pith. sign in

arxiv: 2605.23457 · v1 · pith:3O7PCF2Nnew · submitted 2026-05-22 · 🌌 astro-ph.GA

Cosmic web stripping and starvation of low-mass filament galaxies in TNG50

Daria Zakharova , Gabriella De Lucia , Benedetta Vulcani , Lizhi Xie , Stefania Barsanti , Sean McGee This is my paper

Pith reviewed 2026-05-25 04:01 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords cosmic webfilamentslow-mass galaxiescold gas discsenvironmental effectsTNG50galaxy quenchingstripping
0
0 comments X

The pith

Low-mass filament galaxies develop smaller, more asymmetric cold gas discs than field galaxies of matched mass because early entrants experience altered accretion from tidal fields while late entrants undergo cosmic web stripping.

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

The paper examines low-mass galaxies with stellar masses between 10^8 and 10^10 solar masses in the TNG50 simulation, comparing those in cosmic filaments to those in the field after matching on stellar and halo mass and removing galaxies in groups or clusters. Integrated properties such as stellar and halo mass growth and quenched fractions turn out similar in both environments. In contrast, filament galaxies show distinctly smaller and more asymmetric cold gas discs. The differences arise from two time-dependent processes: cosmic web tidal fields that change the geometry or suppress the rate of gas and dark matter accretion for galaxies that entered filaments early, and rapid hydrodynamical gas removal for galaxies that entered late.

Core claim

When low-mass galaxies in filaments are compared to mass-matched field galaxies after excluding group and cluster members, their cold gas discs are smaller and more asymmetric. Early-entering galaxies experience cosmic web tidal fields that either produce more tangential dark matter motions and thus smaller discs or suppress accretion leading to gradual gas exhaustion through star formation. Late-entering galaxies experience cosmic web stripping that rapidly removes gas in a manner analogous to ram-pressure stripping.

What carries the argument

cosmic web tidal fields acting on early filament entrants and cosmic web stripping acting on late filament entrants, distinguished by entry time into the filament

If this is right

  • Integrated galaxy properties such as stellar mass assembly and quenched fractions remain unaffected by filament membership once mass and group membership are controlled.
  • Spatially resolved cold gas properties reveal environmental influences that integrated quantities miss.
  • Early filament entry can produce a starvation-like path in which galaxies slowly consume their gas without new accretion.
  • Late filament entry produces rapid gas loss comparable to cluster ram-pressure effects but driven by the filament environment.

Where Pith is reading between the lines

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

  • The reported effects on gas discs could contribute to the scatter observed in gas content among low-mass galaxies in real surveys once entry-time information becomes available.
  • If the mechanisms operate at still lower masses, they might help explain the morphology-density relation in the dwarf galaxy regime without invoking group-scale processes.
  • Higher-resolution simulations could test whether the tangential motion channel or the suppression channel dominates at different filament densities.

Load-bearing premise

The chosen filament identification method together with stellar-mass and halo-mass matching and explicit removal of group and cluster members isolates filament-specific effects without leftover contamination from other density variations or from imprecise entry timing.

What would settle it

A direct comparison of cold gas disc sizes and asymmetries in a mass-matched observational sample of low-mass filament and field galaxies, after binning by estimated filament entry time, that finds no systematic differences would falsify the two-mechanism picture.

Figures

Figures reproduced from arXiv: 2605.23457 by Benedetta Vulcani, Daria Zakharova, Gabriella De Lucia, Lizhi Xie, Sean McGee, Stefania Barsanti.

