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arxiv: 2605.11858 · v1 · submitted 2026-05-12 · 🌌 astro-ph.HE

Recognition: no theorem link

High-energy Multi-messenger Emission from Galaxy Clusters in the Local Universe

Gabrijela Zaharijas, Klaus Dolag, Saqib Hussain

Pith reviewed 2026-05-13 04:57 UTC · model grok-4.3

classification 🌌 astro-ph.HE
keywords galaxy clustersgamma-ray emissionneutrino emissioncosmic raysMHD simulationsmulti-messenger astronomyintracluster mediumdiffuse backgrounds
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The pith

Numerical models show that gamma-ray and neutrino emission from local galaxy clusters falls below current telescope upper limits.

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

The paper models high-energy gamma-ray and neutrino emission from nearby galaxy clusters such as Virgo, Perseus, and Coma. It combines magnetohydrodynamic simulations of the intracluster medium with Monte Carlo methods to follow cosmic-ray propagation and the secondaries they produce. The work assumes cosmic-ray injection scales with gas density and finds that the resulting fluxes from individual clusters sit well below LHAASO limits while the cumulative output from local clusters matches IceCube neutrino bounds but falls short of the Fermi-LAT diffuse gamma-ray background. A sympathetic reader would care because the calculation tests whether galaxy clusters can be important sources of the observed diffuse high-energy messengers.

Core claim

Using MHD simulations that supply the distributions of gas, temperature, and magnetic field together with Monte Carlo tracking of cosmic-ray propagation, and taking cosmic-ray injection to scale with gas density, the predicted gamma-ray flux from the individual Virgo, Perseus, and Coma clusters lies well below present LHAASO upper limits; MAGIC data on the central source NGC 1275 exceed the model; the cumulative gamma-ray flux from clusters with masses above 5 times 10^13 solar masses within 500 megaparsecs is significantly lower than the Fermi-LAT diffuse measurement; and the neutrino predictions remain consistent with IceCube upper limits on unresolved flux from clusters above 10^14 solar

What carries the argument

MHD simulations of intracluster gas, temperature, and magnetic fields coupled to Monte Carlo cosmic-ray propagation and secondary production, with cosmic-ray injection scaled to local gas density.

If this is right

  • Individual cluster gamma-ray fluxes remain below LHAASO sensitivity.
  • Cumulative neutrino emission from clusters up to redshift 2 stays within IceCube unresolved limits.
  • Galaxy clusters cannot account for the full Fermi-LAT diffuse gamma-ray background.
  • High-density turbulent and shocked regions inside clusters act as the main sites of cosmic-ray acceleration.

Where Pith is reading between the lines

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

  • Other populations such as starburst galaxies or active galactic nuclei must supply most of the diffuse high-energy backgrounds.
  • Next-generation gamma-ray instruments could detect the faint cluster emission and thereby test the gas-density scaling assumption.
  • The same numerical approach can be extended to higher-redshift or lower-mass systems to estimate the total cluster contribution to the cosmic neutrino background.

Load-bearing premise

Cosmic ray injection scales directly with the gas density inside the clusters.

What would settle it

A gamma-ray detection from Virgo, Perseus, or Coma at a flux level several times higher than the model prediction would falsify the central result.

Figures

Figures reproduced from arXiv: 2605.11858 by Gabrijela Zaharijas, Klaus Dolag, Saqib Hussain.

