Pith. sign in

REVIEW 3 major objections 4 minor 300 references

Radio-halo intensity needs power-law fluctuations, not just a smooth profile, to match the observed angular power spectrum.

Reviewed by Pith at T0; open to challenge. T0 means a machine referee read the full paper against a public rubric. the ladder, T0–T4 →

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗

T0 review · grok-4.5

2026-07-10 17:32 UTC pith:V7GQZFRK

load-bearing objection Solid first application of visibility APS to radio-halo intensity fluctuations; the finite-source TGE correction and the Abell 2744 residual result are real, but the β=3 turbulence claim is still phenomenological and residual-systematics limited. the 3 major comments →

arxiv 2607.07814 v1 pith:V7GQZFRK submitted 2026-07-08 astro-ph.CO

Intensity fluctuations of radio halo in galaxy cluster: Insights from power spectrum estimation

Srijita Pal , Nirupam Roy , Sameer Salunkhe , Surajit Paul , Tanu Sharma , Samir Choudhuri This is my paper
classification astro-ph.CO
keywords galaxy clustersradio halosangular power spectrumICM turbulenceTapered Gridded Estimatorsynchrotron emissionmagnetohydrodynamics
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

This paper argues that the angular power spectrum of radio-halo emission is a practical way to study turbulence and particle acceleration in galaxy-cluster plasma. Using 610 MHz interferometric data on two clusters, the authors recover an excess power spectrum only for the disturbed system Abell 2744. They show that a smooth exponential surface-brightness profile alone cannot reproduce that spectrum; multiplicative Gaussian fluctuations whose power spectrum scales as ℓ^{-3} on top of the exponential are required. The measured slope is then compared with simple MHD-turbulence expectations, and the same visibility-based estimator is proposed as a route to detect faint or mega-halo emission that is hard to see in images, especially with the large data volumes expected from future arrays.

Core claim

A smooth exponential radial surface-brightness profile by itself fails to reproduce the residual angular power spectrum of Abell 2744; multiplicative zero-mean Gaussian fluctuations with C_ℓ ∝ ℓ^{-3.0±0.1} superimposed on that profile recover the observed spectrum over the fitted multipole range.

What carries the argument

Adapted Tapered Gridded Estimator (TGE) with an extra amplitude normalization that corrects for emission confined to a small fraction of the primary beam; the estimator yields unbiased C_ℓ directly from residual visibilities after compact-source subtraction.

Load-bearing premise

That residual power left after compact-source subtraction and above the scaled Galactic-synchrotron prediction is entirely the radio halo, so the fitted fluctuation index can be compared with turbulence models.

What would settle it

A deeper multi-frequency map of Abell 2744 in which residual compact sources and Galactic emission are subtracted to a level well below the present C_ℓ, yet the residual spectrum still requires (or no longer requires) an ℓ^{-3} fluctuation component on top of the exponential profile.

Watch this falsifier — get emailed when new claim-graph text bears on it.

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

3 major / 4 minor

Summary. The paper adapts the Tapered Gridded Estimator (TGE) to measure the angular power spectrum C_ℓ of residual 610 MHz GMRT visibilities from the radio-halo regions of Abell 2744 (MACSJ0014.3-302) and MACSJ0152.5-2852. After compact-source subtraction, only Abell 2744 shows excess power above a TGSS-scaled DGSE prediction. The authors derive and validate a finite-source-size normalization for TGE (Eq. 17), then show that a smooth exponential surface-brightness profile alone cannot reproduce the residual C_ℓ; multiplicative zero-mean Gaussian fluctuations with C_ℓ ∝ ℓ^{-3.0±0.1} on top of that profile recover the observed spectrum over 1700 ≲ ℓ ≲ 8525 (Fig. 10). They present piecewise power-law fits (Table 3) and discuss a possible link to ICM MHD turbulence, while noting that a full 3-D comparison is left for future work.

Significance. If the residual power is genuinely halo emission, the work supplies a visibility-domain route to intensity-fluctuation statistics that is complementary to imaging and RM studies, is computationally light, and is well-matched to large SKA-era cluster samples and megahalo searches. The finite-size TGE correction is derived from first principles and is end-to-end validated on independent simulations that recover the input power law to ≲ 20 % after correction—a concrete, reusable methodological contribution. The explicit demonstration that a smooth exponential fails while a power-law fluctuation component succeeds is a falsifiable, quantitative claim that can be tested on larger samples.