Figure 1
Figure 1. Figure 1: shows the median deviation dxSFMR from the star forma￾tion rate–stellar mass main sequence, computed independently at [PITH_FULL_IMAGE:figures/full_fig_p003_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: shows the stellar mass–𝑅90%,cold gas relation for galaxies in filaments and in the field at z=0, split into four bins of infall time into filaments. Individual galaxies are shown as points. The cold gas extends over a wide range, from ∼ 50 to 150 kpc, and shows a dependence on stellar mass [PITH_FULL_IMAGE:figures/full_fig_p004_2.png] view at source ↗
Figure 4
Figure 4. Figure 4: Example of the growth rate of the cold-gas disc size [PITH_FULL_IMAGE:figures/full_fig_p005_4.png] view at source ↗
Figure 3
Figure 3. Figure 3: The same as Fig [PITH_FULL_IMAGE:figures/full_fig_p005_3.png] view at source ↗
Figure 5
Figure 5. Figure 5: Growth rate of the cold gas disc radius 𝑅90%,cold gas for filament galaxies compared to field galaxies, shown separately before infall (top row) and after infall (bottom row) into filaments. For field galaxies, a mock infall time is assigned (see text), allowing the same before/after segmentation and a consistent estimate of the growth rates. All 100 stellar- and halo-mass–matched field realisations are sh… view at source ↗
Figure 7
Figure 7. Figure 7: Classification of gas evolution scenarios for filament [PITH_FULL_IMAGE:figures/full_fig_p007_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Growth rates of dark matter halo and cold gas disc mass [PITH_FULL_IMAGE:figures/full_fig_p008_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: Properties at z=0 of low-mass gas-accreting filament [PITH_FULL_IMAGE:figures/full_fig_p008_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: Same as Fig [PITH_FULL_IMAGE:figures/full_fig_p009_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: Same as Fig [PITH_FULL_IMAGE:figures/full_fig_p010_11.png] view at source ↗
Figure 12
Figure 12. Figure 12: Geometry of infall into filaments for low-mass galax [PITH_FULL_IMAGE:figures/full_fig_p010_12.png] view at source ↗
read the original abstract

Galaxy properties are known to correlate with their location within the cosmic web. However, the role of filaments remains poorly understood, particularly for low-mass galaxies, which are expected to be more sensitive to environmental effects. In this work, we use the TNG50-1 simulation to investigate the properties of low-mass $8 \le \log(M_{star}/M_{{sun}}) \le 10$ galaxies in filaments and in the field, when controlling for stellar and halo mass and excluding the role of groups and clusters. We find that their integrated properties, including stellar, halo mass assembly and quenched fractions, are similar between the two environments. However, we demonstrate that filament galaxies exhibit smaller and more asymmetric cold gas discs with respect to their field counterparts. We identify two main mechanisms driving these differences. For galaxies that entered filaments in the early Universe, during the phase of active accretion, cosmic web tidal fields modify the accretion of gas and dark matter. In some systems, accretion proceeds at rates comparable to the field but with a different geometry, leading to more tangential motions in the dark matter halo and, consequently, smaller gas discs. In others, the tidal field significantly suppresses both gas and dark matter accretion, leading to a starvation-like evolution, in which galaxies gradually exhaust their gas through star formation and can eventually quench. In contrast, galaxies that fall into filaments at late times can undergo cosmic web stripping, a rapid hydrodynamical removal of gas analogous to ram-pressure stripping in clusters. Our results suggest that spatially resolved gas properties are sensitive to several filament-driven environmental mechanisms.

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

3 major / 2 minor

Summary. The paper uses TNG50-1 to compare low-mass galaxies (8 ≤ log(M_star/M_sun) ≤ 10) in filaments versus the field after stellar- and halo-mass matching and explicit removal of group/cluster members. Integrated properties (stellar/halo mass assembly, quenched fractions) are reported as similar, but filament galaxies show smaller and more asymmetric cold gas discs. The differences are attributed to two mechanisms: cosmic-web tidal fields that modify accretion geometry or suppress accretion (leading to starvation) for early filament entrants, and hydrodynamical cosmic-web stripping for late entrants.

Significance. If the attribution to filament-specific processes holds after controls, the result would demonstrate that resolved cold-gas morphology is sensitive to large-scale tidal and hydrodynamical effects even outside groups and clusters, extending environmental studies to the filament regime for low-mass systems. The simulation-based separation of early versus late entry provides a concrete, falsifiable pathway for testing these mechanisms against observations.

major comments (3)
  1. [methods (filament membership and mass-matching)] Sample construction (methods section on filament identification and matching): the central claim that differences arise from filament entry timing and the two cited mechanisms requires that, after stellar/halo-mass matching and group/cluster removal, residual correlations with large-scale overdensity or tidal-field strength are negligible. No quantitative test (e.g., comparison of tidal tensor eigenvalues or smoothed density outside the filament mask) is described to rule out this confound, which directly undermines unambiguous attribution.
  2. [results (early/late entrant split)] Mechanism separation (results on early vs. late entrants): the distinction between tidal modification of accretion for early entrants and stripping for late entrants is load-bearing, yet the paper does not show that the reported differences in gas-disc size/asymmetry remain after further matching on entry redshift or local tidal strength within each subsample.
  3. [results (disc size and asymmetry)] Quantitative disc measurements: the reported smaller and more asymmetric cold-gas discs are central, but the manuscript does not specify the exact operational definitions (e.g., radius enclosing 90 % of cold gas, asymmetry parameter) or demonstrate that these metrics are robust to projection effects and to the precise temperature/density cuts used to define “cold gas.”
minor comments (2)
  1. [abstract and §2] Notation for stellar and halo masses is inconsistent between the abstract and main text (log(M_star/M_sun) vs. log M_*); adopt a single convention.
  2. [figures] Figure captions should explicitly state the sample sizes for filament versus field subsamples and whether error bars include cosmic variance.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their constructive and detailed report. We address each major comment point-by-point below, outlining the revisions that will be incorporated to strengthen the attribution of results to filament-specific processes.

