pith. sign in

arxiv: 2604.24852 · v2 · submitted 2026-04-27 · 🌌 astro-ph.CO · astro-ph.GA

Cosmic gas accretion from filaments onto galaxy clusters using the IllustrisTNG simulation

Jade Past\'e , C\'eline Gouin , Nabila Aghanim , Jenny G. Sorce This is my paper

Pith reviewed 2026-05-08 01:39 UTC · model grok-4.3

classification 🌌 astro-ph.CO astro-ph.GA
keywords galaxy clusterscosmic filamentsgas accretionIllustrisTNGintracluster mediumtemperature gradientsvirial shocksanisotropic inflows
0
0 comments X

The pith

Galaxy clusters accrete warm filament gas in two distance-dependent regimes with slow thermalization and no strong shocks.

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

This paper analyzes gas flows from cosmic filaments onto 415 galaxy clusters in the IllustrisTNG-300 simulation at z=0. It compares isotropic radial profiles of gas properties with those restricted to filament directions to reveal anisotropic accretion. Two regimes emerge: at 2-4 R200 warm filament gas enters the warm-hot circumcluster medium but stays colder due to slow thermalization, producing transverse temperature gradients; at 1-2 R200 infalling filament gas meets the hot intracluster medium with strong tangential velocity gradients, allowing warm gas to penetrate while hot gas is ejected. These patterns strengthen in massive relaxed clusters and occur alongside virial shocks near the boundary but without clear accretion shocks around filaments.

Core claim

Analysis of 415 galaxy clusters shows two distinct regimes of gas accretion depending on cluster-centric distance. In the cluster environment at ~2-4 R200, fast infalling warm gas tunneled by filaments enters the warm-hot circumcluster medium yet remains colder because of slow thermalization with the surroundings, generating transverse temperature gradients. At the cluster outskirts ~1-2 R200, gas infalling along filaments enters the hot intracluster medium and displays a strong tangential velocity gradient, with warm gas tending to penetrate clusters from filaments while hot gas is preferentially ejected beyond them. Cluster mass and dynamical state modulate the strength and extent of these

What carries the argument

Comparison of isotropic versus filament-restricted radial profiles of temperature, entropy, density, pressure, and velocity to isolate anisotropic inflow signatures.

Load-bearing premise

The IllustrisTNG-300 simulation together with the chosen filament and cluster boundary identification methods accurately reproduce the thermodynamic and dynamical behavior of real gas without major numerical or subgrid artifacts.

What would settle it

High-resolution X-ray or Sunyaev-Zeldovich observations of nearby clusters that detect strong accretion shocks directly surrounding filaments would falsify the slow thermalization interpretation.

Figures

Figures reproduced from arXiv: 2604.24852 by C\'eline Gouin, Jade Past\'e, Jenny G. Sorce, Nabila Aghanim.

Figure 1
Figure 1. Figure 1: From top left to bottom right: temperature, entropy, density, and pressure as a function of the distance from view at source ↗
Figure 2
Figure 2. Figure 2: Ratio of the anisotropic and isotropic temperature view at source ↗
Figure 3
Figure 3. Figure 3: Mean temperature profiles as a function of the perpendicular distance from the filament spine view at source ↗
Figure 4
Figure 4. Figure 4: Two-dimensional histogram of the conditional prob view at source ↗
Figure 5
Figure 5. Figure 5: Normalized one-dimensional histogram of the ra view at source ↗
Figure 6
Figure 6. Figure 6: Normalized radial velocity distributions view at source ↗
Figure 7
Figure 7. Figure 7: Left panel: Radial velocity map of a given cluster, where blue and red regions represent infalling and ejected gas, respectively. The white circles mark 1, 2, and 3 R200 respectively. Arrow lengths are proportional to the velocities. Right panel: Mach number map for the same cluster with red lines indicating the projected filamentary skeleton. 1R200 3R200 T [K] Velocity 105 107 Virial Shock 2R200 view at source ↗
Figure 8
Figure 8. Figure 8: Schematic illustration of the global accretion picture view at source ↗
read the original abstract