major comments (3)
  1. [Section 6, Figure 10] Section 6 / Fig. 10: The central claim that multiplicative fluctuations with β = 3.0 ± 0.1 are required rests on residual C_ℓ after interactive compact-source subtraction being free of residual calibration structure and DGSE spectral-index error. Section 2.3 and the bottom panels of Fig. 1 show residual structure around bright sources; the text itself notes that literature α values 2.5–3.2 shift the DGSE floor by factors of a few (Sec. 5.2). A quantitative robustness test (e.g., re-fitting after varying the CLEAN threshold or α over the stated range, or injecting residual point-source power) is needed before the necessity of the fluctuation component, and therefore the MHD comparison, can be regarded as secure.
  2. [Table 3, Figure 10] Table 3 and Fig. 10 report reduced-χ^{2} values of 0.08–0.22 for the preferred models. The paper notes that the C_ℓ errors assume a Gaussian random field (following Saha et al. 2019b) and may be overestimated when that assumption fails. Either the error model should be re-derived for the non-Gaussian (exponential + fluctuations) surface-brightness distribution used in the simulations, or the low reduced-χ^{2} should be shown not to bias the selection of β = 3.0.
  3. [Section 6, Abstract] Section 6: The comparison of the observed C_ℓ ∝ ℓ^{-3} with MHD turbulence models is left qualitative, with the authors correctly noting that synchrotron emissivity depends on both n_e and B_⊥ and that a full 3-D treatment is future work. The abstract and introduction nevertheless frame the result as constraining turbulence models. Either the abstract/intro language should be softened to match the discussion, or a minimal quantitative mapping (even under simplifying assumptions on n_e–B correlation) should be supplied so that the claimed comparison is falsifiable.
minor comments (4)
  1. [Abstract / Section 2] The abstract and title use MACSJ0014.3-302 while the body consistently uses Abell 2744; a single naming convention (or an explicit alias statement) would avoid confusion.
  2. [Section 6, Figure 8] Eq. (17) and the subsequent redefinition of θ_eff with the free factor m (Sec. 6) are clear in principle, but the numerical value of m θ_1^{2} adopted for the f = 10 o 0.6 scaling in Fig. 8 is not stated; quoting it would aid reproducibility.
  3. [Appendix A] Figures 11–12 (appendix) show the individual TGSS field fits used for the parametric DGSE prediction; a short table of the retained (A, β) values and the interpolated prediction at the cluster coordinates would make the DGSE floor easier to audit.
  4. Typographical inconsistencies: “foregorund” (Sec. 2.3), “Whi 1999” (missing full citation), and occasional C_l vs C_ℓ notation switches.

Circularity Check

1 steps flagged

No significant circularity: finite-size TGE normalization is first-principles and simulation-validated; the β=3.0 fluctuation index is an explicit fit to residual C_ℓ, not a claimed first-principles prediction.

specific steps
  1. fitted input called prediction [Section 6, Figure 10 and surrounding text]
    "If we take the fluctuations δ to be zero mean Gaussian random field that has an underlying power spectrum C_ℓ ∝ (1000/ℓ)^{3.0±0.1}, the APS from the simulation is found to be consistent with the observed C_ℓ. ... We have used simulations for 2.4 ≤ β ≤ 3.3, for which we estimated the reduced-χ^{2}. We find that for β=3.0, the reduced-χ^{2} ≈ 0.22 is the minimum ... Based on our analysis we report (1000/ℓ)^{3.0±0.1} as the best-fit model which best recovers the observed C_ℓ."

    β is chosen by scanning a grid and minimizing reduced-χ^{2} against the residual C_ℓ that the model is meant to explain. The paper does not claim a first-principles derivation of β=3 from MHD; it only reports the best-fit value. This is ordinary phenomenological fitting, not a circular 'prediction,' but it is the only place where an input is tuned to the target spectrum.

full rationale

The paper's methodological core (adapting 2D TGE for finite-extent sources via the amplitude factor θ'_w^{2}/θ_eff^{2} in Eq. 17) is derived from the convolution of the effective window and is independently validated on simulations whose input C_M_ℓ is known a priori (Section 4, Figures 2–3). DGSE is taken from external TGSS measurements (Choudhuri et al. 2020) and scaled by a literature spectral index; residual C_ℓ is then compared to that external floor. The strongest scientific claim—that a smooth exponential alone fails and multiplicative Gaussian fluctuations with C_ℓ ∝ ℓ^{-3.0±0.1} are required—is obtained by minimizing reduced-χ^{2} of simulated models against the same residual spectrum (Section 6, Figure 10). The paper never presents β=3 as a first-principles derivation from MHD theory; it only reports that this index recovers the data and notes that a full comparison with turbulence models is left for future work. That is ordinary model fitting, not circular prediction. Self-citations to the TGE literature are to prior methodological papers by overlapping authors, but those papers supply the estimator that is re-validated here; they are not load-bearing uniqueness theorems that force the scientific conclusion. Score 2 reflects only the minor, non-load-bearing self-citation of the estimator itself.

