pith. sign in

arxiv: 2606.25730 · v1 · pith:FZO7GL6Wnew · submitted 2026-06-24 · 🌌 astro-ph.CO

The SKA View of Cool-core Clusters: Evolution of Radio Mini-halos and AGN Feedback

Myriam Gitti , Paolo Tozzi , Francesco Ubertosi , Annalisa Bonafede , Gianfranco Brunetti , Rossella Cassano , Stefano Ettori , Luigina Feretti
show 7 more authors
Marie-Lou Gendron-Marsolais Simona Giacintucci Julie Hlavacek-Larrondo Alessandro Ignesti Giulia Macario Mamta Pandey-Pommier Tiziana Venturi
This is my paper

Pith reviewed 2026-06-25 20:12 UTC · model grok-4.3

classification 🌌 astro-ph.CO
keywords cool-core clustersradio mini-halosAGN feedbackbrightest cluster galaxiesintra-cluster mediumnon-thermal emissionSKA surveysgalaxy cluster evolution
0
0 comments X

The pith

All-sky SKA-Mid surveys could detect up to 3500 radio mini-halos in cool-core clusters at z<1.

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

The paper focuses on radio-mode feedback in relaxed cool-core galaxy clusters, where the central AGN in the brightest cluster galaxy launches jets and lobes that interact with the hot intra-cluster gas. This interaction often produces cavities visible in X-rays and is accompanied by diffuse radio mini-halos on scales matching the cooling radius. The authors calculate that current luminosity functions applied to existing samples imply SKA-Mid all-sky surveys at arcsecond resolution could increase the known mini-halo population from tens to around 3500 objects below redshift 1. Deeper tiered observations at sub-arcsecond resolution would also complete the census of radio-loud BCGs down to low powers out to redshift 2. Such samples would directly link mini-halo properties to the thermal and dynamical state of cluster cores.

Core claim

In roughly 70 percent of cool-core clusters the central AGN is radio-loud and its relativistic plasma fills X-ray cavities while driving turbulence that can generate extended radio mini-halos. The central claim is that SKA-Mid all-sky surveys at arcsecond resolution have the potential to detect up to about 3500 mini-halos at z<1, while deep tier surveys at sub-arcsecond resolution would enable a complete census of radio-loud BCGs down to 1.4 GHz powers of 10^23 W/Hz up to z~2, yielding a comprehensive view of AGN feedback.

What carries the argument

Radio mini-halos, defined as diffuse non-thermal emission surrounding the radio-loud BCG on scales comparable to the cooling radius, whose statistics are extrapolated from current samples using luminosity functions.

If this is right

  • A sample of thousands of mini-halos would clarify their origin and connection to the thermal and dynamical properties of cluster cores.
  • A complete census of radio-loud BCGs to z~2 would map how AGN feedback operates across cosmic time.
  • The resulting statistics would support future high-resolution X-ray studies of cluster cores by providing a large radio-selected parent sample.
  • The data would reveal the role of AGN feedback in regulating gas cooling and shaping large-scale structure.

Where Pith is reading between the lines

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

  • If the predicted numbers are confirmed, it would test whether mini-halo formation efficiency remains roughly constant over the last 8 billion years.
  • The same surveys would also constrain how often radio-loud BCGs appear in non-cool-core clusters, testing the link between mini-halos and core relaxation.
  • Comparison of the new radio sample with X-ray cavity statistics could quantify the fraction of mechanical AGN power that goes into turbulence versus direct heating.

Load-bearing premise

The number of detectable mini-halos scales directly from the small existing sample using current luminosity functions with no strong redshift evolution in mini-halo properties or occurrence rates.

What would settle it

An SKA survey that finds far fewer than several thousand mini-halos at z<1 or that shows clear redshift evolution in mini-halo occurrence or luminosity would falsify the stated detection potential.

Figures

Figures reproduced from arXiv: 2606.25730 by Alessandro Ignesti, Annalisa Bonafede, Francesco Ubertosi, Gianfranco Brunetti, Giulia Macario, Julie Hlavacek-Larrondo, Luigina Feretti, Mamta Pandey-Pommier, Marie-Lou Gendron-Marsolais, Myriam Gitti, Paolo Tozzi, Rossella Cassano, Simona Giacintucci, Stefano Ettori, Tiziana Venturi.

