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REVIEW 3 major objections 4 minor 101 references

Multi-frequency Radio Observations of the Dissociative Cluster Merger CIZA J0107.7+5408

T0 review · 3 major / 4 minor · reviewed 2026-08-11 · deepseek-v4-flash

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Pith's one-line read In the merging cluster CIZA0107, a 340 MHz radio edge coincides with a weak shock, while the 3 GHz emission shows no edge.

desk verdict Solid new radio data and a real frequency-dependent edge; the X-ray shock coincidence is suggestive but needs an independent wedge and a corrected Mach-number error. read the letter →

arxiv 2412.15015 v3 pith:C4Q3ANQY submitted 2024-12-19 astro-ph.GA

Emma Schwartzman , Tracy Clarke , Simona Giacintucci , Wendy Peters , Scott Randall , Reinout van Weeren , Arnab Sarkar , Lawrence Rudnick
show 4 more authors
Elizabeth Blanton Kyle Finner Tony Mroczkowski Paul Nulsen
This is my paper · ORCID
classification astro-ph.GA
keywords galaxyclustersradiohalosrelicsphoenixclustermergersdiffusesynchrotronemissionultra-steepspectrumCIZAJ0107.7+5408
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

CIZA J0107.7+5408 is a rare dissociative binary cluster merger: two roughly equal subclusters whose gas has been stripped from their galaxies during a head-on passage. Using new VLA images at 340 MHz and 3 GHz, the paper tries to establish that the diffuse radio emission is steep-spectrum ($\alpha \sim -1.3$) on roughly 0.5 Mpc scales in both subclusters, and that the southwestern subcluster shows a sharp radio edge at 340 MHz coincident with a weak X-ray shock ($M \sim 1.2$), while the same edge is absent at 3 GHz. If true, this frequency-dependent edge is not easily explained as a classic radio relic or radio halo-shock edge; the authors argue it may be the boundary of ultra-steep-spectrum fossil plasma re-energized by the shock. The result matters because it constrains how merger shocks re-accelerate old electron populations, and because it leaves open whether the system hosts a rare double radio halo or two projected relics.

What carries the argument

The argument rests on four linked pieces: matched-resolution, point-source-subtracted VLA images at 340 MHz and 3 GHz; a spectral index map and a spectral-tomography separation that divide the emission into a flatter diffuse component and steeper ultra-steep-spectrum components; an X-ray surface-brightness profile extracted in a wedge centered on the radio edge and fit with a projected broken power law; and the standard hydrodynamic shock jump conditions used to convert the fitted density jump into a Mach number. The broken power law is the load-bearing identity: it turns a visual radio edge into a quantitative X-ray shock candidate, while the spectral tomography identifies the edge with the steep-spectrum synchrotron plasma and not with the flatter, GHz-bright emission.

What would settle it

Re-extract the X-ray surface-brightness profile in a wedge defined without reference to the radio image, over the full southern quadrant; if the density jump at $\sim$3 arcmin disappears, the claimed edge-shock coincidence collapses.

Watch

Extended reading notes

Core claim

At 340 MHz the diffuse radio emission associated with the southwestern subcluster ends in a sharp surface-brightness drop, and this radio edge is spatially coincident with an X-ray surface-brightness discontinuity and a region of elevated gas temperature identified in earlier X-ray data. A projected broken-power-law fit to the X-ray profile gives a density compression $C = 1.3 \pm 0.12$, which through the standard shock jump conditions for $\gamma = 5/3$ corresponds to a weak shock with Mach number $M = 1.2 \pm 0.6$. The same region imaged at 3 GHz shows no edge-like feature and the emission extends beyond the shock. The paper confirms steep-spectrum emission ($\alpha \sim -1.3$) over $\sim$0.5 Mpc scales in both subclusters, measures two ultra-steep-spectrum regions with $\alpha \sim -2.2$ and $\sim -2.9$ between 74 and 340 MHz, and uses spectral tomography to show that the 340 MHz edge traces the steep-spectrum component. It concludes that the edge is best understood as a fossil-plasma boundary rather than a standard shock-accelerated relic, while the overall diffuse emission could be either a double radio halo or two projected relics.

Load-bearing premise

The load-bearing premise is that the X-ray surface-brightness discontinuity is a real shock front rather than a fitting artifact or projection effect, because the wedge used for the X-ray profile was chosen specifically where the radio edge had already been seen and the fitted Mach number, $M = 1.2 \pm 0.6$, is within one $\sigma$ of no shock at all.

Editorial extensions

If this is right

  • The standard radio halo-shock edge and radio relic interpretations would need revision, because a low-frequency-only edge is a morphology that must be explained by electron aging and re-acceleration physics.
  • The two ultra-steep-spectrum regions, with $\alpha \sim -2.2$ and $-2.9$, are superimposed on flatter diffuse emission, so single-frequency surveys at GHz wavelengths could miss the fossil component entirely.
  • If the diffuse emission is a double radio halo, CIZA0107 would be a rare post-merger example rather than a pre-merger pair; if it is two projected relics, the relics are about an order of magnitude under-luminous relative to established scaling relations.
  • The lack of a detected counter-shock in the northeast, combined with the likely line-of-sight merger geometry, means the system's true Mach number is probably higher than the observed $M \sim 1.2$, weakening simple estimates of shock acceleration efficiency.