Axiom & Free-Parameter Ledger

5 free parameters · 5 axioms · 0 invented entities

The central claim rests on a small set of fitted amplitudes and indices plus standard radio-interferometric and statistical assumptions. No new physical entities are postulated; the power-law fluctuation field is a phenomenological model, not a new particle or force.

free parameters (5)
  • fluctuation spectral index β = 3.0 ± 0.1
    Fitted by minimizing reduced-χ² of simulated C_ℓ against residual data; best-fit 3.0 ± 0.1 (Section 6).
  • power-spectrum amplitudes A (and constant C) = 17±3 / 253±57 mK² (Abell 2744); 0.12±0.08 mK² (MACSJ0152)
    Piecewise power-law fits to residual C_ℓ (Table 3); free normalizations of the observed spectra.
  • exponential profile parameters I0, a = I0 ~ 4 mJy/beam, a ~ 0.016 arcsec^{-1}
    Best-fit to azimuthally averaged surface brightness of Abell 2744; used as the smooth component of the simulation model.
  • DGSE spectral index α = 2.8
    Adopted from La Porta et al. (2008) to scale TGSS C_ℓ from 147 MHz to 612 MHz; not re-fitted but controls the subtracted background level.
  • tapering parameter f and effective source size m θ1² = f = 0.6 preferred; m θ1² from f=5 and 0.8 pair
    f chosen by hand (0.6–10); m θ1² inferred from relative C_ℓ amplitudes at two f values to generalize the finite-size correction for non-Gaussian profiles.
axioms (5)
  • domain assumption Brightness-temperature fluctuations are a statistically homogeneous and isotropic Gaussian random field so that the two-point function fully characterizes the signal and the TGE noise-bias subtraction is unbiased.
    Stated in Section 3.1 and used throughout estimator derivation and error estimation; authors later note the real halo is non-Gaussian.
  • domain assumption Flat-sky approximation is adequate for the GMRT FoV at 610 MHz (~43′).
    Invoked in Section 3.2 for the finite-size normalization derivation.
  • domain assumption Primary beam and tapering window can be modelled as Gaussians, allowing closed-form effective window and normalization factor.
    Equations (4)–(17); standard for TGE literature but approximate near the first null.
  • ad hoc to paper Residual compact sources after interactive CLEAN subtraction contribute only a constant (Poisson) floor at high ℓ and do not bias the low-ℓ power-law slope.
    Assumed when interpreting the broken power-law and when omitting residual sources from the halo simulations (Section 6).
  • domain assumption DGSE in the target fields can be spatially interpolated from surrounding TGSS pointings and scaled by a single spectral index α = 2.8.
    Section 5.2; parametric and non-parametric routes both used, but α is taken from the literature without local re-measurement.

pith-pipeline@v1.1.0-grok45 · 39914 in / 3306 out tokens · 39862 ms · 2026-07-10T17:32:26.785165+00:00 · methodology

0 comments
read the original abstract

Non-thermal synchrotron emissions from radio halo allow us to study mechanisms of particle (re)acceleration, magnetic field distribution, merger history, and turbulence in the intra-cluster medium. We propose power spectrum estimation as a novel and complementary method to study galaxy clusters. We use 610 MHz observations of MACSJ0014.3-302 and MACSJ0152.5-2852 to estimate the angular power spectrum (C_l) from the central halo regions. The C_l shows excess emission only for MACSJ0014.3-302. Using simulations, we find that a halo model with power-law fluctuations, in addition to the smooth exponential radial profile, is required to explain the observed C_l. We compare the observed power-law with existing models of MHD turbulence. The method may be useful for large data from SKA, finding megahalos in other sources, or detecting faint cluster emissions beyond the visible extent.

Figures

Figures reproduced from arXiv: 2607.07814 by Nirupam Roy, Sameer Salunkhe, Samir Choudhuri, Srijita Pal, Surajit Paul, Tanu Sharma.