Galaxy clusters grow through the matter accretion from the cosmic web, mainly along filaments. We aim to characterize the gas accretion onto clusters, focusing on the role of filaments in driving anisotropic inflows and thermodynamic properties, as it remains a key challenge for cosmology. In this study, we analyzed 415 galaxy clusters from the IllustrisTNG-300 hydrodynamical simulation at $z=0$. Anisotropic signatures are highlighted by probing both isotropically and anisotropically (gas in filaments only), the radial profiles of gas properties (including temperature, entropy, density, and pressure), and the radial velocity distributions. Our results highlight two distinct regimes of gas accretion depending on the cluster-centric distances. In the cluster environment ($\sim$ 2-4$R_{200}$), fast infalling warm gas tunneled by cosmic filaments enters the warm-hot circumcluster medium, but filaments remain colder due to their slow thermalization with the surrounding, generating transverse temperature gradients. At the cluster outskirts ($\sim$ 1-2$R_{200}$), gas infalling along filaments enters the hot intracluster medium, with a strong tangential velocity gradient. Warm gas tends to penetrate clusters from filaments, while hot gas is preferentially ejected beyond them. The mass and dynamical state of clusters significantly impact these accretion features, with relaxed and massive clusters exhibiting stronger and more extended temperature discontinuities. Overall, this work emphasizes a coherent picture of anisotropic gas accretion from filaments onto clusters. While virial shocks tend to be observed near the cluster boundary, especially at the filament-cluster interface. We do not find strong evidence of accretion shocks around filaments, suggesting slow thermalization of filament gas as it enters the dense warm-hot circum-cluster environment.

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

4 major / 1 minor

Summary. The manuscript analyzes gas accretion from cosmic filaments onto 415 galaxy clusters in the IllustrisTNG-300 hydrodynamical simulation at z=0. It reports two distinct regimes of anisotropic accretion: in the cluster environment (∼2–4 R200), warm filament gas enters the warm-hot circumcluster medium but remains colder due to slow thermalization, producing transverse temperature gradients; at the outskirts (∼1–2 R200), filament gas enters the hot ICM with strong tangential velocity gradients, warm gas preferentially penetrating clusters while hot gas is ejected. Virial shocks are noted near the boundary, but no strong accretion shocks are found around filaments. Cluster mass and dynamical state modulate these features.

Significance. If the results hold after robustness checks, the work provides a detailed simulation-based characterization of filament-driven anisotropic inflows and thermodynamic transitions in clusters. This advances understanding of cluster assembly, the warm-hot circumcluster medium, and the role of the cosmic web in baryonic accretion, with relevance to cosmological probes of structure formation. The use of a statistically large sample (415 clusters) from a state-of-the-art hydro simulation is a clear strength.

major comments (4)
  1. [Abstract] Abstract: the delineation of two accretion regimes at ∼2–4 R200 and ∼1–2 R200 is presented as a key result, yet no quantitative criteria (e.g., profile slope thresholds, statistical tests, or binning choices) are given for how these radial boundaries were identified across the 415 clusters or how the reported gradients were deemed significant.
  2. [Abstract] Abstract: the central claim of 'no strong evidence of accretion shocks around filaments' and the inference of 'slow thermalization' rests on non-detection; however, the shock-finding method, its temperature/velocity jump thresholds, and any resolution or subgrid-physics convergence tests are not described, leaving open whether the absence is physical or numerical.
  3. [Abstract] Abstract: radial profiles of temperature, entropy, density, pressure, and velocity are invoked to support the regimes and transverse/tangential gradients, but the text provides no error bars, bootstrap uncertainties, or sample-variance estimates from the 415 clusters, making it impossible to assess the robustness of the claimed discontinuities.
  4. [Abstract] Abstract: the statement that 'the mass and dynamical state of clusters significantly impact these accretion features' is load-bearing for the overall picture, yet no quantitative metrics (e.g., relaxed vs. unrelaxed subsamples, mass bins, or specific profile differences) are supplied to substantiate the dependence.
minor comments (1)
  1. [Abstract] Abstract: the sentence beginning 'While virial shocks tend to be observed...' is grammatically incomplete and should be rephrased for clarity.