Reading between the lines

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

  • We infer that low-frequency-only radio edges may be common in post-merger clusters and are currently missed by surveys at 1-3 GHz; a systematic 150-400 MHz survey of dissociative mergers could reveal a population of fossil-plasma edges.
  • We infer that the degeneracy between a double halo and a projected double relic could be broken by deep polarization imaging: halos are typically unpolarized while relics show roughly 30% polarization, and no such measurement yet exists for CIZA0107.
  • We infer that if the edge is re-energized fossil AGN plasma, deeper low-frequency imaging should show the ultra-steep-spectrum regions extending to or beyond the shock front, and may reveal faint detached radio lobes outside the current 74 MHz contours.
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Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 4 minor

Summary. The paper presents new VLA 340 MHz (P-band) and 3 GHz (S-band) observations of the dissociative cluster merger CIZA J0107.7+5408. After point-source subtraction and matched-resolution imaging, the authors confirm ~0.5 Mpc diffuse steep-spectrum emission (alpha ~ -1.3) in both subclusters, measure integrated fluxes and spectral indices, identify two ultra-steep-spectrum regions with alpha < -2, and use spectral tomography to separate flatter and steeper components. The central new morphological claim is a sharp 340 MHz radio edge in the southwest that is spatially coincident with a candidate weak shock (M ~ 1.2) inferred from a Chandra surface-brightness discontinuity, while the 3 GHz emission shows no corresponding edge and extends beyond the shock. The paper concludes that the system may host a double radio halo or two projected relics, and that the 340 MHz edge may be an extension of the northwestern ultra-steep-spectrum emission related to a compressed fossil electron population.

Significance. If the edge-shock association is accepted, CIZA0107 would be an unusual system: a low-frequency-only radio edge coincident with a weak X-ray shock, in tension with standard relic and halo-shock-edge scenarios, and relevant to models of electron re-acceleration and fossil plasma compression. The radio products themselves are a genuine strength: the 340 MHz edge is visible even in the non-point-source-subtracted image, the 3 GHz comparison is made at matched resolution, integrated flux errors include flux-scale uncertainties, and the ultra-steep-spectrum fits are clearly documented. The paper's weakest load-bearing element is the X-ray shock analysis in Section 5, which is not independent of the radio detection and whose quoted Mach-number uncertainty is not internally consistent with the stated density-jump error. The direct radio measurements and the frequency-dependent morphology are solid; the shock coincidence and the phoenix interpretation built on it currently need either re-analysis or a clearly downgraded status.

major comments (3)
  1. [Section 5, Figure 6B; Section 7, bullet 4] The X-ray surface-brightness profile is extracted in a wedge 'guided by the radio observations' (Section 5), and a broken power law is then fitted to that selected wedge. The resulting discontinuity at r_model = 3.02' therefore cannot be regarded as an independent confirmation of a shock at the radio edge. The conclusion bullet in Section 7 states without caveat that 'we have identified an X-ray surface brightness discontinuity at the radio edge,' which overstates what a radio-selected wedge can establish. I recommend fitting the profile in several wedges defined blind to the radio feature, checking stability with respect to wedge boundaries, and reporting the change in chi^2 with the number of free parameters, or explicitly presenting the X-ray result as a candidate that requires independent confirmation.
  2. [Section 5, Equation (1), Figure 6C] Propagating C = 1.3 +/- 0.12 through Equation (1) yields M = 1.20 +/- 0.08, not +/- 0.6. The quoted +/- 0.6 is not derivable from the stated density-jump uncertainty. If +/- 0.6 is intended to include projection or systematic effects, that derivation should be given. As written, the significance of the shock is ambiguous: with +/- 0.6, M is consistent with no shock (M = 1) at the 1-sigma level, while with +/- 0.08 the density jump is precise but still measured only in a radio-selected wedge. In addition, the comparison between the broken power law (reduced chi^2 = 1.004) and the single beta model (reduced chi^2 = 1.29) is reported without Delta-chi^2, degrees of freedom, or a parameter penalty, so the claim that the broken power law is 'statistically better' is not quantitatively supported.
  3. [Section 6.1.1] The phoenix/compression interpretation is built on the edge-shock coincidence: the text proposes that the ultra-steep-spectrum emission has been adiabatically compressed and re-energized by the passage of the shock. If the X-ray discontinuity is not robust, is a fitting artifact, or is strongly affected by projection, this scenario loses its main observational support. The frequency-dependent morphology itself (a 340 MHz edge with no corresponding 3 GHz edge) is an interesting result independent of the shock, and the discussion should be reorganized so that the radio-only morphology is presented as the secure finding, with the shock association and the phoenix scenario explicitly labeled as speculative pending an independent X-ray analysis. The paper does note the possible line-of-sight merger component from Finner et al. (2023), but this caveat is used mainly to explain a low Mach number rather than as a test of the association.
minor comments (4)
  1. [Section 5, Equation (1)] The sentence 'where 1/C is equivalent to the gas density ratio rho_2/rho_1' appears to invert the ratio: for C = rho_2/rho_1 > 1, the Rankine-Hugoniot relation gives rho_1/rho_2 on the left-hand side of Equation (1). Please correct the notation or define C as the pre-to-post-shock density ratio.
  2. [Section 4.2.1, Figure 4] The spectral-tomography coefficients A and B are described only as chosen to avoid negative residuals; for reproducibility, state the numerical values and the exact subtraction equations, even if the figure is intended for qualitative illustration.
  3. [Section 6.1.3, Figure 8B] For the individual subclusters, the text reports Spearman coefficients of 0.34 and 0.40 but does not report the individual p-values that accompany those coefficients; adding them would make the point-to-point correlation results fully comparable to the whole-cluster result.
  4. [References] The van Weeren et al. (2019) reference appears twice in the reference list with different journal formatting (SSRv 215, 16 and Space Science Reviews 215); these entries should be merged.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: all quantitative claims are direct measurements or independent fits, with no parameter defined from the quantity it is used to predict; the radio-guided X-ray wedge is a selection caveat, not a definitional circularity.