Figure 1
Figure 1. Figure 1: Total intensity map of Abell 2744 (left column) and MACSJ0152 (right column) fields at ∼ 610 MHz, obtained using CASA task tclean, after - (uppermost row) initial processing of the data with SPAM; (middle row) additional rounds of manual self-calibration using CASA; (lowermost row) compact source subtraction from the data [PITH_FULL_IMAGE:figures/full_fig_p005_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Cℓ as a function of ℓ for different tapering values ‘f’ as indicated in the legend, considering simulations of Abell 2744 observation. The leftmost panel shows Cℓ estimated from one realization of the simulations. The data points in the middle panel show Cℓ with 1σ error bars estimated from simulations of 10 different sky realizations drawn from the input model angular power spectrum C M ℓ (solid black lin… view at source ↗
Figure 3
Figure 3. Figure 3: Upper parts : The data points show Cℓ as a function of ℓ for simulations of Abell 2744 at different ta￾pering values ‘f’ after amplitude correction with 1σ error bars estimated from simulations of 10 different sky realiza￾tions drawn from the input model angular power spectrum C M ℓ (black solid lines). Lower parts : The fractional error δ = [C M ℓ − Cℓ]/CM ℓ (data points) and the relative statisti￾cal flu… view at source ↗
Figure 4
Figure 4. Figure 4: Cℓ as a function of ℓ estimated for Abell 2744 (left panel) and MACSJ0152 (right panel) at different tapering values ‘f’, as indicated in the legend, before (solid lines) and after (dashed lines) compact source subtraction. The vertical dashed lines show ℓmin where the convolution in TGE is expected to be important at the particular value of the f corresponding to the same colour. The 1σ errors in Cℓ are e… view at source ↗
Figure 5
Figure 5. Figure 5: This shows the fields surrounding Abell 2744 and MACSJ0152 within a radius of 3.5 ◦ that are observed in the TGSS survey. The black ×’ denotes the phase centre of the fields, and the black lines around them roughly show the FoV of GMRT for the TGSS survey. The red circular regions show the FoV for our observations at TGSS frequency; the phase centers (‘×’) correspond to (RA, DEC) of the two galaxy clusters… view at source ↗
Figure 6
Figure 6. Figure 6: The data points show Cℓ along with 1σ errors (the shaded regions) estimated by S. Choudhuri et al. 2020 at ∼ 147 MHz for the TGSS fields surrounding Abell 2744 and MACSJ0152, as shown in [PITH_FULL_IMAGE:figures/full_fig_p015_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: The shaded regions along with the data points show the same data as in [PITH_FULL_IMAGE:figures/full_fig_p015_7.png] view at source ↗
Figure 9
Figure 9. Figure 9: Piecewise power law model fit to the Cℓ for the residual data. The observed Cℓ (blue data points) at f = 0.6 for the residual data are shown with 1σ errors along with esti￾mated DGSE contribution (black-dashed lines). The best-fit models are also shown. The vertical blue-dashed lines denote ℓmin; the vertical black-dashed line in the left panel denote the ℓ corresponding to 300 ′′ angular size of the radio… view at source ↗
Figure 8
Figure 8. Figure 8: The observed Cℓ at f = 0.6 (blue-solid lines with data points) for the residual data for Abell 2744 are shown with 1σ errors. The same is also shown at f = 10 (red-dashed lines with data points) after we have scaled the estimated Cℓ to account for the small and finite size of the radio halo. The vertical blue-dashed line denotes ℓmin. sider which fields are meaningful in our analysis, as well as by conside… view at source ↗
Figure 10
Figure 10. Figure 10: The observed Cℓ at f = 0.6 (blue data points) for the residual data for Abell 2744 are shown with 1σ er￾rors. The recovered Cℓ with 1σ errors estimated from three independent realizations of the simulated model with an ex￾ponential radial profile and power-law fluctuations for the surface brightness are also shown. The model with Cℓ ∝ ℓ −3 power-law fluctuations (black-solid line and data points) agrees w… view at source ↗
Figure 11
Figure 11. Figure 11: DGSE fits for individual fields around Abell 2744, as shown in the left panel of [PITH_FULL_IMAGE:figures/full_fig_p024_11.png] view at source ↗
Figure 12
Figure 12. Figure 12: DGSE fits for individual fields around MACSJ0152, as shown in the right panel of [PITH_FULL_IMAGE:figures/full_fig_p025_12.png] view at source ↗

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

300 extracted references · 300 canonical work pages · 212 internal anchors

  1. [1]

    Intema, H.; Mooley, K. , url=

    work page

  2. [2]

    Low-frequency radio study of MACS clusters at 610 and 235 MHz using the GMRT

    Low-frequency radio study of MACS clusters at 610 and 235 MHz using the GMRT. , keywords =. doi:10.1093/mnras/stz1965 , archivePrefix =. 1903.06799 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stz1965 1903

  3. [3]

    , keywords =

    Strong-lensing analysis of a complete sample of 12 MACS clusters at z > 0.5: mass models and Einstein radii. , keywords =. doi:10.1111/j.1365-2966.2010.17574.x , archivePrefix =. 1002.0521 , primaryClass =

    work page doi:10.1111/j.1365-2966.2010.17574.x 2010

  4. [4]

    , keywords =

    The X-ray brightest clusters of galaxies from the Massive Cluster Survey. , keywords =. doi:10.1111/j.1365-2966.2010.16920.x , archivePrefix =. 1004.4683 , primaryClass =

    work page doi:10.1111/j.1365-2966.2010.16920.x 2010

  5. [5]

    Extragalactic Radio Sources , year = 1996, editor =

    Diffuse Cluster Radio Sources (Review). Extragalactic Radio Sources , year = 1996, editor =

    work page 1996

  6. [6]

    Observations of extended radio emission in clusters

    Observations of Extended Radio Emission in Clusters. , keywords =. doi:10.1007/s11214-008-9311-x , archivePrefix =. 0801.0985 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1007/s11214-008-9311-x

  7. [7]

    Clusters of galaxies : observational properties of the diffuse radio emission

    Clusters of galaxies: observational properties of the diffuse radio emission. , keywords =. doi:10.1007/s00159-012-0054-z , archivePrefix =. 1205.1919 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1007/s00159-012-0054-z 1919

