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arxiv: 2606.31503 · v1 · pith:IBEILT7Inew · submitted 2026-06-30 · 🌌 astro-ph.CO

The Large-Scale Structure of the Universe through the SKA lenses

Virginia Cuciti , Surajit Paul , Viral Parekh , Franco Vazza , M. Br\"uggen , Prateek Gupta , Sameer Salunkhe , S. Sankhyayan
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A. Bonafede T. Akahori G. Brunetti R. Cassano M. Hoeft R. Kale
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Pith reviewed 2026-07-01 04:16 UTC · model grok-4.3

classification 🌌 astro-ph.CO
keywords cosmic webSKAradio emissionfilamentsbaryon distributioncluster outskirtsmegahalosLambda-CDM
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The pith

The Square Kilometre Array will detect faint radio emission from plasma in cosmic web filaments and cluster outskirts.

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

This review summarizes how Lambda-CDM simulations predict a filamentary cosmic web whose nodes and filaments contain plasma at temperatures from 10^5 to 10^8 K. Energy dissipated through plasma processes during galaxy accretion produces radio-emitting electrons that trace the dynamical evolution of large-scale structure. While massive clusters are well observed, the fainter outskirts and intergalactic filaments have remained elusive, though recent detections of megahalos and radio bridges with LOFAR, uGMRT and MeerKAT demonstrate the approach. The paper's central claim is that the SKA's sensitivity will map this emission across the cosmic web and thereby reveal the distribution of baryons.

Core claim

Cosmological simulations within the Lambda-CDM framework reproduce the filamentary cosmic web and predict that its nodes and filaments are filled with tenuous plasma at 10^5-10^8 K. The hottest plasma resides in cluster nodes while cooler gas extends along filaments; galaxies flow along these filaments before accreting onto clusters. Enormous energy is dissipated through plasma processes that accelerate electrons and produce observable radio emission. Current facilities have detected emission from denser regions such as megahalos and cluster-pair bridges, but the fainter emission from cluster outskirts and intergalactic filaments has stayed below detection thresholds. The forthcoming Square

What carries the argument

Faint radio emission from electrons accelerated by plasma processes in the tenuous gas of cosmic-web filaments and cluster outskirts, which traces energy dissipation during structure formation.

If this is right

  • Detection of radio megahalos and bridges will trace the flow of galaxies and groups along filaments toward clusters.
  • Mapping of the emission will provide direct observational constraints on the baryon content in the warm-hot intergalactic medium.
  • Successful observations will test the plasma physics and energy dissipation mechanisms assumed in structure-formation simulations.
  • Wider coverage will reveal how the cosmic web evolves across different redshifts and environments.

Where Pith is reading between the lines

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

  • These SKA maps could locate the bulk of the missing baryons by imaging the warm-hot gas in filaments.
  • The same data would allow study of accretion shocks and turbulence on scales larger than individual clusters.
  • Deviations between observed radio structures and simulation predictions could motivate refinements to feedback or magnetic-field models in cosmology.

Load-bearing premise

That Lambda-CDM simulations correctly predict the temperature and density of the plasma in filaments and cluster outskirts, and that SKA sensitivity will be sufficient to detect the expected faint radio emission.

What would settle it

Non-detection of the predicted radio emission from cluster outskirts and intergalactic filaments in SKA observations at the sensitivity levels expected from current simulations.

Figures

Figures reproduced from arXiv: 2606.31503 by A. Bonafede, Franco Vazza, G. Brunetti, M. Br\"uggen, M. Hoeft, Prateek Gupta, R. Cassano, R. Kale, Sameer Salunkhe, S. Sankhyayan, Surajit Paul, T. Akahori, Viral Parekh, Virginia Cuciti.