full rationale

The paper's quantitative results—340 MHz and 3 GHz integrated fluxes, spectral indices between 74 MHz and 3 GHz, USS component slopes, and the X-ray surface brightness broken-power-law fit—are direct measurements from archival or new data. No equation is defined in terms of the quantity it claims to predict. The spectral tomography coefficients A and B are explicitly used for qualitative display only and do not enter any numerical claim. The X-ray wedge is admittedly 'guided by the radio observations,' so the subsequent 'coincidence' between the fitted break radius and the radio edge is not an independent blind detection; however, the broken-power-law fit is not forced by construction to place a break at the radio edge, and no parameter is fitted to the edge position and then renamed a prediction. Prior results from R16 and Finner et al. (2023), some with overlapping authors, are used as supporting data (temperature map, 74 MHz contours, lensing geometry) rather than as a uniqueness or existence theorem that alone forces the paper's interpretation. The mismatch between the stated Mach-number uncertainty (±0.6) and simple error propagation from C = 1.3 ± 0.12 (~±0.08) is a statistical reporting issue, not circularity. No load-bearing self-citation chain or ansatz-smuggling step was found; the central radio-edge morphology claim rests on the directly imaged 340 MHz drop-off and the matched-resolution absence of a 3 GHz edge, both of which are independent of the fitted X-ray parameters.

Assumptions & free parameters 2 free parameters · 5 assumptions · 1 invented entities

The quantitative claims rest on direct radio and X-ray measurements, not on fitted parameters. The only hand-chosen free parameters are the qualitative spectral tomography coefficients A and B. The main axioms are standard cosmology, standard synchrotron and shock physics, and the assumption that the 74 MHz contours trace the USS regions. One unobserved fossil electron population is invoked to explain the steepest emission, with no independent detection.

free parameters (2)
  • Spectral tomography subtraction coefficient A = Not quoted numerically; chosen as the maximum fraction subtracted without creating negative residuals
    Used only for the qualitative flatter-component image in Figure 4; does not enter any quantitative claim.
  • Spectral tomography subtraction coefficient B = Not quoted numerically; chosen as the maximum fraction subtracted without creating negative residuals
    Used only for the qualitative steeper-component image in Figure 4; does not enter any quantitative claim.
assumptions (5)
  • domain assumption Flat Lambda-CDM cosmology with Omega_L = 0.69, Omega_m = 0.31, H0 = 67.7 km/s/Mpc
    Adopted in Section 1 for luminosity distances, physical scales, and luminosities.
  • standard math Rankine-Hugoniot jump conditions with adiabatic index gamma = 5/3
    Used in Section 5, Equation 1, to convert the fitted gas density compression factor into a Mach number.
  • domain assumption Synchrotron power-law model S_nu proportional to nu^alpha
    Used throughout for spectral indices of radio emission and for interpreting steep spectra as old or re-energized electron populations.
  • domain assumption Broken power-law model projected on the sky for the X-ray surface brightness profile
    Used in Section 5 to identify the X-ray surface brightness discontinuity at about 3 arcminutes.
  • domain assumption The 74 MHz VLSSr 3-sigma contours delineate the ultra-steep-spectrum regions
    Used in Section 4.2.2 and Figure 5 to define the USS regions and measure their 340 MHz and 3 GHz fluxes.
invented entities (1)
  • Unseen fossil relativistic electron population in the southwestern subcluster
    purpose: Proposed to explain the ultra-steep-spectrum emission and the 340 MHz radio edge as adiabatically compressed, re-energized old AGN plasma (a radio phoenix).
    The paper explicitly states in Section 6.1.1 that no radio galaxy that might be the source of fossil electrons is observed; the population is invoked to match the data rather than detected directly.

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Cite this review

Pith. "Pith review of Multi-frequency Radio Observations of the Dissociative Cluster Merger CIZA J0107.7+5408." pith.science (2026). https://pith.science/paper/C4Q3ANQY

@misc{pith2026241215015,
  author       = {Pith},
  title        = {Pith review of: Multi-frequency Radio Observations of the Dissociative Cluster Merger CIZA J0107.7+5408},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/C4Q3ANQY}},
  note         = {Machine review of arXiv:2412.15015}
}
abstract

We present new radio observations of the galaxy cluster merger CIZA J0107.7+5408 (CIZA0107), a large, roughly equal mass, post-core passage, dissociative binary system at z = 0.1066. CIZA0107 is an elongated, disturbed system, hosting two subclusters with optical galaxy number density peaks offset from their associated X-ray density peaks and double-peaked diffuse radio structure. We present new 240-470 MHz and 2.0-4.0 GHz Very Large Array observations of CIZA0107. We image the diffuse emission at high resolution, constrain its integrated spectrum, and map the spectral index distribution. We confirm the presence of steep-spectrum ($\alpha$ $\sim$ -1.3) emission on a scale of about 0.5 Mpc in both subclusters. We identify two smaller ultra-steep spectrum ($\alpha$ $<$ -2) regions, superimposed on larger-scale radio emission associated with the southwestern subcluster. At 340 MHz, we detect a radio edge bounding the emission to the south and show that it is coincident with a weak (M $\sim$ 1.2) shock identified in the Chandra image. At 3 GHz, the emission does not show any corresponding edge-like feature, and in fact it extends beyond the shock. We investigate the nature of the emission in CIZA0107 and find that, while the system may host a double halo structure, we cannot rule out a scenario in which the emission arises from two relics projected on the central cluster regions.