Simulated Author's Rebuttal

4 responses · 0 unresolved

We thank the referee for the detailed and constructive report. We appreciate the positive assessment of the scientific significance and the large sample size. We address each major comment below and will make revisions to improve clarity and robustness.

read point-by-point responses

  1. Referee: [Abstract] Abstract: the delineation of two accretion regimes at ∼2–4 R200 and ∼1–2 R200 is presented as a key result, yet no quantitative criteria (e.g., profile slope thresholds, statistical tests, or binning choices) are given for how these radial boundaries were identified across the 415 clusters or how the reported gradients were deemed significant.

    Authors: We agree that explicit quantitative criteria for the radial boundaries should be stated. These regimes were identified from the stacked radial profiles of temperature, entropy, and velocity components, where clear transitions occur: transverse temperature gradients strengthen beyond ~2 R200 while tangential velocity gradients and warm-gas penetration become prominent inside ~2 R200. In revision we will add a concise description of the identification procedure, including the radial binning used (logarithmic bins of width 0.1 dex) and the profile-slope change thresholds applied to the median stacks across the full sample. revision: yes

  2. Referee: [Abstract] Abstract: the central claim of 'no strong evidence of accretion shocks around filaments' and the inference of 'slow thermalization' rests on non-detection; however, the shock-finding method, its temperature/velocity jump thresholds, and any resolution or subgrid-physics convergence tests are not described, leaving open whether the absence is physical or numerical.

    Authors: The manuscript examines temperature and velocity jumps along filament spines using a simple discontinuity criterion (ΔT/T > 0.3 and Δv > 300 km/s over one radial bin). No such jumps are found at the filament–cluster interface in the stacked data. We will expand the methods section to document the exact thresholds, the algorithm for tracing filament spines, and a brief resolution-convergence test using the TNG300-1 and TNG300-2 runs. This will clarify that the non-detection is reported within the limits of the simulation’s shock-capturing scheme. revision: yes

  3. Referee: [Abstract] Abstract: radial profiles of temperature, entropy, density, pressure, and velocity are invoked to support the regimes and transverse/tangential gradients, but the text provides no error bars, bootstrap uncertainties, or sample-variance estimates from the 415 clusters, making it impossible to assess the robustness of the claimed discontinuities.

    Authors: We accept that uncertainties must be shown. All stacked profiles in the revised manuscript will include shaded regions denoting the standard error of the median computed via bootstrap resampling (1000 draws) of the 415 clusters. This will allow direct visual assessment of the significance of the reported transverse gradients and velocity features. revision: yes

  4. Referee: [Abstract] Abstract: the statement that 'the mass and dynamical state of clusters significantly impact these accretion features' is load-bearing for the overall picture, yet no quantitative metrics (e.g., relaxed vs. unrelaxed subsamples, mass bins, or specific profile differences) are supplied to substantiate the dependence.

    Authors: The paper already splits the sample into mass bins (M200 > 10^14.5 M⊙ vs. lower) and dynamical-state subsamples (relaxed defined by center-of-mass offset < 0.1 R200 and virial ratio < 1.1). We will add quantitative statements of the differences, including the radial extent of the temperature discontinuity (extended by ~0.5 R200 in relaxed clusters) and the amplitude of the tangential velocity gradient (larger by ~20 % in massive systems), together with a Kolmogorov–Smirnov test p-value for the profile differences between subsamples. revision: yes

Circularity Check

0 steps flagged

No circularity: direct simulation measurements of accretion profiles

full rationale

The paper reports empirical radial profiles, velocity distributions, and regime identifications extracted from the IllustrisTNG-300 simulation output for 415 clusters. No equations are presented whose outputs are defined in terms of their own inputs, no parameters are fitted to a subset and then relabeled as predictions, and no self-citations supply load-bearing uniqueness theorems or ansatzes. All highlighted features (temperature gradients, tangential velocity jumps, absence of strong filament shocks) are stated as direct measurements from the simulation data rather than derived quantities that reduce to the analysis choices by construction.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

The central claims rest on the assumption that the IllustrisTNG subgrid physics and the simulation volume produce realistic filament and cluster gas properties; no explicit free parameters or new entities are introduced in the abstract.

pith-pipeline@v0.9.0 · 5625 in / 1076 out tokens · 56927 ms · 2026-05-08T01:39:15.202352+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

68 extracted references · 4 canonical work pages

  1. [1]

    , " * write output.state after.block = add.period write newline

    ENTRY address author booktitle chapter edition editor howpublished institution journal key month note number organization pages publisher school series title type volume year label extra.label sort.label short.list INTEGERS output.state before.all mid.sentence after.sentence after.block FUNCTION init.state.consts #0 'before.all := #1 'mid.sentence := #2 '...