  8. [8]

    doi:10.1046/j.1365-8711.2001.04315.x , keywords =

    Particle reacceleration in the Coma cluster: radio properties and hard X-ray emission. , keywords =. doi:10.1046/j.1365-8711.2001.03978.x , archivePrefix =. astro-ph/0008518 , primaryClass =

    work page doi:10.1046/j.1365-8711.2001.03978.x 2001

  9. [9]

    On The Non Thermal Emission and Acceleration of Electrons in Coma and Other Clusters of Galaxies

    On the Nonthermal Emission and Acceleration of Electrons in Coma and Other Clusters of Galaxies. , keywords =. doi:10.1086/321557 , archivePrefix =. astro-ph/0101145 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/321557

  10. [10]

    Particle acceleration mechanisms

    Particle Acceleration Mechanisms. , keywords =. doi:10.1007/s11214-008-9315-6 , archivePrefix =. 0801.0923 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1007/s11214-008-9315-6

  11. [11]

    , keywords =

    Formation of radio halos in clusters of galaxies from cosmic-ray protons. , keywords =. doi:10.1086/183300 , adsurl =

    work page doi:10.1086/183300

  12. [12]

    Cosmic Rays, Radio Halos and Non-Thermal X-ray Emission in Clusters of Galaxies

    Cosmic rays, radio halos and nonthermal X-ray emission in clusters of galaxies. Astroparticle Physics , keywords =. doi:10.1016/S0927-6505(99)00079-1 , archivePrefix =. astro-ph/9905122 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1016/s0927-6505(99)00079-1

  13. [13]

    Radio Halos of Galaxy Clusters from Hadronic Secondary Electron Injection in Realistic Magnetic Field Configurations

    Radio halos of galaxy clusters from hadronic secondary electron injection in realistic magnetic field configurations. , keywords =. doi:10.48550/arXiv.astro-ph/0008333 , archivePrefix =. astro-ph/0008333 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/0008333

  14. [14]

    The intracluster magnetic field power spectrum in Abell 2255

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

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:20065964

  15. [15]

    Long RXTE Observations of A2163

    Long RXTE Observations of A2163. , keywords =. doi:10.1086/506310 , archivePrefix =. astro-ph/0606097 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/506310

  16. [16]

    A Cold Front in A3667: Hydrodynamics and Magnetic Field in the Intracluster Medium

    A Cold Front in the Galaxy Cluster A3667: Hydrodynamics, Heat Conduction and Magnetic Field in the Intergalactic Medium. Astronomy Letters , keywords =. doi:10.1134/1.1499173 , archivePrefix =. astro-ph/0209551 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1134/1.1499173

  17. [17]

    , keywords =

    Evolution and structure of magnetic fields in simulated galaxy clusters. , keywords =. doi:10.1051/0004-6361:20020241 , adsurl =

    work page doi:10.1051/0004-6361:20020241

  18. [18]

    Planck 2018 results. V. CMB power spectra and likelihoods. , keywords =. doi:10.1051/0004-6361/201936386 , archivePrefix =. 1907.12875 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201936386 2018

  19. [19]

    Deep low-frequency radio observations of Abell 2256. II. The ultra-steep spectrum radio halo. , keywords =. doi:10.1051/0004-6361/202244925 , archivePrefix =. 2209.03288 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202244925

  20. [20]

    Formation of Galaxy Clusters

    Formation of Galaxy Clusters. , keywords =. doi:10.1146/annurev-astro-081811-125502 , archivePrefix =. 1205.5556 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1146/annurev-astro-081811-125502

  21. [21]

    Diffuse Radio Emission from Galaxy Clusters

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

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1007/s11214-019-0584-z 1901

  22. [22]

    CHEX-MATE: Characterization of the intra-cluster medium temperature distribution

    CHEX-MATE: Characterization of the intra-cluster medium temperature distribution. , keywords =. doi:10.1051/0004-6361/202346651 , archivePrefix =. 2311.02176 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202346651

  23. [23]

    Exploring diffuse radio emission in galaxy clusters and groups with the uGMRT and the SKA

    Exploring diffuse radio emission in galaxy clusters and groups with uGMRT and SKA. Journal of Astrophysics and Astronomy , keywords =. doi:10.1007/s12036-023-09914-2 , archivePrefix =. 2211.01393 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1007/s12036-023-09914-2

  24. [24]

    , keywords =

    Origin and transport of electrons in the halo radio source in the Coma cluster. , keywords =. doi:10.1086/155011 , adsurl =

    work page doi:10.1086/155011

  25. [25]

    Magnetic fields and relativistic electrons fill entire galaxy cluster

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

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1126/sciadv.abq7623

  26. [26]

    The Case for Electron Re-Acceleration at Galaxy Cluster Shocks

    The case for electron re-acceleration at galaxy cluster shocks. Nature Astronomy , keywords =. doi:10.1038/s41550-016-0005 , archivePrefix =. 1701.01439 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/s41550-016-0005

  27. [27]