Figures

Figures reproduced from arXiv: 2412.15015 by the authors.

Figure 1
Figure 1. A (top left): VLA 340 MHz A-configuration image with a 5.93” × 5.01” × -70◦ beam. B (top right): VLA 340 MHz B-configuration image with a 19.44” × 13.28” × 86◦ beam. C (bottom left): VLA 3 GHz C-configuration image with a 6.65” × 6.10” × -1◦ beam. D (bottom right): VLA 3 GHz D-configuration image with a 23.33” × 21.46” × 20◦ beam. Cyan stars mark the location of the subcluster BCGs. The physical scale is 1.95 kilopa… view at source ↗
Figure 2
Figure 2. A (top left): VLA 340 MHz B-configuration image with compact emission subtracted out, and a 18.98” × 13.01” × 87◦ beam. B (top right): VLA 3 GHz D-configuration image with compact emission subtracted out, and a 23.13” × 21.41” × 18◦ beam. C (bottom left): VLA 340 MHz B-configuration image with compact emission subtracted out, convolved to a 40” beam. Cyan contours trace the 74 MHz VLSSr emission, beginning at 3σ and… view at source ↗
Figure 3
Figure 3. A (left): Spectral index map between 340 MHz and 3 GHz. Contours from 340 MHz observations at B configuration convolved to a 40” beam are shown, beginning at 3σ and proceeding in integer multiples of √ 2. B (right): Spectral index error map, shown with the same contours from the 340 MHz observations [PITH_FULL_IMAGE:figures/full_fig_p009_3.png] view at source ↗
Figures from the paper (5 more)
Figure 4
Figure 4. Figure 4: Spectral separation image produced using a tech￾nique related to that of spectral tomography in order to highlight the flatter and steeper components in CIZA0107. The flatter emission is represented in blue, while the steeper emission is represented in orange. The yell…
Figure 6
Figure 6. Figure 6: A (top left): 160 ks, point-source-subtracted, exposure-corrected and background-subtracted Chandra X-ray image in the 0.5-7 keV band, binned by 10 pixels to a new pixel size of 4.92”. BCGs are marked with cyan stars. B (top right): the bin-10 pixel Chandra image, now …
Figure 7
Figure 7. Figure 7: The radio (blue, red) and X-ray (black) surface brightness profiles. The X-ray values were extracted using logarithmically-spaced bins with a minimum size of 1 pixel = 0.492”. The radio values plotted as points use radial bins as wide as FWHM ( 15” at 340 MHz and 24” a…
Figure 8
Figure 8. Figure 8: A (left): The 3 GHz point source-subtracted radio map, shown with the cells used for the point-to-point analysis. All cells were drawn within the 3σ contour and are beam-independent (25”×25” size). The BCGs are marked with cyan stars. B (right): IR − IX relation for th…
Figure 9
Figure 9. Figure 9: A (left): 340 MHz VLA observations at B-configuration with a beam of 19.44” × 13.28” × 86◦ , marked with all regions used in point source subtraction. To give a sense of the location of the radio structure, contours are displayed tracing the 340 MHz emission convolved …

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Works this paper leans on

101 extracted references · 8 canonical work pages

  1. [1]

    J., Ogrean , G

    Akamatsu , H., van Weeren , R. J., Ogrean , G. A., et al. 2015, , 582, A87, 10.1051/0004-6361/201425209

    doi:10.1051/0004-6361/201425209 2015

  2. [2]

    M., Sip o cz , B

    Astropy Collaboration , Price-Whelan , A. M., Sip o cz , B. M., et al. 2018, , 156, 123, 10.3847/1538-3881/aabc4f

    doi:10.3847/1538-3881/aabc4f 2018

  3. [3]

    Baars , J. W. M., Genzel , R., Pauliny-Toth , I. I. K., & Witzel , A. 1977, , 61, 99

    1977

  4. [4]

    2024, , 686, A5, 10.1051/0004-6361/202347965

    Balboni , M., Gastaldello , F., Bonafede , A., et al. 2024, , 686, A5, 10.1051/0004-6361/202347965

    doi:10.1051/0004-6361/202347965 2024

  5. [5]

    1987, , 154, 1, 10.1016/0370-1573(87)90134-7

    Blandford , R., & Eichler , D. 1987, , 154, 1, 10.1016/0370-1573(87)90134-7

    doi:10.1016/0370-1573(87)90134-7 1987

  6. [6]

    1999, Astroparticle Physics, 12, 169, 10.1016/S0927-6505(99)00079-1

    Blasi , P., & Colafrancesco , S. 1999, Astroparticle Physics, 12, 169, 10.1016/S0927-6505(99)00079-1

    doi:10.1016/s0927-6505(99)00079-1 1999

  7. [7]

    2010, , 18, 127, 10.1007/s00159-009-0023-3

    B \"o hringer , H., & Werner , N. 2010, , 18, 127, 10.1007/s00159-009-0023-3

    doi:10.1007/s00159-009-0023-3 2010

  8. [8]

