of conduction. , keywords =. doi:10.1051/0004-6361/201424043 , archivePrefix =. 1404.5302 , primaryClass =

    doi arXiv

  44. [52]

    , keywords =

    X-ray surface brightness fluctuations in smooth galaxy cluster atmospheres. , keywords =. doi:10.1093/mnras/staf134 , archivePrefix =. 2503.08680 , primaryClass =

    doi arXiv

  45. [53]

    , keywords =

    X-ray surface brightness and gas density fluctuations in the Coma cluster. , keywords =. doi:10.1111/j.1365-2966.2011.20372.x , archivePrefix =. 1110.5875 , primaryClass =

    2011 doi

  46. [54]

    , keywords =

    Unexpected circular radio objects at high Galactic latitude. , keywords =. doi:10.1017/pasa.2020.52 , archivePrefix =. 2006.14805 , primaryClass =

    2020 doi arXiv

  47. [55]

    arXiv e-prints , keywords =

    Single- and double-headed odd radio circles in the LOFAR surveys. arXiv e-prints , keywords =. doi:10.48550/arXiv.2602.18294 , archivePrefix =. 2602.18294 , primaryClass =

    doi arXiv

  48. [56]

    , keywords =

    Discovery of diffuse radio source in Abell 1060. , keywords =. doi:10.1093/pasj/psae011 , archivePrefix =. 2311.08693 , primaryClass =

    doi arXiv

  49. [57]

    , year = 1968, month = jan, volume =

    The radio emission from galaxies in the Perseus cluster. , year = 1968, month = jan, volume =. doi:10.1093/mnras/138.1.1 , adsurl =

    1968 doi

  50. [58]

    , keywords =

    Origin and evolution of the structure in the head-tail radio galaxy of Abell 3322. , keywords =. doi:10.1093/pasj/psaf128 , archivePrefix =. 2511.03937 , primaryClass =

    doi

  51. [59]

    , keywords =

    Merger-driven multiscale ICM density perturbations: testing cosmological simulations and constraining plasma physics. , keywords =. doi:10.1093/mnras/stae208 , archivePrefix =. 2401.15179 , primaryClass =

    doi arXiv

  52. [60]

    Science Advances , keywords =

    Magnetic fields and relativistic electrons fill entire galaxy cluster. Science Advances , keywords =. doi:10.1126/sciadv.abq7623 , archivePrefix =. 2211.01493 , primaryClass =

    doi arXiv

  53. [61]

    , keywords =

    Stochastic reacceleration of relativistic electrons by turbulent reconnection: a mechanism for cluster-scale radio emission?. , keywords =. doi:10.1093/mnras/stw496 , archivePrefix =. 1603.00458 , primaryClass =

    doi arXiv

  54. [62]

    , keywords =

    The diffuse radio emission from the Coma cluster at 2.675 GHz and 4.85 GHz. , keywords =. doi:10.1051/0004-6361:20021474 , archivePrefix =. astro-ph/0210147 , primaryClass =

    doi arXiv

  55. [63]

    Science , keywords =

    Turbulence and Magnetic Fields in the Large-Scale Structure of the Universe. Science , keywords =. doi:10.1126/science.1154923 , archivePrefix =. 0805.2466 , primaryClass =

    doi arXiv

  56. [64]

    , keywords =

    Faraday Rotation Measure Due to the Intergalactic Magnetic Field. , keywords =. doi:10.1088/0004-637X/723/1/476 , archivePrefix =. 1009.0570 , primaryClass =

    doi arXiv

  57. [65]

    , keywords =

    Cosmic evolution of the Faraday rotation measure in the intracluster medium of galaxy clusters. , keywords =. doi:10.1051/0004-6361/202451119 , archivePrefix =. 2409.18580 , primaryClass =

    doi arXiv

  58. [66]

    doi:10.1017/9781139046657 , adsurl =

    Astrophysical Magnetic Fields: From Galaxies to the Early Universe. doi:10.1017/9781139046657 , adsurl =

    doi

  59. [67]

    , keywords =

    Diffuse Radio Emission from Galaxy Clusters. , keywords =. doi:10.1007/s11214-019-0584-z , archivePrefix =. 1901.04496 , primaryClass =