Figure 1
Figure 1. Figure 1: The X-ray Chandra image (residual after 𝛽-model subtraction) of the galaxy cluster RBS 797 at 𝑧 = 0.35 (Ubertosi et al., 2021) is shown in color scale with superimposed VLA contours at 1.4 GHz (green, Gitti et al., 2006) and at 3 GHz (white, Ubertosi et al., 2024a). Contours levels start at 3×rms (rms ∼13 𝜇Jy/beam at 1.4 GHz and 5 𝜇Jy/beam at 3 GHz; beam ∼ 3 ′′ at 1.4 GHz and 0.9′′ at 3 GHz), and increase … view at source ↗
Figure 2
Figure 2. Figure 2: Left panel: Mini-halo radio power at 1.4 GHz versus the cluster X-ray luminosity inside a radius of 600 kpc for the mini-halo sample of Richard-Laferrière et al. (2020). The best-fitting line using the BCES-orthogonal method (Akritas and Bershady, 1996), which is calculated including also candidate and uncertain mini-halos, is displayed (black solid line) along with the 95% confidence region (orange shaded… view at source ↗
Figure 3
Figure 3. Figure 3: Left panel: Chandra image of the cluster RBS 797 (z=0.35, 1 ′′ ∼ 5 kpc) with the contours of the mini-halo radio emission (in green, starting at 0.035 mJy/beam and increasing by a factor of 2, beam ∼ 3 ′′ , Doria et al., 2012) and radio-loud BCG (in black, starting at 0.03 mJy/beam and increasing by a factor of 2, beam ∼1.3′′ , Gitti et al., 2013). Shown in white is an example of the mesh for the point-to-… view at source ↗
Figure 4
Figure 4. Figure 4: Left y-axis (blue): The blue solid line shows the 1.4 GHz luminos￾ity corresponding to a detection limit of 1 Jy (defined as 5× rms noise), which will be reached by SKA-Mid Deep Tier sur￾veys (see Tab. 1). The blue horizontal dashed line indicates the minimum lumi￾nosity currently measured in radio galax￾ies hosted in local CC clusters. Right y-axis (red): The red solid line shows the expected surface brig… view at source ↗
read the original abstract

In about 70 per cent of relaxed, cool-core galaxy clusters, the brightest cluster galaxy (BCG) is radio loud, showing non-thermal radio jets and lobes ejected by the central active galactic nucleus (AGN). In recent years such relativistic plasma has been shown to interact with the surrounding thermal intra-cluster medium (ICM) as revealed by striking images where radio lobe fill the cavities in the X-ray-emitting gas. This "radio-mode feedback" phenomenon is widespread and crucial for understanding the physics of cluster cores and the properties of the central BCG. Mechanically-powerful AGN are expected to drive turbulence in the central ICM which may also contribute to the origin of non-thermal emission on cluster-scales. Diffuse non-thermal emission has been observed in many cool-core clusters in the form of a radio mini-halo surrounding the radio-loud BCG on scales comparable to the cooling radius. Large samples of mini-halos are essential to clarify their origin and their link with the thermal and dynamical properties of clusters, especially in view of future high-resolution X-ray studies with NewAthena X-IFU. All-sky surveys with the SKA-Mid telescope at arcsecond resolution would have the potential to detect up to about 3500 mini-halos at redshift z<1 (compared to the few tens currently known). Deep Tier surveys with the SKA-Mid at sub-arcsecond resolution would further enable a complete census of radio-loud BCGs down to 1.4 GHz powers of 10^23 W/Hz up to z~2. This will provide a comprehensive view of AGN feedback and its role in shaping large scale structures.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 0 minor

Summary. The manuscript reviews radio-mode AGN feedback in cool-core clusters, where radio jets from the BCG interact with the ICM to create cavities and potentially drive turbulence leading to radio mini-halos on scales comparable to the cooling radius. It argues that large mini-halo samples are needed to clarify their origin and connection to cluster properties ahead of NewAthena X-IFU observations, and forecasts that all-sky SKA-Mid surveys at arcsecond resolution could detect up to ~3500 mini-halos at z<1 (versus the few tens known today), while deep Tier surveys at sub-arcsecond resolution would enable a complete census of radio-loud BCGs down to 1.4 GHz powers of 10^23 W/Hz out to z~2.