    T., Br \"u ggen , M., et al

    Bonafede , A., Intema , H. T., Br \"u ggen , M., et al. 2014, , 785, 1, 10.1088/0004-637X/785/1/1

    doi:10.1088/0004-637x/785/1/1 2014

Show all 101 references
  1. [9]

    2022, , 933, 218, 10.3847/1538-4357/ac721d

    Bonafede , A., Brunetti , G., Rudnick , L., et al. 2022, , 933, 218, 10.3847/1538-4357/ac721d

    2022 doi

  2. [10]

    2020, , 634, A64, 10.1051/0004-6361/201936216

    Botteon , A., Brunetti , G., Ryu , D., & Roh , S. 2020, , 634, A64, 10.1051/0004-6361/201936216

    2020 doi

  3. [11]

    2016 a , , 460, L84, 10.1093/mnrasl/slw082

    Botteon , A., Gastaldello , F., Brunetti , G., & Dallacasa , D. 2016 a , , 460, L84, 10.1093/mnrasl/slw082

    2016 doi

  4. [12]

    2016 b , Galaxies, 4, 68, 10.3390/galaxies4040068

    ---. 2016 b , Galaxies, 4, 68, 10.3390/galaxies4040068

    2016 doi

  5. [13]

    2016 c , , 463, 1534, 10.1093/mnras/stw2089

    Botteon , A., Gastaldello , F., Brunetti , G., & Kale , R. 2016 c , , 463, 1534, 10.1093/mnras/stw2089

    2016 doi

  6. [14]

    W., Bonafede , A., et al

    Botteon , A., Shimwell , T. W., Bonafede , A., et al. 2018, , 478, 885, 10.1093/mnras/sty1102

    2018 doi

  7. [15]

    J., Eckert , D., et al

    Botteon , A., van Weeren , R. J., Eckert , D., et al. 2024, , 690, A222, 10.1051/0004-6361/202451293

    2024 doi

  8. [16]

    2011, , 412, 2, 10.1111/j.1365-2966.2010.17738.x

    Brown , S., & Rudnick , L. 2011, , 412, 2, 10.1111/j.1365-2966.2010.17738.x

    2011

  9. [17]

    Brunetti , G., Cappi , M., Setti , G., Feretti , L., & Harris , D. E. 2001 a , , 372, 755, 10.1051/0004-6361:20010484

    2001 doi

  10. [18]

    Brunetti , G., & Jones , T. W. 2014, International Journal of Modern Physics D, 23, 1430007, 10.1142/S0218271814300079

    2014 doi

  11. [19]

    2001 b , , 320, 365, 10.1046/j.1365-8711.2001.03978.x

    Brunetti , G., Setti , G., Feretti , L., & Giovannini , G. 2001 b , , 320, 365, 10.1046/j.1365-8711.2001.03978.x

    2001

  12. [20]

    G., Bonafede , A., Botteon , A., et al

    Campitiello , M. G., Bonafede , A., Botteon , A., et al. 2024, , 683, A9, 10.1051/0004-6361/202346591

    2024 doi

  13. [21]

    2014, , 783, 91, 10.1088/0004-637X/783/2/91

    Caprioli , D., & Spitkovsky , A. 2014, , 783, 91, 10.1088/0004-637X/783/2/91

    2014 doi

  14. [22]

    2022, , 134, 114501, 10.1088/1538-3873/ac9642

    CASA Team , Bean , B., Bhatnagar , S., et al. 2022, , 134, 114501, 10.1088/1538-3873/ac9642

    2022 doi

  15. [23]

    2013, , 777, 141, 10.1088/0004-637X/777/2/141

    Cassano , R., Ettori , S., Brunetti , G., et al. 2013, , 777, 141, 10.1088/0004-637X/777/2/141

    2013 doi

  16. [24]

    J., Cotton , W

    Condon , J. J., Cotton , W. D., Greisen , E. W., et al. 1998, , 115, 1693, 10.1086/300337

    1998 doi

  17. [25]

    Cornwell , T. J. 2008, IEEE Journal of Selected Topics in Signal Processing, 2, 793, 10.1109/JSTSP.2008.2006388

    2008

  18. [26]

    2013, Obit: Radio Astronomy Data Handling , Astrophysics Source Code Library, record ascl:1307.008

    Cotton , B. 2013, Obit: Radio Astronomy Data Handling , Astrophysics Source Code Library, record ascl:1307.008. 1307.008

    2013

  19. [27]

    2021, , 647, A51, 10.1051/0004-6361/202039208

    Cuciti , V., Cassano , R., Brunetti , G., et al. 2021, , 647, A51, 10.1051/0004-6361/202039208

    2021 doi

  20. [28]

    A., van Weeren , R

    de Gasperin , F., Ogrean , G. A., van Weeren , R. J., et al. 2015, , 448, 2197, 10.1093/mnras/stv129

    2015 doi

  21. [29]

    J., Br \"u ggen , M., et al

    de Gasperin , F., van Weeren , R. J., Br \"u ggen , M., et al. 2014, , 444, 3130, 10.1093/mnras/stu1658

    2014 doi

  22. [30]

    2022, , 659, A146, 10.1051/0004-6361/202142658

    de Gasperin , F., Rudnick , L., Finoguenov , A., et al. 2022, , 659, A146, 10.1051/0004-6361/202142658

    2022 doi

  23. [31]