    Radio halos in nearby (z < 0.4) clusters of galaxies

    Radio halos in nearby (z < 0.4) clusters of galaxies. , keywords =. doi:10.1051/0004-6361/200912667 , archivePrefix =. 0909.0911 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/200912667

  28. [28]

    Galaxy clusters enveloped by vast volumes of relativistic electrons

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

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/s41586-022-05149-3

  29. [29]

    Discovery of a radio megahalo in the cluster PLCKG287.0+32.9 using the uGMRT

    Discovery of a radio megahalo in the cluster PLCKG287.0+32.9 using the uGMRT. arXiv e-prints , keywords =. doi:10.48550/arXiv.2503.12136 , archivePrefix =. 2503.12136 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2503.12136

  30. [30]

    Evolution of shocks and turbulence in major cluster mergers

    Evolution of Shocks and Turbulence in Major Cluster Mergers. , keywords =. doi:10.1088/0004-637X/726/1/17 , archivePrefix =. 1001.1170 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/726/1/17

  31. [31]

    Cosmic rays in galaxy clusters and their non-thermal emission

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

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1142/s0218271814300079

  32. [32]

    The Physics of Cluster Mergers

    The Physics of Cluster Mergers. Merging Processes in Galaxy Clusters , year = 2002, editor =. doi:10.1007/0-306-48096-4_1 , archivePrefix =. astro-ph/0105418 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1007/0-306-48096-4_1 2002

  33. [33]

    Advancing Astrophysics with the Square Kilometre Array (AASKA14) , year = 2015, month = apr, eid =

    Advancing Astrophysics with the Square Kilometre Array. Advancing Astrophysics with the Square Kilometre Array (AASKA14) , year = 2015, month = apr, eid =. doi:10.22323/1.215.0174 , adsurl =

    work page doi:10.22323/1.215.0174 2015

  34. [34]

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

    work page doi:10.1086/175121

  35. [35]

    Polarization intermittency in MHD and its influence on turbulent cascade

    Polarization Intermittency and Its Influence on MHD Turbulence. , keywords =. doi:10.1086/503708 , archivePrefix =. astro-ph/0512315 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/503708

  36. [36]

    Burgers Turbulence

    Burgers turbulence. , keywords =. doi:10.1016/j.physrep.2007.04.002 , archivePrefix =. 0704.1611 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1016/j.physrep.2007.04.002 2007

  37. [37]

    On the evolution of giant radio halos and their connection with cluster mergers

    On the evolution of giant radio halos and their connection with cluster mergers. , keywords =. doi:10.1051/0004-6361/200912751 , archivePrefix =. 0909.2343 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/200912751

  38. [38]

    Back and forth from cool core to non-cool core: clues from radio-halos

    Back and forth from cool core to non-cool core: clues from radio halos. , keywords =. doi:10.1051/0004-6361/201117306 , archivePrefix =. 1106.4563 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201117306

  39. [39]

    New giant radio sources and underluminous radio halos in two galaxy clusters

    New giant radio sources and underluminous radio halos in two galaxy clusters. , keywords =. doi:10.1051/0004-6361/201731174 , archivePrefix =. 1709.06364 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201731174

  40. [40]

    Akademiia Nauk SSSR Doklady , year = 1941, month = jan, volume =

    The Local Structure of Turbulence in Incompressible Viscous Fluid for Very Large Reynolds' Numbers. Akademiia Nauk SSSR Doklady , year = 1941, month = jan, volume =

    work page 1941

  41. [41]

    , year = 1964, month = feb, volume =

    Turbulence of a Conducting Fluid in a Strong Magnetic Field. , year = 1964, month = feb, volume =

    work page 1964

  42. [42]

    Physics of Fluids , year = 1965, month = jul, volume =

    Inertial-Range Spectrum of Hydromagnetic Turbulence. Physics of Fluids , year = 1965, month = jul, volume =. doi:10.1063/1.1761412 , adsurl =

    work page doi:10.1063/1.1761412 1965

  43. [43]

    MHD Turbulence as a Foreground for CMB Studies

    Magnetohydrodynamic Turbulence as a Foreground for Cosmic Microwave Background Studies. , keywords =. doi:10.1086/342722 , archivePrefix =. astro-ph/0205284 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/342722

  44. [44]

    Compressible Sub-Alfvenic MHD turbulence in Low-beta Plasmas

    Compressible Sub-Alfv \'e nic MHD Turbulence in Low- Plasmas. , keywords =. doi:10.1103/PhysRevLett.88.245001 , archivePrefix =. astro-ph/0205282 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevlett.88.245001

  45. [45]

    New Regime of MHD Turbulence: Cascade Below Viscous Cutoff

    New Regime of Magnetohydrodynamic Turbulence: Cascade below the Viscous Cutoff. , keywords =. doi:10.1086/339453 , archivePrefix =. astro-ph/0112195 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/339453

  46. [46]

    , keywords =

    Magnetohydrodynamic turbulence in supernova remnants. , keywords =. doi:10.1111/j.1745-3933.2008.00591.x , archivePrefix =. 0811.1466 , primaryClass =

    work page doi:10.1111/j.1745-3933.2008.00591.x 2008

  47. [47]