read point-by-point responses

  1. Referee: [methods (filament membership and mass-matching)] Sample construction (methods section on filament identification and matching): the central claim that differences arise from filament entry timing and the two cited mechanisms requires that, after stellar/halo-mass matching and group/cluster removal, residual correlations with large-scale overdensity or tidal-field strength are negligible. No quantitative test (e.g., comparison of tidal tensor eigenvalues or smoothed density outside the filament mask) is described to rule out this confound, which directly undermines unambiguous attribution.

    Authors: We agree that an explicit quantitative test is needed to confirm negligible residual correlations with large-scale overdensity or tidal-field strength after our mass matching and group/cluster removal. In the revised manuscript we will add a direct comparison of tidal tensor eigenvalues and smoothed density fields (outside the filament mask) between the matched filament and field samples to demonstrate consistency. revision: yes

  2. Referee: [results (early/late entrant split)] Mechanism separation (results on early vs. late entrants): the distinction between tidal modification of accretion for early entrants and stripping for late entrants is load-bearing, yet the paper does not show that the reported differences in gas-disc size/asymmetry remain after further matching on entry redshift or local tidal strength within each subsample.

    Authors: We acknowledge that the mechanism separation would be more robust if the gas-disc differences are shown to persist after additional matching on entry redshift and local tidal strength within the early- and late-entrant subsamples. We will perform this further matching and present the results (including updated statistics on disc size and asymmetry) in the revised manuscript. revision: yes

  3. Referee: [results (disc size and asymmetry)] Quantitative disc measurements: the reported smaller and more asymmetric cold-gas discs are central, but the manuscript does not specify the exact operational definitions (e.g., radius enclosing 90 % of cold gas, asymmetry parameter) or demonstrate that these metrics are robust to projection effects and to the precise temperature/density cuts used to define “cold gas.”

    Authors: We will revise the methods section to state the precise operational definitions (radius enclosing 90% of cold-gas mass for size; the adopted asymmetry parameter) and will add explicit tests of robustness to projection effects as well as to variations in the temperature and density thresholds used to identify cold gas. revision: yes

Circularity Check

0 steps flagged

No circularity: direct simulation comparison of matched samples

full rationale

The paper reports differences in cold-gas disc properties between filament and field galaxies in TNG50 after stellar/halo-mass matching and explicit group/cluster removal. No equations, fitted parameters, or derivations are presented that reduce any reported quantity to a definition or fit drawn from the same data. The analysis consists of direct output comparisons and mechanism identification from simulation snapshots; it contains no self-definitional steps, fitted-input predictions, or load-bearing self-citations that close a loop.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

The central claim rests on standard definitions of filaments, field, and group/cluster membership plus the assumption that TNG50-1 accurately captures hydrodynamical and tidal processes at the resolved scales; no new free parameters or invented entities are introduced in the abstract.

axioms (2)
  • domain assumption Filament membership can be robustly identified and galaxies can be cleanly separated from groups and clusters while controlling for stellar and halo mass.
    Required to attribute differences solely to filament environment.
  • domain assumption TNG50-1 resolution and subgrid physics are sufficient to track cold gas disc sizes and asymmetries without numerical artifacts dominating the signal.
    Underlies all reported morphological differences.

pith-pipeline@v0.9.0 · 5836 in / 1469 out tokens · 39943 ms · 2026-05-25T04:01:05.200743+00:00 · methodology

discussion (0)

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

Lean theorems connected to this paper

Citations machine-checked in the Pith Canon. Every link opens the source theorem in the public Lean library.