    1980, , 239, L93, 10.1086/183300

    Dennison , B. 1980, , 239, L93, 10.1086/183300

    1980 doi

  24. [32]

    2018, , 620, A25, 10.1051/0004-6361/201832801

    Di Gennaro , G., Venturi , T., Dallacasa , D., et al. 2018, , 620, A25, 10.1051/0004-6361/201832801

    2018 doi

  25. [33]

    J., Rudnick , L., et al

    Di Gennaro , G., van Weeren , R. J., Rudnick , L., et al. 2021, , 911, 3, 10.3847/1538-4357/abe620

    2021 doi

  26. [34]

    2021, , 500, 795, 10.1093/mnras/staa3018

    Dominguez-Fernandez , P., Bruggen , M., Vazza , F., et al. 2021, , 500, 795, 10.1093/mnras/staa3018

    2021 doi

  27. [35]

    Dutta , S., Singh , V., Chandra , C. H. I., et al. 2023, , 944, 176, 10.3847/1538-4357/acaf01

    2023 doi

  28. [36]

    R., & Tully , R

    Ebeling , H., Mullis , C. R., & Tully , R. B. 2002, , 580, 774, 10.1086/343790

    2002 doi

  29. [37]

    2020, The Open Journal of Astrophysics, 3, 12, 10.21105/astro.2009.13944

    Eckert , D., Finoguenov , A., Ghirardini , V., et al. 2020, The Open Journal of Astrophysics, 3, 12, 10.21105/astro.2009.13944

    2020 arXiv

  30. [38]

    A., Biermann , P

    Ensslin , T. A., Biermann , P. L., Klein , U., & Kohle , S. 1998, , 332, 395, 10.48550/arXiv.astro-ph/9712293

    1998 doi arXiv

  31. [39]

    A., & Gopal-Krishna

    En lin , T. A., & Gopal-Krishna . 2001, , 366, 26, 10.1051/0004-6361:20000198

    2001 doi

  32. [40]

    2012, , 20, 54, 10.1007/s00159-012-0054-z

    Feretti , L., Giovannini , G., Govoni , F., & Murgia , M. 2012, , 20, 54, 10.1007/s00159-012-0054-z

    2012 doi

  33. [41]

    1949, Physical Review, 75, 1169, 10.1103/PhysRev.75.1169

    Fermi , E. 1949, Physical Review, 75, 1169, 10.1103/PhysRev.75.1169

    1949 doi

  34. [42]

    W., Jee , M

    Finner , K., Randall , S. W., Jee , M. J., et al. 2023, , 942, 23, 10.3847/1538-4357/ac9fd3

    2023 doi

  35. [43]

    1982, , 20, 547, 10.1146/annurev.aa.20.090182.002555

    Forman , W., & Jones , C. 1982, , 20, 547, 10.1146/annurev.aa.20.090182.002555

    1982

  36. [44]

    2008, , 486, 347, 10.1051/0004-6361:200809459

    Giacintucci , S., Venturi , T., Macario , G., et al. 2008, , 486, 347, 10.1051/0004-6361:200809459

    2008 doi

  37. [45]

    A., Feretti , L., & Giovannini , G

    Govoni , F., En lin , T. A., Feretti , L., & Giovannini , G. 2001 a , , 369, 441, 10.1051/0004-6361:20010115

    2001 doi

  38. [46]

    2001 b , , 376, 803, 10.1051/0004-6361:20011016

    Govoni , F., Feretti , L., Giovannini , G., et al. 2001 b , , 376, 803, 10.1051/0004-6361:20011016

    2001 doi

  39. [47]

    Greisen , E. W. 2003, in Astrophysics and Space Science Library, Vol. 285, Information Handling in Astronomy - Historical Vistas, ed. A. Heck , 109, 10.1007/0-306-48080-8_7

    2003 doi

  40. [48]

    N., Shimwell , T

    Hoang , D. N., Shimwell , T. W., van Weeren , R. J., et al. 2018, , 478, 2218, 10.1093/mnras/sty1123

    2018 doi

  41. [49]

    2007, , 375, 77, 10.1111/j.1365-2966.2006.11111.x

    Hoeft , M., & Br \"u ggen , M. 2007, , 375, 77, 10.1111/j.1365-2966.2006.11111.x

    2007

  42. [50]

    2023, , 680, A31, 10.1051/0004-6361/202245102

    Jones , A., de Gasperin , F., Cuciti , V., et al. 2023, , 680, A31, 10.1051/0004-6361/202245102

    2023 doi

  43. [51]

    Kale , R., & Dwarakanath , K. S. 2012, , 744, 46, 10.1088/0004-637X/744/1/46

    2012 doi

  44. [52]

    Kang , H., Ryu , D., & Jones , T. W. 2012, , 756, 97, 10.1088/0004-637X/756/1/97

    2012 doi

  45. [53]

    M., & Rudnick , L

    Katz-Stone , D. M., & Rudnick , L. 1997, , 488, 146, 10.1086/304661

    1997 doi

  46. [54]

    M., Rudnick , L., & Anderson , M

    Katz-Stone , D. M., Rudnick , L., & Anderson , M. C. 1993, , 407, 549, 10.1086/172536

    1993 doi

  47. [55]

    Kelly , B. C. 2007, , 665, 1489, 10.1086/519947

    2007 doi

  48. [56]