    On the connection between turbulent motions and particle acceleration in galaxy clusters

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

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/2041-8213/aa7c1a 2041

  48. [48]

    Power Spectrum of the density of cold atomic gas in the Galaxy towards Cas A and Cygnus A

    Power Spectrum of the Density of Cold Atomic Gas in the Galaxy toward Cassiopeia A and Cygnus A. , keywords =. doi:10.1086/317104 , archivePrefix =. astro-ph/0007366 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/317104

  49. [49]

    Faraday Rotation Observations of Magnetic Fields in galaxy Clusters

    Faraday Rotation Observations of Magnetic Fields in Galaxy Clusters. Journal of Korean Astronomical Society , keywords =. doi:10.5303/JKAS.2004.37.5.337 , archivePrefix =. astro-ph/0412268 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.5303/jkas.2004.37.5.337 2004

  50. [50]

    Magnetic Field in Clusters of Galaxies

    Magnetic Fields in Clusters of Galaxies. International Journal of Modern Physics D , keywords =. doi:10.1142/S0218271804005080 , archivePrefix =. astro-ph/0410182 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1142/s0218271804005080

  51. [51]

    Faraday Rotation Measure Synthesis

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

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:20052990

  52. [52]

    Physics of Fluids , year = 1967, month = jul, volume =

    Inertial Ranges in Two-Dimensional Turbulence. Physics of Fluids , year = 1967, month = jul, volume =. doi:10.1063/1.1762301 , adsurl =

    work page doi:10.1063/1.1762301 1967

  53. [53]

    Journal of Fluid Mechanics , year = 1971, month = jan, volume =

    Inertial-range transfer in two- and three-dimensional turbulence. Journal of Fluid Mechanics , year = 1971, month = jan, volume =. doi:10.1017/S0022112071001216 , adsurl =

    work page doi:10.1017/s0022112071001216 1971

  54. [54]

    Physics of Fluids , year = 1968, month = mar, volume =

    Diffusion Approximation for Two-Dimensional Turbulence. Physics of Fluids , year = 1968, month = mar, volume =. doi:10.1063/1.1691968 , adsurl =

    work page doi:10.1063/1.1691968 1968

  55. [55]

    Physics of Fluids , year = 1969, month = dec, volume =

    Computation of the Energy Spectrum in Homogeneous Two-Dimensional Turbulence. Physics of Fluids , year = 1969, month = dec, volume =. doi:10.1063/1.1692443 , adsurl =

    work page doi:10.1063/1.1692443 1969

  56. [56]

    , keywords =

    Low-wavenumber spectral characteristics of velocity and temperature in the atmospheric surface layer. , keywords =. doi:10.1029/94JD02616 , adsurl =

    work page doi:10.1029/94jd02616

  57. [57]

    Energy spectrum of two-dimensional acoustic turbulence

    Energy Spectrum of Two-Dimensional Acoustic Turbulence. , keywords =. doi:10.1103/PhysRevLett.128.224501 , archivePrefix =. 2112.10662 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevlett.128.224501

  58. [58]

    A study of Kepler supernova remnant: angular power spectrum estimation from radio frequency data

    A study of Kepler supernova remnant: angular power spectrum estimation from radio frequency data. , keywords =. doi:10.1093/mnras/stz2528 , archivePrefix =. 1909.03195 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stz2528 1909

  59. [59]

    IEEE Proceedings , keywords =

    The Very Large Array: design and performance of a modern synthesis radio telescope. IEEE Proceedings , keywords =. doi:10.1109/PROC.1983.12765 , adsurl =

    work page doi:10.1109/proc.1983.12765 1983

  60. [60]

    MeerKAT Key Project Science, Specifications, and Proposals

    MeerKAT Key Project Science, Specifications, and Proposals. arXiv e-prints , keywords =. doi:10.48550/arXiv.0910.2935 , archivePrefix =. 0910.2935 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.0910.2935

  61. [61]

    American Astronomical Society Meeting Abstracts \#215 , year = 2010, series =

    Survey Science with ASKAP: Polarization Sky Survey of the Universe's Magnetism (POSSUM). American Astronomical Society Meeting Abstracts \#215 , year = 2010, series =

    work page 2010

  62. [62]

    Synthesis Imaging in Radio Astronomy II , year = 1999, series =

    Synthesis Imaging in Radio Astronomy II. Synthesis Imaging in Radio Astronomy II , year = 1999, series =

    work page 1999

  63. [63]

    Evidence for Reionization at z ~ 6: Detection of a Gunn-Peterson Trough in a z=6.28 Quasar

    Evidence for Reionization at z -0.5ex 6: Detection of a Gunn-Peterson Trough in a z=6.28 Quasar. , keywords =. doi:10.1086/324231 , archivePrefix =. astro-ph/0108097 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/324231

  64. [64]