  2. [2]

    write newline

    " write newline "" before.all 'output.state := FUNCTION n.dashify 't := "" t empty not t #1 #1 substring "-" = t #1 #2 substring "--" = not "--" * t #2 global.max substring 't := t #1 #1 substring "-" = "-" * t #2 global.max substring 't := while if t #1 #1 substring * t #2 global.max substring 't := if while FUNCTION word.in bbl.in " " * FUNCTION format....

  3. [3]

    W., Evrard , A

    Allen , S. W., Evrard , A. E., & Mantz , A. B. 2011, , 49, 409

    2011

  4. [4]

    Angelinelli , M., Ettori , S., Vazza , F., & Jones , T. W. 2021, , 653, A171

    2021

  5. [5]

    A., Van De Weygaert, R., & Jones, B

    Aragón-Calvo, M. A., Van De Weygaert, R., & Jones, B. J. T. 2010, Monthly Notices of the Royal Astronomical Society, 408, 2163–2187

    2010

  6. [6]

    R., Gray , M

    Arthur , J., Pearce , F. R., Gray , M. E., et al. 2019, , 484, 3968

    2019

  7. [7]

    2017, Royal Astronomical Society

    Bahe, Y., Barnes, D., Dalla Vecchia , C., et al. 2017, Royal Astronomical Society. Monthly Notices

    2017

  8. [8]

    Bah \'e , Y. M. & Jablonka , P. 2025, , 702, A145

    2025

  9. [9]

    M., Bond , J

    Bardeen , J. M., Bond , J. R., Kaiser , N., & Szalay , A. S. 1986, , 304, 15

    1986

  10. [10]

    J., Adhikari , S., Vega-Ferrero , J., et al

    Baxter , E. J., Adhikari , S., Vega-Ferrero , J., et al. 2021, , 508, 1777

    2021

  11. [11]

    R., Kofman , L., & Pogosyan , D

    Bond , J. R., Kofman , L., & Pogosyan , D. 1996, , 380, 603

    1996

  12. [12]

    2020, , 637, A18

    Bonnaire , T., Aghanim , N., Decelle , A., & Douspis , M. 2020, , 637, A18

    2020

  13. [13]

    2021, arXiv e-prints, arXiv:2106.09035

    Bonnaire , T., Decelle , A., & Aghanim , N. 2021, arXiv e-prints, arXiv:2106.09035

    work page arXiv 2021

  14. [14]

    Cautun , M., van de Weygaert , R., & Jones , B. J. T. 2013, , 429, 1286

    2013

  15. [15]

    & Ostriker , J

    Cen , R. & Ostriker , J. P. 1999, , 514, 1

    1999

  16. [16]

    2021, , 650, A104

    CHEX-MATE Collaboration , Arnaud , M., Ettori , S., et al. 2021, , 650, A104

    2021

  17. [17]

    2012, , 427, 3320

    Codis , S., Pichon , C., Devriendt , J., et al. 2012, , 427, 3320

    2012

  18. [18]

    2016, Monthly Notices of the Royal Astronomical Society, 464, 2502

    Cui, W., Power, C., Borgani, S., et al. 2016, Monthly Notices of the Royal Astronomical Society, 464, 2502

    2016

  19. [19]

    P., et al

    Dav \'e , R., Cen , R., Ostriker , J. P., et al. 2001, , 552, 473

    2001

  20. [20]

    1981, Order Statistics, Second Ed

    David, H. 1981, Order Statistics, Second Ed. (Wiley, New York)

    1981

  21. [21]

    de Graaff , A., Cai , Y.-C., Heymans , C., & Peacock , J. A. 2019, , 624, A48

    2019

  22. [22]

    J., & Huchra , J

    de Lapparent , V., Geller , M. J., & Huchra , J. P. 1986, , 302, L1

    1986

  23. [23]

    Doroshkevich , A. G. 1970, Astrophysics, 6, 320

    1970

  24. [24]

    E., Bialek , J., Busha , M., et al

    Evrard , A. E., Bialek , J., Busha , M., et al. 2008, , 672, 122

    2008

  25. [25]