    C., Blanton , E

    Kempner , J. C., Blanton , E. L., Clarke , T. E., et al. 2004, in The Riddle of Cooling Flows in Galaxies and Clusters of galaxies, ed. T. Reiprich , J. Kempner , & N. Soker , 335, 10.48550/arXiv.astro-ph/0310263

    2004 doi arXiv

  49. [57]

    D., Ebeling, H., & Mullis, C

    Kocevski, D. D., Ebeling, H., & Mullis, C. R. 2003, Clusters in the Zone of Avoidance. astro-ph/0304453

    2003 arXiv

  50. [58]

    V., & Borgani, S

    Kravtsov, A. V., & Borgani, S. 2012, Annual Review of Astronomy and Astrophysics, 50, 353, 10.1146/annurev-astro-081811-125502

    2012 doi

  51. [59]

    D., & Lifshitz , E

    Landau , L. D., & Lifshitz , E. M. 1959, Fluid mechanics

    1959

  52. [60]

    M., Cotton , W

    Lane , W. M., Cotton , W. D., van Velzen , S., et al. 2014, , 440, 327, 10.1093/mnras/stu256

    2014 doi

  53. [61]

    2024, , 686, A55, 10.1051/0004-6361/202348194

    Lee , W., Pillepich , A., ZuHone , J., et al. 2024, , 686, A55, 10.1051/0004-6361/202348194

    2024 doi

  54. [62]

    T., van Weeren , R

    Mandal , S., Intema , H. T., van Weeren , R. J., et al. 2020, , 634, A4, 10.1051/0004-6361/201936560

    2020 doi

  55. [64]

    2005 b , , 627, 733, 10.1086/430695

    ---. 2005 b , , 627, 733, 10.1086/430695

    2005 doi

  56. [65]

    2007, Physics Reports, 443, 1, 10.1016/j.physrep.2007.01.001

    Markevitch, M., & Vikhlinin, A. 2007, Physics Reports, 443, 1, 10.1016/j.physrep.2007.01.001

    2007 doi

  57. [66]

    2022, , 516, 5289, 10.1093/mnras/stac2276

    McDonald , W., Obreschkow , D., & Garratt-Smithson , L. 2022, , 516, 5289, 10.1093/mnras/stac2276

    2022 doi

  58. [67]

    2015, PyBDSF: Python Blob Detection and Source Finder , Astrophysics Source Code Library, record ascl:1502.007

    Mohan , N., & Rafferty , D. 2015, PyBDSF: Python Blob Detection and Source Finder , Astrophysics Source Code Library, record ascl:1502.007. 1502.007

    2015

  59. [68]

    2010, , 509, A86, 10.1051/0004-6361/200913414

    Murgia , M., Govoni , F., Feretti , L., & Giovannini , G. 2010, , 509, A86, 10.1051/0004-6361/200913414

    2010 doi

  60. [69]

    R., Mack , K

    Murgia , M., Parma , P., de Ruiter , H. R., Mack , K. H., & Fanti , R. 2005, in X-Ray and Radio Connections, ed. L. O. Sjouwerman & K. K. Dyer , 8.15, 10.48550/arXiv.astro-ph/0405091

    2005 doi arXiv

  61. [70]

    2024 a , P-band CASA Guide 5.0

    National Radio Astronomy Observatory (NRAO) . 2024 a , P-band CASA Guide 5.0. https://casaguides.nrao.edu/index.php?title=CASA_Guides:P-band_casa_guide_5.0

    2024

  62. [71]

    2024 b , Flux Density Scale

    ---. 2024 b , Flux Density Scale. https://science.nrao.edu/facilities/vla/docs/manuals/oss/performance/fdscale

    2024

  63. [72]

    R., McKinley , B., Hurley-Walker , N., et al

    Offringa , A. R., McKinley , B., Hurley-Walker , N., et al. 2014, , 444, 606, 10.1093/mnras/stu1368

    2014 doi

  64. [73]

    Pal , A., Kale , R., Wang , Q. H. S., & Wik , D. R. 2024, arXiv e-prints, arXiv:2411.15480, 10.48550/arXiv.2411.15480

    2024 doi arXiv

  65. [74]

    2021, Astronomische Nachrichten, 342, 1166, 10.1002/asna.20210078

    Patil , P., Whittle , M., Nyland , K., et al. 2021, Astronomische Nachrichten, 342, 1166, 10.1002/asna.20210078

    2021 doi

  66. [75]

    2022, , 934, 26, 10.3847/1538-4357/ac71b0

    ---. 2022, , 934, 26, 10.3847/1538-4357/ac71b0

    2022 doi

  67. [76]

    Pearce , C. J. J., van Weeren , R. J., Andrade-Santos , F., et al. 2017, , 845, 81, 10.3847/1538-4357/aa7e2f

    2017 doi

  68. [77]

    A., & Butler , B

    Perley , R. A., & Butler , B. J. 2017, , 230, 7, 10.3847/1538-4365/aa6df9

    2017 doi

  69. [78]

    2001, , 557, 560, 10.1086/321557

    Petrosian , V. 2001, , 557, 560, 10.1086/321557

    2001 doi

  70. [79]

    Pfrommer , C., & En lin , T. A. 2004, Journal of Korean Astronomical Society, 37, 455, 10.5303/JKAS.2004.37.5.455

    2004 doi

  71. [80]

    P., & Pfrommer , C

    Pinzke , A., Oh , S. P., & Pfrommer , C. 2013, , 435, 1061, 10.1093/mnras/stt1308

    2013 doi

  72. [81]