What do these tags mean?
matches
The paper's claim is directly supported by a theorem in the formal canon.
supports
The theorem supports part of the paper's argument, but the paper may add assumptions or extra steps.
extends
The paper goes beyond the formal theorem; the theorem is a base layer rather than the whole result.
uses
The paper appears to rely on the theorem as machinery.
contradicts
The paper's claim conflicts with a theorem or certificate in the canon.
unclear
Pith found a possible connection, but the passage is too broad, indirect, or ambiguous to say the theorem truly supports the claim.

Reference graph

Works this paper leans on

300 extracted references · 210 canonical work pages · 90 internal anchors

  1. [1]

    N.,& Stewart, J

    Cox, A. N.,& Stewart, J. N. 1969,

    1969

  2. [2]

    Tscharnuter W. M. 1987,

    1987

  3. [3]

    1992, in ASP Conf

    Terlevich, R. 1992, in ASP Conf. Ser. 31,

    1992

  4. [4]

    F., Tytler, D

    Zheng, W., Davidsen, A. F., Tytler, D. & Kriss, G. A

  5. [5]

    Alpaslan , M., Driver , S., Robotham , A. S. G., et al. 2015, , 451, 3249

    2015

  6. [6]

    A., Neyrinck , M

    Aragon Calvo , M. A., Neyrinck , M. C., & Silk , J. 2019, The Open Journal of Astrophysics, 2, 7

    2019

  7. [7]

    A., van de Weygaert , R., & Jones , B

    Arag \'o n-Calvo , M. A., van de Weygaert , R., & Jones , B. J. T. 2010, , 408, 2163

    2010

  8. [8]

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

    2025

  9. [9]

    M., McCarthy , I

    Bah \'e , Y. M., McCarthy , I. G., Balogh , M. L., & Font , A. S. 2013, , 430, 3017

    2013

  10. [10]

    2022, arXiv e-prints, arXiv:2208.10767

    Barsanti , S., Colless , M., Welker , C., et al. 2022, arXiv e-prints, arXiv:2208.10767

    work page arXiv 2022

  11. [11]

    M., Colless , M., et al

    Barsanti , S., Croom , S. M., Colless , M., et al. 2025, , 538, 2660

    2025

  12. [12]

    Large-scale and local environmental drivers of quenching: tracing H$\alpha$ concentration in X-ray and optical galaxy groups

    Barsanti , S., Wang , D., Colless , M., et al. 2026, arXiv e-prints, arXiv:2602.14628

    work page internal anchor Pith review Pith/arXiv arXiv 2026

  13. [13]

    S., Wechsler , R

    Behroozi , P. S., Wechsler , R. H., Lu , Y., et al. 2014, , 787, 156

    2014

  14. [14]

    F., Abadi , M

    Ben \' tez-Llambay , A., Navarro , J. F., Abadi , M. G., et al. 2013, , 763, L41

    2013

  15. [15]

    V., Busekool , E., Verheijen , M

    Bilimogga , P. V., Busekool , E., Verheijen , M. A. W., & van der Hulst , J. M. 2025, arXiv e-prints, arXiv:2508.01425

    work page arXiv 2025

  16. [16]

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

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

    1996

  17. [17]

    2017, , 469, 594

    Borzyszkowski , M., Porciani , C., Romano-D \' az , E., & Garaldi , E. 2017, , 469, 594

    2017

  18. [18]

    J., & Puerari , I

    Bournaud , F., Combes , F., Jog , C. J., & Puerari , I. 2005, , 438, 507

    2005

  19. [19]

    2020, , 496, 4787

    Cadiou , C., Pichon , C., Codis , S., et al. 2020, , 496, 4787

    2020

  20. [20]

    2022 a , , 657, A9

    Castignani , G., Combes , F., Jablonka , P., et al. 2022 a , , 657, A9

    2022

  21. [21]

    A., et al

    Castignani , G., Vulcani , B., Finn , R. A., et al. 2022 b , , 259, 43

    2022

  22. [22]

    Cautun , M., van de Weygaert , R., Jones , B. J. T., & Frenk , C. S. 2014, , 441, 2923

    2014

  23. [23]

    E., et al

    Codis , S., Jindal , A., Chisari , N. E., et al. 2018, , 481, 4753

    2018

  24. [24]

    A., et al

    Conger , K., Rudnick , G., Finn , R. A., et al. 2025, , 978, 113

    2025

  25. [25]

    P., et al

    Crone Odekon , M., Hallenbeck , G., Haynes , M. P., et al. 2018, , 852, 142

    2018

  26. [26]