Significance. If the detection forecasts hold, the work would highlight how SKA surveys can deliver order-of-magnitude increases in mini-halo statistics, enabling statistical studies of their link to thermal and dynamical cluster properties and providing a comprehensive view of AGN feedback's role in structure formation.

major comments (2)
  1. [Abstract] Abstract: the central forecast of up to ~3500 detectable mini-halos at z<1 is obtained by scaling the current small sample using existing luminosity functions, yet no explicit luminosity function, derivation steps, assumed parameters, or error ranges on the extrapolation are supplied, leaving the numerical claim without visible support.
  2. [Abstract] Abstract: the scaling implicitly assumes no strong redshift evolution in mini-halo occurrence rates or luminosity-function shape beyond the current low-z, X-ray-selected sample, but the manuscript provides no test, justification, or sensitivity analysis of this assumption against higher-redshift data.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the detailed and constructive report. The two major comments both concern the level of detail and justification provided for the mini-halo detection forecast in the abstract. We address each point below and will revise the manuscript to improve transparency.

read point-by-point responses

  1. Referee: [Abstract] Abstract: the central forecast of up to ~3500 detectable mini-halos at z<1 is obtained by scaling the current small sample using existing luminosity functions, yet no explicit luminosity function, derivation steps, assumed parameters, or error ranges on the extrapolation are supplied, leaving the numerical claim without visible support.

    Authors: We agree that the abstract states the numerical forecast without sufficient supporting information. The full manuscript derives the estimate from published mini-halo luminosity functions and the known cool-core fraction, but these steps are not summarized in the abstract. In the revised version we will add a concise description of the adopted luminosity function, the scaling procedure, key parameters (e.g., flux limit, redshift range), and an indicative uncertainty range, while retaining the abstract length limit. revision: yes

  2. Referee: [Abstract] Abstract: the scaling implicitly assumes no strong redshift evolution in mini-halo occurrence rates or luminosity-function shape beyond the current low-z, X-ray-selected sample, but the manuscript provides no test, justification, or sensitivity analysis of this assumption against higher-redshift data.

    Authors: The forecast is anchored to the existing low-redshift, X-ray-selected sample because higher-redshift mini-halos remain observationally scarce. We acknowledge that the abstract does not discuss possible redshift evolution or provide a sensitivity test. In revision we will insert a short paragraph (or footnote) that (i) states the no-evolution assumption explicitly, (ii) notes the current lack of high-z constraints, and (iii) reports the effect on the predicted number if a modest positive or negative evolution is assumed, using the limited existing higher-z upper limits. revision: yes

Circularity Check

0 steps flagged

Detection forecasts are direct extrapolations from observed samples with no self-referential reduction

full rationale

The paper's central claim of detecting up to ~3500 mini-halos is an order-of-magnitude scaling from the known sample of a few tens, using existing luminosity functions and an explicit assumption of limited redshift evolution. No equations, fitted parameters, or derivations are presented that would make this number equivalent to its inputs by construction. No self-citations are invoked as load-bearing uniqueness theorems or ansatzes for the forecast. The estimates remain externally falsifiable against future observations and do not reduce to prior fitted values within the paper itself.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

Abstract-only review provides no explicit free parameters, axioms, or invented entities; the 3500 estimate implicitly rests on unstated extrapolations from the current small sample of mini-halos whose details cannot be audited here.

pith-pipeline@v0.9.1-grok · 5911 in / 1325 out tokens · 34470 ms · 2026-06-25T20:12:51.058201+00:00 · methodology

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

88 extracted references · 47 canonical work pages · 2 internal anchors

  1. [1]

    doi: 10.1086/177901. C. S. Anderson et al.ApJ, 937(1):45, Sept

    doi:10.1086/177901

  2. [2]

    doi: 10.3847/1538-4357/ac7ec0. F. Andrade-Santos et al.ApJ, 843(1):76, July

    work page doi:10.3847/1538-4357/ac7ec0

  3. [3]

    doi: 10.3847/1538-4357/aa7461. S. Andreon et al.MNRAS, 522(3):4301–4309, July

    doi:10.3847/1538-4357/aa7461

  4. [4]

    doi: 10.1093/mnras/stad1270. Y. Ascasibar and M. Markevitch.ApJ, 650:102–127, Oct

    work page doi:10.1093/mnras/stad1270

  5. [5]

    doi: 10.1086/506508. P. N. Best et al.MNRAS, 379:894–908, Aug

    doi:10.1086/506508

  6. [6]

    doi: 10.1111/j.1365-2966.2007.11937.x. N. Biava et al.MNRAS, 508(3):3995–4007, Dec