    2020, , 641, A6, 10.1051/0004-6361/201833910

    Planck Collaboration , Aghanim , N., Akrami , Y., et al. 2020, , 641, A6, 10.1051/0004-6361/201833910

    2020 doi

  73. [82]

    2009, Monthly Notices of the Royal Astronomical Society, 399, 410, 10.1111/j.1365-2966.2009.15290.x

    Planelles, S., & Quilis, V. 2009, Monthly Notices of the Royal Astronomical Society, 399, 410, 10.1111/j.1365-2966.2009.15290.x

    2009

  74. [83]

    J., et al

    Rajpurohit , K., Hoeft , M., van Weeren , R. J., et al. 2018, , 852, 65, 10.3847/1538-4357/aa9f13

    2018 doi

  75. [84]

    2020, , 642, L13, 10.1051/0004-6361/202039165

    Rajpurohit , K., Vazza , F., Hoeft , M., et al. 2020, , 642, L13, 10.1051/0004-6361/202039165

    2020 doi

  76. [85]

    2023, , 669, A1, 10.1051/0004-6361/202244925

    Rajpurohit , K., Osinga , E., Brienza , M., et al. 2023, , 669, A1, 10.1051/0004-6361/202244925

    2023 doi

  77. [86]

    W., Clarke, T

    Randall, S. W., Clarke, T. E., van Weeren, R. J., et al. 2016, The Astrophysical Journal, 823, 94, 10.3847/0004-637x/823/2/94

    2016 doi

  78. [87]

    Sarazin , C. L. 1988, X-ray emission from clusters of galaxies

    1988

  79. [88]

    Sarazin , C. L. 2002, in Astrophysics and Space Science Library, Vol. 272, Merging Processes in Galaxy Clusters, ed. L. Feretti , I. M. Gioia , & G. Giovannini , 1--38, 10.1007/0-306-48096-4_1

    2002 doi

  80. [89]

    L., & Kempner , J

    Sarazin , C. L., & Kempner , J. C. 2000, , 533, 73, 10.1086/308649

    2000 doi

  81. [90]

    2022, , 935, L23, 10.3847/2041-8213/ac86d4

    Sarkar , A., Randall , S., Su , Y., et al. 2022, , 935, L23, 10.3847/2041-8213/ac86d4

    2022 doi

  82. [91]

    W., Brown , S., Feain , I

    Shimwell , T. W., Brown , S., Feain , I. J., et al. 2014, , 440, 2901, 10.1093/mnras/stu467

    2014 doi

  83. [92]

    Taylor , M. B. 2005, in Astronomical Society of the Pacific Conference Series, Vol. 347, Astronomical Data Analysis Software and Systems XIV, ed. P. Shopbell , M. Britton , & R. Ebert , 29

    2005

  84. [93]

    2004, , 350, 1397, 10.1111/j.1365-2966.2004.07736.x

    Tormen , G., Moscardini , L., & Yoshida , N. 2004, , 350, 1397, 10.1111/j.1365-2966.2004.07736.x

    2004

  85. [94]

    2020, , 890, 148, 10.3847/1538-4357/ab6bca

    Umetsu , K., Sereno , M., Lieu , M., et al. 2020, , 890, 148, 10.3847/1538-4357/ab6bca

    2020 doi

  86. [95]

    u ggen , M., R \

    van Weeren , R. J., Br \"u ggen , M., R \"o ttgering , H. J. A., & Hoeft , M. 2011 a , Journal of Astrophysics and Astronomy, 32, 505, 10.1007/s12036-011-9108-2

    2011 doi

  87. [96]

    u ggen , M., R \

    van Weeren , R. J., Br \"u ggen , M., R \"o ttgering , H. J. A., et al. 2011 b , , 533, A35, 10.1051/0004-6361/201117149

    2011 doi

  88. [98]

    J., de Gasperin, F., Akamatsu, H., et al

    van Weeren, R. J., de Gasperin, F., Akamatsu, H., et al. 2019, Space Science Reviews, 215, 10.1007/s11214-019-0584-z

    2019 doi

  89. [99]

    o ttgering , H. J. A., & Br \

    van Weeren , R. J., R \"o ttgering , H. J. A., & Br \"u ggen , M. 2011 c , , 527, A114, 10.1051/0004-6361/201015991

    2011 doi

  90. [100]

    J., Brunetti , G., Br \"u ggen , M., et al

    van Weeren , R. J., Brunetti , G., Br \"u ggen , M., et al. 2016, , 818, 204, 10.3847/0004-637X/818/2/204

    2016 doi

  91. [101]

    J., Andrade-Santos , F., Dawson , W

    van Weeren , R. J., Andrade-Santos , F., Dawson , W. A., et al. 2017, Nature Astronomy, 1, 0005, 10.1038/s41550-016-0005

    2017 doi

  92. [102]

    Wang , Q. H. S., Giacintucci , S., & Markevitch , M. 2018, , 856, 162, 10.3847/1538-4357/aab2aa

    2018 doi

  93. [103]

    2012, The Merger Dynamics of the X-Ray-Emitting Plasma in Clusters of Galaxies (Springer Nature Singapore), 1–44, 10.1007/978-981-16-4544-0_124-1

    ZuHone, J., & Su, Y. 2012, The Merger Dynamics of the X-Ray-Emitting Plasma in Clusters of Galaxies (Springer Nature Singapore), 1–44, 10.1007/978-981-16-4544-0_124-1

    2012 doi

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