    Evolution of the Ionizing Background and the Epoch of Reionization from the Spectra of z~6 Quasars

    Evolution of the Ionizing Background and the Epoch of Reionization from the Spectra of z -0.5ex 6 Quasars. , keywords =. doi:10.1086/339030 , archivePrefix =. astro-ph/0111184 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/339030

  65. [65]

    Constraining the Evolution of the Ionizing Background and the Epoch of Reionization with z -0.5ex 6 Quasars. II. A Sample of 19 Quasars. , keywords =. doi:10.1086/504836 , archivePrefix =. astro-ph/0512082 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/504836

  66. [66]

    , keywords =

    The Large Bright QSO Survey for Damped LY alpha Absorption Systems. , keywords =. doi:10.1086/176523 , adsurl =

    work page doi:10.1086/176523

  67. [67]

    Data Analysis for Precision 21 cm Cosmology

    Data Analysis for Precision 21 cm Cosmology. , keywords =. doi:10.1088/1538-3873/ab5bfd , archivePrefix =. 1907.08211 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/1538-3873/ab5bfd 1907

  68. [68]

    Radiative processes in astrophysics

    work page

  69. [69]

    IEEE Transactions on Acoustics Speech and Signal Processing , keywords =

    Some Windows with Very Good Sidelobe Behavior. IEEE Transactions on Acoustics Speech and Signal Processing , keywords =

    work page

  70. [70]

    Science with the Murchison Widefield Array

    Science with the Murchison Widefield Array. , keywords =. doi:10.1017/pas.2013.009 , archivePrefix =. 1212.5151 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1017/pas.2013.009 2013

  71. [71]

    HI constraints from the cross-correlation of eBOSS galaxies and Green Bank Telescope intensity maps

    HI constraints from the cross-correlation of eBOSS galaxies and Green Bank Telescope intensity maps. , keywords =. doi:10.1093/mnras/stab3621 , archivePrefix =. 2102.04946 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stab3621

  72. [72]

    Lack of clustering in low-redshift 21-cm intensity maps cross-correlated with 2dF galaxy densities

    Low-amplitude clustering in low-redshift 21-cm intensity maps cross-correlated with 2dF galaxy densities. , keywords =. doi:10.1093/mnras/sty346 , archivePrefix =. 1710.00424 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sty346

  73. [73]

    Baryonic acoustic oscillations from 21cm intensity mapping: the Square Kilometre Array case

    Baryonic acoustic oscillations from 21 cm intensity mapping: the Square Kilometre Array case. , keywords =. doi:10.1093/mnras/stw3224 , archivePrefix =. 1609.00019 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stw3224

  74. [74]

    The Hydrogen Intensity and Real-time Analysis eXperiment: 256-Element Array Status and Overview

    Hydrogen Intensity and Real-Time Analysis Experiment: 256-element array status and overview. Journal of Astronomical Telescopes, Instruments, and Systems , keywords =. doi:10.1117/1.JATIS.8.1.011019 , archivePrefix =. 2109.13755 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1117/1.jatis.8.1.011019

  75. [75]

    Effects of Antenna Beam Chromaticity on Redshifted 21~cm Power Spectrum and Implications for Hydrogen Epoch of Reionization Array

    Effects of Antenna Beam Chromaticity on Redshifted 21 cm Power Spectrum and Implications for Hydrogen Epoch of Reionization Array. , keywords =. doi:10.3847/0004-637X/825/1/9 , archivePrefix =. 1603.08958 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/0004-637x/825/1/9

  76. [76]

    The auto and cross angular power spectrum of the Cas A supernova remnant in radio and X-ray

    The auto- and cross-angular power spectrum of the Cas A supernova remnant in radio and X-ray. , keywords =. doi:10.1093/mnras/stab446 , archivePrefix =. 2102.06093 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stab446

  77. [77]

    Cosmological constraints from 21cm surveys after reionization

    Cosmological constraints from 21cm surveys after reionization. , keywords =. doi:10.1088/1475-7516/2009/10/030 , archivePrefix =. 0812.0419 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/1475-7516/2009/10/030 2009

  78. [78]

    Primordial Non-Gaussianity in the Forest: 3D Bispectrum of Ly-alpha Flux Spectra Along Multiple Lines of Sight

    Primordial Non-Gaussianity in the Forest: 3D Bispectrum of Lyman- Flux Spectra along Multiple Lines of Sight. , keywords =. doi:10.1103/PhysRevLett.109.121301 , archivePrefix =. 1205.2790 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevlett.109.121301

  79. [79]

    arXiv e-prints , keywords =

    Detection of Cosmological 21 cm Emission with the Canadian Hydrogen Intensity Mapping Experiment. arXiv e-prints , keywords =

    work page

  80. [80]

    Time series analysis with CLEAN. I. Derivation of a spectrum. , year = 1987, month = apr, volume =. doi:10.1086/114383 , adsurl =

    work page doi:10.1086/114383 1987

Showing first 80 references.