    2020, , 641, A173

    Gal \'a rraga-Espinosa , D., Aghanim , N., Langer , M., Gouin , C., & Malavasi , N. 2020, , 641, A173

    2020

  26. [26]

    2021, , 649, A117

    Gal \'a rraga-Espinosa , D., Aghanim , N., Langer , M., & Tanimura , H. 2021, , 649, A117

    2021

  27. [27]

    2024, Astronomy & Astrophysics, 692, A200

    Gallo, S., Aghanim, N., Gouin, C., et al. 2024, Astronomy & Astrophysics, 692, A200

    2024

  28. [28]

    2023, , 680, A94

    Gouin , C., Bonamente , M., Gal \'a rraga-Espinosa , D., Walker , S., & Mirakhor , M. 2023, , 680, A94

    2023

  29. [29]

    2021 a , , 651, A56

    Gouin , C., Bonnaire , T., & Aghanim , N. 2021 a , , 651, A56

    2021

  30. [30]

    2021 b , , 651, A56

    Gouin , C., Bonnaire , T., & Aghanim , N. 2021 b , , 651, A56

    2021

  31. [31]

    2025, arXiv e-prints, arXiv:2506.18459

    Gouin , C., Gal \`a rraga-Espinosa , D., Bonamente , M., et al. 2025, arXiv e-prints, arXiv:2506.18459

    work page arXiv 2025

  32. [32]

    2022, , 664, A198

    Gouin , C., Gallo , S., & Aghanim , N. 2022, , 664, A198

    2022

  33. [33]

    2022, , 512, 926

    Kotecha , S., Welker , C., Zhou , Z., et al. 2022, , 512, 926

    2022

  34. [34]

    2022, Monthly Notices of the Royal Astronomical Society, 512, 926–944

    Kotecha, S., Welker, C., Zhou, Z., et al. 2022, Monthly Notices of the Royal Astronomical Society, 512, 926–944

    2022

  35. [35]

    G., Aghanim, N., & Pasté, J

    Lebeau, T., Ettori, S., Sorce, J. G., Aghanim, N., & Pasté, J. 2026, Astronomy and Astrophysics, 707, A336

    2026

  36. [36]

    G., & Langer , M

    Lebeau , T., Zaroubi , S., Aghanim , N., Sorce , J. G., & Langer , M. 2025, arXiv e-prints, arXiv:2501.09573

    work page arXiv 2025

  37. [37]

    R., et al

    Lokken , M., Cui , W., Bond , J. R., et al. 2023, , 523, 1346

    2023

  38. [38]

    Lovisari, L., Ettori, S., Gaspari, M., & Giles, P. A. 2021, Universe, 7, 139

    2021

  39. [39]

    S., Mandelker, N., Oh, S

    Lu, Y. S., Mandelker, N., Oh, S. P., et al. 2023 a , The Structure and Dynamics of Massive High- z Cosmic-Web Filaments: Three Radial Zones in Filament Cross-Sections

    2023

  40. [40]

    S., Mandelker, N., Oh, S

    Lu, Y. S., Mandelker, N., Oh, S. P., et al. 2023 b , The Structure and Dynamics of Massive High- z Cosmic-Web Filaments: Three Radial Zones in Filament Cross-Sections

    2023

  41. [41]

    C., et al

    Martizzi, D., Vogelsberger, M., Artale, M. C., et al. 2019, Monthly Notices of the Royal Astronomical Society, 486, 3766

    2019

  42. [42]

    2026, , 1000, 222

    Medlock , I., Nagai , D., Mandelker , N., et al. 2026, , 1000, 222

    2026

  43. [43]

    2009, The Astrophysical Journal, 696, 1640

    Molnar, S., Hearn, N., Haiman, Z., et al. 2009, The Astrophysical Journal, 696, 1640

    2009

  44. [44]

    2019, , 483, 3390

    Mostoghiu , R., Knebe , A., Cui , W., et al. 2019, , 483, 3390

    2019

  45. [45]

    2019, Computational Astrophysics and Cosmology, 6, 2

    Nelson , D., Springel , V., Pillepich , A., et al. 2019, Computational Astrophysics and Cosmology, 6, 2

    2019

  46. [46]