    work page doi:10.1111/j.1365-2966.2007.11937.x 2007

  7. [7]

    doi: 10.1093/mnras/stab2840. N. Biava et al.A&A, 686:A82, June

    work page doi:10.1093/mnras/stab2840

  8. [8]

    doi: 10.1051/0004-6361/202348045. L. Bîrzan et al.ApJ, 607:800–809, June

    work page doi:10.1051/0004-6361/202348045

  9. [9]

    doi: 10.1086/383519. L. Bîrzan et al.ApJ, 686:859–880, Oct

    work page doi:10.1086/383519

  10. [10]

    doi: 10.1086/591416. A. Bonafede et al.A&A, 680:A5, Dec

    work page doi:10.1086/591416

  11. [11]

    R.Braunetal.arXive-prints,art.arXiv:1912.12699,Dec.2019

    doi: 10.1051/0004-6361/202347567. R.Braunetal.arXive-prints,art.arXiv:1912.12699,Dec.2019. doi: 10.48550/arXiv.1912.12699. L.Bravi,M.Gitti,andG.Brunetti.MNRAS,455:L41–L45,Jan.2016. doi: 10.1093/mnrasl/slv137. G. Brunetti and T. W. Jones.International Journal of Modern Physics D, 23:1430007, Mar

    work page doi:10.1051/0004-6361/202347567 1912

  12. [12]

    doi: 10.1142/S0218271814300079. J. O. Burns.AJ, 99:14–30, Jan

    work page doi:10.1142/s0218271814300079

  13. [13]

    doi: 10.1086/115307. C. L. Carilli et al.ApJ, 928(1):59, Mar

    doi:10.1086/115307

  14. [14]

    R.Cassano, M.Gitti, andG.Brunetti.A&A,486:L31–L34, Aug.2008b

    doi: 10.3847/1538-4357/ac55a0. R.Cassano, M.Gitti, andG.Brunetti.A&A,486:L31–L34, Aug.2008b. doi: 10.1051/0004-6361: 200810179. R.Cassanoetal.Radiohalosingalaxyclustersasunveiledbytheskatelescope.InAdvancingAstro- physicswiththeSKA–II(AASKAII).2026. arXivsearch: ReportnumberAASKAII/Cassano01. M. Chiaberge et al.ApJ, 710:L107–L110, Feb

    doi:10.3847/1538-4357/ac55a0 2026

  15. [15]

    doi: 10.1088/2041-8205/710/2/L107. D. J. Croton et al.MNRAS, 365:11–28, Jan

    work page doi:10.1088/2041-8205/710/2/l107 2041

  16. [16]

    doi: 10.1111/j.1365-2966.2005.09675.x. M. Cruise et al.Nature Astronomy, 9:36–44, Jan

    work page doi:10.1111/j.1365-2966.2005.09675.x 2005

  17. [17]

    doi: 10.1038/s41550-024-02416-3. T. J. Dennis and B. D. G. Chandran.ApJ, 622:205–216, Mar

    work page doi:10.1038/s41550-024-02416-3

  18. [18]

    doi: 10.1086/427424. M. Donahue and G. M. Voit.Phys. Rep., 973:1–109, Aug

    work page doi:10.1086/427424

  19. [19]

    doi: 10.1016/j.physrep.2022.04

    work page doi:10.1016/j.physrep.2022.04 2022

  20. [20]

    16 The SKA View of Cool-core Clusters M

    doi: 10.1088/0004-637X/753/1/47. 16 The SKA View of Cool-core Clusters M. Gitti R. J. H. Dunn and A. C. Fabian.MNRAS, 373:959–971, Dec

    work page doi:10.1088/0004-637x/753/1/47

  21. [22]

    doi: 10.3390/universe7050142. A. C. Fabian.ARA&A, 32:277–318,

    work page doi:10.3390/universe7050142

  22. [23]

    doi: 10.1146/annurev.aa.32.090194.001425. A. C. Fabian.ARA&A, 50:455–489, Sept

    work page doi:10.1146/annurev.aa.32.090194.001425

  23. [24]

    doi: 10.1146/annurev-astro-081811-125521. B. L. Fanaroff and J. M. Riley.MNRAS, 167:31P–36P, May

    work page internal anchor Pith review doi:10.1146/annurev-astro-081811-125521

  24. [25]

    doi: 10.1088/0004-637X/746/1/53. Y. Fujita, T. Matsumoto, and K. Wada.JKAS, 37:571–574, Dec

    doi:10.1088/0004-637x/746/1/53

  25. [26]