    1901 doi arXiv

  60. [68]

    , keywords =

    Probing turbulence in the Coma galaxy cluster. , keywords =. doi:10.1051/0004-6361:20041039 , archivePrefix =. astro-ph/0404132 , primaryClass =

    doi arXiv

  61. [69]

    Magnetohydrodynamics: Historical Evolution and Trends , year = 2007, editor =

    Turbulence and Magnetic Fields in Astrophysical Plasmas. Magnetohydrodynamics: Historical Evolution and Trends , year = 2007, editor =. doi:10.48550/arXiv.astro-ph/0507686 , adsurl =

    2007 doi arXiv

  62. [70]

    , keywords =

    Effects of Forcing on Shocks and Energy Dissipation in Interstellar and Intracluster Turbulences. , keywords =. doi:10.3847/1538-4357/ac41cc , archivePrefix =. 2111.02109 , primaryClass =

    doi arXiv

  63. [71]

    , keywords =

    Suppression of small scale dynamo action by an imposed magnetic field. , keywords =. doi:10.1103/PhysRevE.70.036408 , archivePrefix =. astro-ph/0402281 , primaryClass =

    doi arXiv

  64. [72]

    , keywords =

    Simulations of the Small-Scale Turbulent Dynamo. , keywords =. doi:10.1086/422547 , archivePrefix =. astro-ph/0312046 , primaryClass =

    doi arXiv

  65. [73]

    , keywords =

    Evolving turbulence and magnetic fields in galaxy clusters. , keywords =. doi:10.1111/j.1365-2966.2006.09918.x , archivePrefix =. astro-ph/0505144 , primaryClass =

    2006 doi

  66. [74]

    , keywords =

    Seed magnetic fields in turbulent small-scale dynamos. , keywords =. doi:10.1093/mnras/staa2978 , archivePrefix =. 2009.12024 , primaryClass =

    2009 doi arXiv

  67. [75]

    Reports on Progress in Physics , keywords =

    The origin, evolution and signatures of primordial magnetic fields. Reports on Progress in Physics , keywords =. doi:10.1088/0034-4885/79/7/076901 , archivePrefix =. 1504.02311 , primaryClass =

    doi arXiv

  68. [76]

    Physical Review Fluids , keywords =

    Saturation mechanism of the fluctuation dynamo at Pr _ M 1. Physical Review Fluids , keywords =. doi:10.1103/PhysRevFluids.5.043702 , archivePrefix =. 2003.07997 , primaryClass =

    2003 doi arXiv

  69. [77]

    , keywords =

    Turbulent Amplification and Structure of the Intracluster Magnetic Field. , keywords =. doi:10.3847/0004-637X/817/2/127 , archivePrefix =. 1507.00342 , primaryClass =

    doi arXiv

  70. [78]

    Physical Review Fluids , keywords =

    Saturation mechanism of the fluctuation dynamo in supersonic turbulent plasmas. Physical Review Fluids , keywords =. doi:10.1103/PhysRevFluids.6.103701 , archivePrefix =. 2109.11698 , primaryClass =

    doi arXiv

  71. [79]

    , keywords =

    Fluctuation dynamos and their Faraday rotation signatures. , keywords =. doi:10.1093/mnras/sts516 , archivePrefix =. 1210.3243 , primaryClass =

    doi arXiv

  72. [80]

    , keywords =

    Probing cluster magnetism with embedded and background radio sources in Planck clusters. , keywords =. doi:10.1051/0004-6361/202451885 , archivePrefix =. 2408.07178 , primaryClass =

    doi arXiv

  73. [81]

    Characterisation of the Fornax cluster's magnetic field and new insights on magnetisation in large scale systems

    The MeerKAT Fornax Survey VII. Characterisation of the Fornax cluster's magnetic field and new insights on magnetisation in large scale systems. arXiv e-prints , keywords =. doi:10.48550/arXiv.2604.18338 , archivePrefix =. 2604.18338 , primaryClass =

    doi arXiv

Pith tools

Reviewed July 8, 2026 · model on record in the stance chip above.