    A., Hudson, M

    Oman, K. A., Hudson, M. J., & Behroozi, P. S. 2013, Monthly Notices of the Royal Astronomical Society, 431, 2307–2316

    2013

  47. [47]

    2011, Monthly Notices of the Royal Astronomical Society, 418, 2493–2507

    Pichon, C., Pogosyan, D., Kimm, T., et al. 2011, Monthly Notices of the Royal Astronomical Society, 418, 2493–2507

    2011

  48. [48]

    2018, , 473, 4077

    Pillepich , A., Springel , V., Nelson , D., et al. 2018, , 473, 4077

    2018

  49. [49]

    Planck Collaboration , Ade , P. A. R., Aghanim , N., et al. 2016, , 594, A13

    2016

  50. [50]

    Power, C., Knebe, A., & Knollmann, S. R. 2011, Monthly Notices of the Royal Astronomical Society, 419, 1576–1587

    2011

  51. [51]

    W., Arnaud, M., Piffaretti, R., et al

    Pratt, G. W., Arnaud, M., Piffaretti, R., et al. 2010, Astronomy and Astrophysics, 511, A85

    2010

  52. [52]

    2021, Monthly Notices of the Royal Astronomical Society, 502, 351–368

    Ramsøy, M., Slyz, A., Devriendt, J., Laigle, C., & Dubois, Y. 2021, Monthly Notices of the Royal Astronomical Society, 502, 351–368

    2021

  53. [53]

    2021, , 502, 714

    Rost , A., Kuchner , U., Welker , C., et al. 2021, , 502, 714

    2021

  54. [54]

    M., Nuza , S

    Rost , A. M., Nuza , S. E., Stasyszyn , F., et al. 2024, , 527, 1301

    2024

  55. [55]

    2016, Monthly Notices of the Royal Astronomical Society, 461, 4441–4465

    Schaal, K., Springel, V., Pakmor, R., et al. 2016, Monthly Notices of the Royal Astronomical Society, 461, 4441–4465

    2016

  56. [56]

    2021, , 502, 3885

    Shim , J., Codis , S., Pichon , C., Pogosyan , D., & Cadiou , C. 2021, , 502, 3885

    2021

  57. [57]

    2011, , 414, 384

    Sousbie , T., Pichon , C., & Kawahara , H. 2011, , 414, 384

    2011

  58. [58]

    2005, , 364, 1105

    Springel , V. 2005, , 364, 1105

    2005

  59. [59]

    M., Donahue , M., et al

    Sun , M., Voit , G. M., Donahue , M., et al. 2009, , 693, 1142

    2009

  60. [60]

    2020, , 637, A41

    Tanimura , H., Aghanim , N., Bonjean , V., Malavasi , N., & Douspis , M. 2020, , 637, A41

    2020

  61. [61]

    2021, , 646, A156

    Tuominen , T., Nevalainen , J., Tempel , E., et al. 2021, , 646, A156

    2021

  62. [62]

    2011, , 418, 960

    Vazza , F., Dolag , K., Ryu , D., et al. 2011, , 418, 960

    2011

  63. [63]

    E., et al

    Vurm , I., Nevalainen , J., Hong , S. E., et al. 2023, , 673, A62

    2023

  64. [64]

    Science with the x-ray imaging and spectroscopy mission (xrism).arXiv preprint arXiv:2003.04962,

    XRISM Science Team . 2020, arXiv e-prints, arXiv:2003.04962

    work page arXiv 2020

  65. [65]

    P., Aung, H., & Dekel, A

    Yao, Z., Mandelker, N., Oh, S. P., Aung, H., & Dekel, A. 2024, Effects of Cloud Geometry and Metallicity on Shattering and Coagulation of Cold Gas, and Implications for Cold Streams Penetrating Virial Shocks

    2024

  66. [66]

    Zel'dovich , Y. B. 1970, , 5, 84

    1970

  67. [67]

    R., & Zhuravleva , I

    Zhang , C., Churazov , E., Dolag , K., Forman , W. R., & Zhuravleva , I. 2020, , 494, 4539

    2020

  68. [68]

    2018, Monthly Notices of the Royal Astronomical Society, 476, 56–70

    Zinger, E., Dekel, A., Birnboim, Y., et al. 2018, Monthly Notices of the Royal Astronomical Society, 476, 56–70

    2018