    2012.21704.x

    M.Gaspari,F.Brighenti,andP.Temi.MNRAS,424:190–209,July2012.doi: 10.1111/j.1365-2966. 2012.21183.x. M. Gaspari, F. Brighenti, and M. Ruszkowski.Astronomische Nachrichten, 334(4-5):394, Apr

    work page doi:10.1111/j.1365-2966 2012

  26. [27]

    doi: 10.1002/asna.201211865. S. Giacintucci et al.ApJ, 841:71, June

    doi:10.1002/asna.201211865

  27. [28]

    doi: 10.3847/1538-4357/aa7069. S. Giacintucci et al.ApJ, 880(2):70, Aug

    doi:10.3847/1538-4357/aa7069

  28. [29]

    doi: 10.3847/1538-4357/ab29f1. M. Gitti, G. Brunetti, and G. Setti.A&A, 386:456–463, May

    work page doi:10.3847/1538-4357/ab29f1

  29. [31]

    doi: 10.1051/0004-6361: 20053998. M. Gitti, C. Ferrari, W. Domainko, and et al.A&A, 470:L25–L28, Aug

    doi:10.1051/0004-6361:

  30. [32]

    doi: 10.1051/ 0004-6361:20077658. M. Gitti, F. Brighenti, and B. R. McNamara.Advances in Astronomy, 2012:950641,

    2012

  31. [33]

    doi: 10.1155/2012/950641. M. Gitti et al.A&A, 557:L14, Sept

    doi:10.1155/2012/950641 2012

  32. [34]

    doi: 10.1051/0004-6361/201322401. M. Gitti, P. Tozzi, G. Brunetti, and et al.PoS(AASKA14)076, art. 76,

    work page doi:10.1051/0004-6361/201322401

  33. [35]

    doi: 10.1093/mnras/stu1725. S. Heinz and E. Churazov.ApJ, 634(2):L141–L144, Dec

    doi:10.1093/mnras/stu1725

  34. [36]

    17 The SKA View of Cool-core Clusters M

    doi: 10.1086/498301. 17 The SKA View of Cool-core Clusters M. Gitti S. Heinz, M. Brüggen, A. Young, and E. Levesque.MNRAS, 373:L65–L69, Nov

    doi:10.1086/498301

  35. [37]

    doi: 10.1111/j.1745-3933.2006.00243.x. e. a. Hitomi Collaboration.Nature, 535:117–121, July

    doi:10.1111/j.1745-3933.2006.00243.x 2006

  36. [38]

    doi: 10.1038/nature18627. e. a. Hitomi Collaboration.ArXiv e-prints, Nov

    doi:10.1038/nature18627

  37. [39]

    doi: 10.1111/j.1365-2966.2011. 20405.x. J. Hlavacek-Larrondo et al.ApJ, 805(1):35, May

    work page doi:10.1111/j.1365-2966.2011 2011

  38. [40]

    doi: 10.1088/0004-637X/805/1/35. J. Hlavacek-Larrondo et al.ApJ, 898(2):L50, Aug

    doi:10.1088/0004-637x/805/1/35

  39. [41]

    doi: 10.3847/2041-8213/ab9ca5. J. Hlavacek-Larrondo et al.ApJ, 987(2):L40, July

    work page doi:10.3847/2041-8213/ab9ca5 2041

  40. [42]

    doi: 10.3847/2041-8213/add527. M. T. Hogan et al.MNRAS, 453(2):1201–1222, Oct

    work page doi:10.3847/2041-8213/add527 2041

  41. [43]

    doi: 10.1093/mnras/stv1517. D. S. Hudson, R. Mittal, T. H. Reiprich, and et al.A&A, 513:A37, Apr

    doi:10.1093/mnras/stv1517

  42. [44]

    doi: 10.1093/mnras/stx132. R. Kale et al.A&A, 557:A99, Sept

    work page doi:10.1093/mnras/stx132

  43. [45]

    doi: 10.1051/0004-6361/201321515. M. Koss et al.arXiv e-prints, art. arXiv:2511.00253, Oct

    work page doi:10.1051/0004-6361/201321515

  44. [46]