Figure 1
Figure 1. Figure 1: Left panel: A projection map of dark-matter density overlaid with the average Mach number of shocks along the line of sight. All the gravitationally-collapsed structures (shown in orange/white) are surrounded by successive shock surfaces (in blue), which encode their formation histories. Right panel: A projection map combining gas temperature (colour) and shock Mach number (brightness). Red indicates 10 mi… view at source ↗
Figure 2
Figure 2. Figure 2: SDSS galaxies overplotted by identified interacting clusters (Oak and Paul, 2024). Numerous studies have sought to identify and characterize galaxy clusters using such optical datasets over the past decades (e.g., Yoon, 2008; Tempel, 2012). However, the early system￾atic attempts to identify merging clusters, ex￾tending beyond simple cluster detection—were made by Tempel (2017). More recently, Oak and Paul… view at source ↗
Figure 3
Figure 3. Figure 3: Blue: simulated gas density distribution (Vazza et al., 2019). Orange: LOFAR image of the megahalo in Zwcl 0634.1+4750. Grey: LOFAR image of the radio halo in Zwcl 0634.1+4750. Inset: Surface brightness profile of the radio emission in Zwcl 0634.1+4750 (Cuciti et al., 2022). Another illustrative case is that of the massive cluster PLCK G287.0+32.9. Using uGMRT obser￾vations, Salunkhe et al. (2025) reported… view at source ↗
Figure 4
Figure 4. Figure 4: Mass–redshift diagram for all clusters in the Planck sample (red dots). Red filled dots indicate clusters included in the Planck LoTSS DR2 sample, while black dots represent clusters from the ACT catalogue. Stars mark clus￾ters hosting megahalos. Solid lines show the region where megahalos are detectable with LoTSS, and the dashed line indicates the region where they are expected to be detectable with SKA-… view at source ↗
Figure 5
Figure 5. Figure 5: Radio bridges. Left: A399 – A401 (Govoni et al., 2019). Color and contours show the radio emission at 144 MHz with a resolution of 80′′ and rms= 1 mJy/beam. Contours start at 3 mJy/beam and increase by factors of two. Right: A1758 (Botteon et al., 2020). Color and contours show the radio emission at 144 MHz with a resolution of 35′′ and rms= 160 𝜇Jy/beam. Contours start at 3 𝜎 and increase by factors of tw… view at source ↗
Figure 6
Figure 6. Figure 6: Top left panel: projected (mass weighted) mean magnetic field strength (colours) and contours of mass-weighted mean gas temperature along the line of sight of a cosmological simulation. The other panels show the predicted synchrotron radio emission from cosmic shocks, detectable with different observing configurations: a) with 1hr exposure time with SKA-Low (50 − 250 MHz, rms = 21.2 𝜇Jy/beam with beam =13.… view at source ↗
read the original abstract

The large-scale distribution of galaxies in the Universe forms an intricate, interconnected network known as the cosmic web. Cosmological simulations within the standard Lambda-CDM framework successfully reproduce this filamentary structure and predict that the nodes and filaments are filled with tenuous plasma at temperatures ranging from 10^5-10^8 K. The hottest and luminous plasma in the nodes corresponds to the intra-cluster medium, while the cooler, more tenuous, gas extends along filaments and cluster outskirts. Galaxies and galaxy groups form and flow along these filaments before accreting onto galaxy clusters (the nodes), outlining the dynamical evolution of large-scale structures. During this process, an enormous amount of energy is dissipated through complex plasma processes that can be traced by radio emitting electrons. Despite strong theoretical support for this picture, observational validation remains limited. While massive clusters have been widely detected across various wavelengths, cluster outskirts and the diffuse intergalactic medium within filaments has remained elusive due to their extremely faint emission. The advent of highly sensitive radio facilities such as LOFAR, uGMRT, and MeerKAT has recently enabled a few successful detections of emission from comparatively denser regions of the cosmic-web. These include radio megahalos, permeating the entire cluster volume, as well as bridges of radio emission connecting cluster pairs. In this chapter, we summarize current theoretical insights into the cosmic web, discuss observational strategies and recent discoveries, and highlight how the forthcoming Square Kilometre Array (SKA) is expected to transform our understanding of the cosmic web and the distribution of baryons in the Universe.

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

0 major / 1 minor

Summary. This review chapter summarizes Lambda-CDM predictions for the filamentary cosmic web and the distribution of baryonic plasma (10^5-10^8 K) in nodes and filaments, reviews recent radio detections of diffuse emission (megahalos, cluster bridges) with LOFAR/uGMRT/MeerKAT, and outlines how the SKA is expected to map the large-scale structure and address the baryon distribution.

Significance. The manuscript offers a clear, consensus-level synthesis of theoretical expectations and observational progress in radio studies of the cosmic web. It correctly identifies the gap between simulation predictions and current detections of faint filamentary emission, and positions SKA as the instrument likely to close that gap. No new derivations, quantitative forecasts, or empirical results are advanced; the value is therefore as a consolidated reference rather than a primary research contribution.

minor comments (1)
  1. [Abstract] Abstract: the phrase 'in this chapter' appears only at the end; moving an explicit statement that the work is a review chapter to the opening sentence would improve reader orientation.

Simulated Author's Rebuttal

0 responses · 0 unresolved

We thank the referee for their positive assessment and recommendation to accept the manuscript. The referee's summary correctly reflects the scope and intent of this review chapter on the cosmic web, radio observations, and the role of the SKA.

Circularity Check

0 steps flagged

No significant circularity; review paper without derivations or fitted predictions

full rationale

The manuscript is a review chapter summarizing Lambda-CDM simulation predictions for the cosmic web, recent detections from LOFAR/uGMRT/MeerKAT, and qualitative SKA prospects. No equations, derivations, parameter fits, or quantitative forecasts are advanced in the provided text or abstract. All load-bearing statements (simulation fidelity for filament plasma, SKA sensitivity) are explicitly inherited from cited external literature rather than generated internally. No self-citation chains, self-definitional steps, or renamings of results occur. This is the expected outcome for a purely descriptive review.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

As a review chapter, the paper introduces no new free parameters, axioms, or invented entities; it references the standard Lambda-CDM framework from prior literature.

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