    2024, , 687, A68

    De Lucia , G., Fontanot , F., Xie , L., & Hirschmann , M. 2024, , 687, A68

    2024

  27. [27]

    2009, , 703, 785

    Dekel , A., Sari , R., & Ceverino , D. 2009, , 703, 785

    2009

  28. [28]

    D., et al

    Donnari , M., Pillepich , A., Joshi , G. D., et al. 2021, , 500, 4004

    2021

  29. [29]

    2014, , 444, 1453

    Dubois , Y., Pichon , C., Welker , C., et al. 2014, , 444, 1453

    2014

  30. [30]

    2024, , 684, A63

    Gal \'a rraga-Espinosa , D., Cadiou , C., Gouin , C., et al. 2024, , 684, A63

    2024

  31. [31]

    2026, , 706, A21

    Gal \'a rraga-Espinosa , D., Kauffmann , G., Bonoli , S., et al. 2026, , 706, A21

    2026

  32. [32]

    2018, , 481, 414

    Ganeshaiah Veena , P., Cautun , M., van de Weygaert , R., et al. 2018, , 481, 414

    2018

  33. [33]

    M., Porciani , C., & Dekel , A

    Hahn , O., Carollo , C. M., Porciani , C., & Dekel , A. 2007, , 381, 41

    2007

  34. [34]

    N., Abeyta , A., et al

    Hasan , F., Burchett , J. N., Abeyta , A., et al. 2023, , 950, 114

    2023

  35. [35]

    E., et al

    Hoosain , M., Blyth , S.-L., Skelton , R. E., et al. 2024, , 528, 4139

    2024

  36. [36]

    2025, arXiv e-prints, arXiv:2509.18077

    Jego , B., Kraljic , K., B \'e thermin , M., & Dav \'e , R. 2025, arXiv e-prints, arXiv:2509.18077

    work page arXiv 2025

  37. [37]

    Katz , N., Keres , D., Dave , R., & Weinberg , D. H. 2003, in Astrophysics and Space Science Library, Vol. 281, The IGM/Galaxy Connection. The Distribution of Baryons at z=0, ed. J. L. Rosenberg & M. E. Putman , 185

    2003

  38. [38]

    H., & Dav \'e , R

    Kere s , D., Katz , N., Weinberg , D. H., & Dav \'e , R. 2005, , 363, 2

    2005

  39. [39]

    A., Jones , D

    Kleiner , D., Pimbblet , K. A., Jones , D. H., Koribalski , B. S., & Serra , P. 2017, , 466, 4692

    2017

  40. [40]

    2017, Monthly Notices of the Royal Astronomical Society, 474, 547

    Kraljic, K., Arnouts, S., Pichon, C., et al. 2017, Monthly Notices of the Royal Astronomical Society, 474, 547

    2017

  41. [41]

    2021, , 504, 4626

    Kraljic , K., Duckworth , C., Tojeiro , R., et al. 2021, , 504, 4626

    2021

  42. [42]

    2017, , 600, L6

    Kuutma , T., Tamm , A., & Tempel , E. 2017, , 600, L6

    2017

  43. [43]

    2018, , 474, 5437

    Laigle , C., Pichon , C., Arnouts , S., et al. 2018, , 474, 5437

    2018

  44. [44]

    T., Primack , J

    Lee , C. T., Primack , J. R., Behroozi , P., et al. 2017, , 466, 3834

    2017

  45. [45]

    & Kauffmann , G

    Lemson , G. & Kauffmann , G. 1999, , 302, 111

    1999

  46. [46]

    C., et al

    Luber , N., Stierwalt , S., Privon , G. C., et al. 2025, , 993, L14

    2025

  47. [47]

    H., Hess , K

    Luber , N., van Gorkom , J. H., Hess , K. M., et al. 2019, , 157, 254

    2019

  48. [48]

    2018, , 480, 5113

    Marinacci , F., Vogelsberger , M., Pakmor , R., et al. 2018, , 480, 5113

    2018

  49. [49]

    C., et al

    Martizzi , D., Vogelsberger , M., Artale , M. C., et al. 2019, , 486, 3766

    2019

  50. [50]

    J., Mao , S., & White , S

    Mo , H. J., Mao , S., & White , S. D. M. 1998, , 295, 319

    1998

  51. [51]

    Mo , H. J. & White , S. D. M. 1996, , 282, 347

    1996

  52. [52]