    doi: 10.48550/arXiv.2511.00253. M. Lepore et al.A&A, 682:A186, Feb

    work page doi:10.48550/arxiv.2511.00253

  45. [47]

    doi: 10.1051/0004-6361/202347538. G. Lusetti et al.A&A, 683:A132, Mar

    work page doi:10.1051/0004-6361/202347538

  46. [48]

    doi: 10.1051/0004-6361/202347635. A. B. Mantz et al.MNRAS, 496(2):1554–1564, Aug

    doi:10.1051/0004-6361/202347635

  47. [49]

    doi: 10.1093/mnras/staa1581. M. Markevitch and A. Vikhlinin.Phys. Rep., 443:1–53, May

    work page doi:10.1093/mnras/staa1581

  48. [50]

    doi: 10.1016/j.physrep.2007. 01.001. P. Mazzotta and S. Giacintucci.ApJ, 675:L9–L12, Mar

    doi:10.1016/j.physrep.2007 2007

  49. [51]

    doi: 10.1086/529433. M. McDonald et al.ApJ, 774:23, Sept

    work page doi:10.1086/529433

  50. [52]

    M.McDonald,M.Gaspari,B.R.McNamara,andG.R.Tremblay.ApJ,858(1):45,May2018

    doi: 10.1088/0004-637X/774/1/23. M.McDonald,M.Gaspari,B.R.McNamara,andG.R.Tremblay.ApJ,858(1):45,May2018. doi: 10.3847/1538-4357/aabace. B. R. McNamara and P. E. J. Nulsen.ARA&A, 45:117–175, Sept

    doi:10.1088/0004-637x/774/1/23

  51. [53]

    astro.45.051806.110625

    doi: 10.1146/annurev. astro.45.051806.110625. B. R. McNamara and P. E. J. Nulsen.New Journal of Physics, 14(5):055023, May

    Pith/arXiv arXiv doi:10.1146/annurev

  52. [54]

    doi: 10.1088/1367-2630/14/5/055023. B. R. McNamara et al.ApJ, 648:164–175, Sept

    doi:10.1088/1367-2630/14/5/055023

  53. [55]

    doi: 10.1086/505859. G. K. Miley et al.ApJ, 650:L29–L32, Oct

    doi:10.1086/505859

  54. [56]

    18 The SKA View of Cool-core Clusters M

    doi: 10.1086/508534. 18 The SKA View of Cool-core Clusters M. Gitti R. Mittal, D. S. Hudson, T. H. Reiprich, and T. Clarke.A&A, 501:835–850, July

    work page doi:10.1086/508534

  55. [57]

    doi: 10.1051/0004-6361/200810836. C. R. Mullis, A. Vikhlinin, J. P. Henry, and et al.ApJ, 607:175–189, May

    work page doi:10.1051/0004-6361/200810836

  56. [58]

    doi: 10.1002/asna.201211863. V. Olivares et al.MNRAS, 516(1):L101–L106, Oct

    work page doi:10.1002/asna.201211863

  57. [59]

    doi: 10.1093/mnrasl/slac096. R. A. Overzier.A&A Rv., 24(1):14, Nov

    work page doi:10.1093/mnrasl/slac096

  58. [60]

    J.R.PetersonandA.C.Fabian.Phys.Rep.,427:1–39,Apr.2006

    doi: 10.1007/s00159-016-0100-3. J.R.PetersonandA.C.Fabian.Phys.Rep.,427:1–39,Apr.2006. doi: 10.1016/j.physrep.2005.12

    work page doi:10.1007/s00159-016-0100-3 2006

  59. [61]

    doi: 10.1051/0004-6361:20031464. C. Pinto et al.MNRAS, 480(3):4113–4123, Nov

    work page doi:10.1051/0004-6361:20031464

  60. [62]

    doi: 10.1093/mnras/sty2185. M. Postman et al.ApJS, 199:25, Apr

    work page doi:10.1093/mnras/sty2185

  61. [63]

    doi: 10.1088/0067-0049/199/2/25. I. Prandoni and N. Seymour.PoS(AASKA14)067,

    doi:10.1088/0067-0049/199/2/25

  62. [64]

    doi: 10.1086/591240. C. S. Reynolds et al. In J.-W. A. den Herder, S. Nikzad, and K. Nakazawa, editors,Space Telescopes and Instrumentation 2024: Ultraviolet to Gamma Ray, volume 13093 ofSociety of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, page 1309328, Aug

    doi:10.1086/591240 2024

  63. [65]