    L., Kere s , D., Faucher-Gigu \`e re , C.-A., et al

    Muratov , A. L., Kere s , D., Faucher-Gigu \`e re , C.-A., et al. 2015, , 454, 2691

    2015

  53. [53]

    2018, , 476, 4877

    Musso , M., Cadiou , C., Pichon , C., et al. 2018, , 476, 4877

    2018

  54. [54]

    P., Pillepich , A., Springel , V., et al

    Naiman , J. P., Pillepich , A., Springel , V., et al. 2018, , 477, 1206

    2018

  55. [55]

    Navdha , Busch , P., & White , S. D. M. 2025, , 539, 1248

    2025

  56. [56]

    2018, , 475, 624

    Nelson , D., Pillepich , A., Springel , V., et al. 2018, , 475, 624

    2018

  57. [57]

    J., Kuchner , U., Gray , M

    O'Kane , C. J., Kuchner , U., Gray , M. E., & Arag \'o n-Salamanca , A. 2024, , 534, 1682

    2024

  58. [58]

    C., Springel , V., & van de Voort , F

    Pasha , I., Mandelker , N., van den Bosch , F. C., Springel , V., & van de Voort , F. 2023, , 520, 2692

    2023

  59. [59]

    2011, , 418, 2493

    Pichon , C., Pogosyan , D., Kimm , T., et al. 2011, , 418, 2493

    2011

  60. [60]

    2018 a , , 475, 648

    Pillepich , A., Nelson , D., Hernquist , L., et al. 2018 a , , 475, 648

    2018

  61. [61]

    2019, , 490, 3196

    Pillepich , A., Nelson , D., Springel , V., et al. 2019, , 490, 3196

    2019

  62. [62]

    2018 b , , 473, 4077

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

    2018

  63. [63]

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

    2016

  64. [64]

    Proshina , I. S. & Oparin , D. V. 2025, , 980, 118

    2025

  65. [65]

    & Combes , F

    Reshetnikov , V. & Combes , F. 1998, , 337, 9

    1998

  66. [66]

    D., Brown , T., Zabel , N., et al

    Roberts , I. D., Brown , T., Zabel , N., et al. 2023, , 675, A78

    2023

  67. [67]

    & Br \"u ggen , M

    Roediger , E. & Br \"u ggen , M. 2006, , 369, 567

    2006

  68. [68]

    2019, , 632, A49

    Sarron , F., Adami , C., Durret , F., & Laigle , C. 2019, , 632, A49

    2019

  69. [69]

    2011, , 414, 350

    Sousbie , T. 2011, , 414, 350

    2011

  70. [70]

    2011, , 414, 384

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

    2011

  71. [71]

    2018, , 475, 676

    Springel , V., Pakmor , R., Pillepich , A., et al. 2018, , 475, 676

    2018

  72. [72]

    2016, , 591, A51

    Steinhauser , D., Schindler , S., & Springel , V. 2016, , 591, A51

    2016

  73. [73]

    2014 a , , 572, A8

    Tempel , E., Kipper , R., Saar , E., et al. 2014 a , , 572, A8

    2014

  74. [74]

    S., Mart \' nez , V

    Tempel , E., Stoica , R. S., Mart \' nez , V. J., et al. 2014 b , , 438, 3465

    2014

  75. [75]

    2026, arXiv e-prints, arXiv:2602.15142

    Vulcani , B., De Lucia , G., Zakharova , D., et al. 2026, arXiv e-prints, arXiv:2602.15142

    work page arXiv 2026

  76. [76]

    M., Moretti , A., et al

    Vulcani , B., Poggianti , B. M., Moretti , A., et al. 2021, , 914, 27

    2021

  77. [77]

    M., Moretti , A., et al

    Vulcani , B., Poggianti , B. M., Moretti , A., et al. 2019, , 487, 2278

    2019

  78. [78]

    M., Moretti , A., et al

    Vulcani , B., Poggianti , B. M., Moretti , A., et al. 2018, , 852, 94

    2018

  79. [79]

    J., Jing , Y

    Wang , H., Mo , H. J., Jing , Y. P., Yang , X., & Wang , Y. 2011, , 413, 1973

    2011

  80. [80]

    2014, , 445, L46

    Welker , C., Devriendt , J., Dubois , Y., Pichon , C., & Peirani , S. 2014, , 445, L46

    2014

Showing first 80 references.