    A.Richard-Laferrièreetal.MNRAS,499(2):2934–2958,Dec.2020

    doi: 10.1117/12.3022993. A.Richard-Laferrièreetal.MNRAS,499(2):2934–2958,Dec.2020. doi: 10.1093/mnras/staa2877. C. J. Riseley et al.MNRAS, 512(3):4210–4230, May

    doi:10.1117/12.3022993 2020

  64. [66]

    doi: 10.1093/mnras/stac672. F. Ruppin et al.ApJ, 918(2):43, Sept

    work page doi:10.1093/mnras/stac672

  65. [67]

    doi: 10.3847/1538-4357/ac0bba. H. R. Russell et al.MNRAS, 432(1):530–553, June

    work page doi:10.3847/1538-4357/ac0bba

  66. [68]

    doi: 10.1093/mnras/stt490. H. R. Russell et al.Universe, 10(7):273, June

    work page doi:10.1093/mnras/stt490

  67. [69]

    doi: 10.3390/universe10070273. J. S. Santos, P. Tozzi, P. Rosati, and H. Böhringer.A&A, 521:A64, Oct

    work page doi:10.3390/universe10070273

  68. [70]

    doi: 10.1051/0004-6361/201118162. F. Savini et al.A&A, 622:A24, Feb

    work page doi:10.1051/0004-6361/201118162

  69. [71]

    J.Shin,J.-H.Woo,andJ.S.Mulchaey.ApJS,227(2):31,Dec.2016

    doi: 10.1051/0004-6361/201833882. J.Shin,J.-H.Woo,andJ.S.Mulchaey.ApJS,227(2):31,Dec.2016. doi: 10.3847/1538-4365/227/ 2/31. M. W. Sommer et al.MNRAS, 466(1):996–1009, Apr

    doi:10.1051/0004-6361/201833882 2016

  70. [72]

    doi: 10.1093/mnras/stw3015. M. Sun.ApJ, 704:1586–1604, Oct

    doi:10.1093/mnras/stw3015

  71. [73]

    19 The SKA View of Cool-core Clusters M

    doi: 10.1088/0004-637X/704/2/1586. 19 The SKA View of Cool-core Clusters M. Gitti R. Timmerman et al.A&A, 687:A31, July

    doi:10.1088/0004-637x/704/2/1586

  72. [74]

    doi: 10.1051/0004-6361/202347974. P. Tozzi et al.ApJ, 799(1):93, Jan

    doi:10.1051/0004-6361/202347974

  73. [75]

    doi: 10.1088/0004-637X/799/1/93. P. Tozzi et al.A&A, 667:A134, Nov

    doi:10.1088/0004-637x/799/1/93

  74. [76]

    doi: 10.1051/0004-6361/202244337. A. Travascio et al.arXiv e-prints, art. arXiv:2508.20074, Aug

    doi:10.1051/0004-6361/202244337

  75. [77]

    doi: 10.48550/arXiv.2508. 20074. F. Ubertosi et al.ApJ, 923(2):L25, Dec

    doi:10.48550/arxiv.2508

  76. [78]

    doi: 10.3847/2041-8213/ac374c. F. Ubertosi et al.ApJ, 944(2):216, Feb

    doi:10.3847/2041-8213/ac374c 2041

  77. [79]

    doi: 10.3847/1538-4357/acacf9. F. Ubertosi et al.A&A, 688:A86, Aug. 2024a. doi: 10.1051/0004-6361/202349011. F. Ubertosi et al.ApJ, 961(1):134, Jan. 2024b. doi: 10.3847/1538-4357/ad11d8. R. J. van Weeren et al.Space Sci. Rev., 215(1):16, Feb

    doi:10.3847/1538-4357/acacf9

  78. [80]

    doi: 10.1007/s11214-019-0584-z. R. J. van Weeren et al.A&A, 692:A12, Dec

    doi:10.1007/s11214-019-0584-z

  79. [81]

    doi: 10.1051/0004-6361/202451618. R. J. van Weeren et al.MNRAS, 546(2):stag054, Feb

    work page doi:10.1051/0004-6361/202451618

  80. [82]

    doi: 10.1093/mnras/stag054. F. Vazza and G. Brunetti.arXiv e-prints, art. arXiv:2507.04727, July

    doi:10.1093/mnras/stag054

Showing first 80 references.