Figure 1
Figure 1. Figure 1: The left column (top to bottom) represents 2D (XZ) central slices (at y=0) of the gas density of the Coma, Perseus, and Virgo clusters, respectively. The right column represents the magnetic field configurations of the same clusters. These maps are obtained from the SLOW MHD simulation at redshift z ≃ 0 (Dolag et al. 2023) [PITH_FULL_IMAGE:figures/full_fig_p005_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: The γ−ray spectra in our simulations, integrated over the entire volume of the Coma, Perseus, and Virgo clusters. The magenta band represents spectra for parameters α = 2.0 − 2.5 & Emax = 1016 − 1017 eV. We also depicted upper limits of LHAASO for these clusters (Cao et al. 2025). Blue error bar in the top left panel represents the upper limits of Fermi-LAT for the Coma cluster above energy 10 GeV (Xi et a… view at source ↗
Figure 3
Figure 3. Figure 3: Projected 2D γ−ray intensity map of a Perseus-like cluster obtained directly from our Monte-Carlo simulations. 10 11 10 12 10 13 10 14 10 15 10 16 E [eV] 10 10 10 9 10 8 10 7 10 6 10 5 10 4 E 2 [M e V c m 2 s 1 ] this work KM3Net [PITH_FULL_IMAGE:figures/full_fig_p009_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: All-flavor neutrino flux for Virgo cluster, for same parameters as in [PITH_FULL_IMAGE:figures/full_fig_p009_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: The magenta (γ−rays) and blue (neutrinos) bands represent spectra for parameters α = 2.0 − 2.5 & Emax = 1016 − 1017 eV. These bands represent the integrated fluxes of γ−rays and neutrinos (all-fla￾vor) computed from our simulations for all clusters of masses ≳ 5 × 1013 M⊙ within a distance ∼ 500 Mpc. The diffuse γ−ray flux of Fermi-LAT (Ackermann et al. 2015b) and HAWC upper limits (Albert et al. 2022) are… view at source ↗
Figure 6
Figure 6. Figure 6: Left panel: 2D map of extended injection as a function of radius and CR energy. The color scale shows the injection rate in arbitrary units. The injection follows the volume-averaged profile of gas density of a Perseus-like cluster. Right panel: Radial profile of CR injection. The central injection is represented by a point source (delta-function) at the cluster core, while the extended injection follows t… view at source ↗
Figure 7
Figure 7. Figure 7 [PITH_FULL_IMAGE:figures/full_fig_p017_7.png] view at source ↗
read the original abstract

The origin of diffuse neutrinos and $\gamma$-rays is unknown, and galaxy clusters hosting AGN and starburst galaxies are the most probable sources of these cosmic messengers. In this work, we investigate the diffuse $\gamma$-ray and neutrino emission from the Virgo, Perseus, and Coma clusters using a detailed numerical method, combining MHD simulations with Monte Carlo methods. The MHD simulation provides the distributions of temperature, gas, and magnetic field in clusters. The Monte Carlo simulations are used to investigate the cosmic-ray (CR) propagation in ICM and subsequently the secondaries stemming from CRs. Our primary assumption is that CR injection scales with the gas density of clusters, providing a physically motivated approximation. High-density regions in clusters are associated with strong turbulence and prominent shock structures, making them natural sites for efficient CR acceleration. Our predicted $\gamma$-ray flux from the individual clusters lies well below the present LHAASO upper limits. The MAGIC observations of the central source NGC $1275$ of the Perseus cluster are significantly higher than our results. Further, we estimated the cumulative $\gamma$-ray and neutrino fluxes from clusters with masses $\gtrsim 5\times 10^{13}, M_{\odot}$ in the local Universe (within $500$ Mpc). The diffuse $\gamma$-ray flux reported by the Fermi-LAT collaboration is significantly higher than our results. Our predictions are consistent with IceCube's existing upper limits on the unresolved neutrino flux from galaxy clusters ($M > 10^{14}, M_{\odot}$) up to $z = 2$.

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 / 2 minor

Summary. The paper uses MHD simulations of the intracluster medium (temperature, gas density, magnetic fields) in Virgo, Perseus, and Coma combined with Monte Carlo cosmic-ray propagation to predict secondary gamma-ray and neutrino fluxes. It adopts the assumption that CR injection scales linearly with gas density, motivated by associations with turbulence and shocks. The central results are that predicted gamma-ray fluxes from the three clusters lie well below LHAASO upper limits (with MAGIC data for NGC 1275 noted as higher), the cumulative gamma-ray flux from clusters with M ≳ 5×10^13 M_⊙ within 500 Mpc is below the Fermi-LAT diffuse measurement, and the neutrino predictions are consistent with IceCube upper limits on unresolved flux from M > 10^14 M_⊙ clusters to z=2.

Significance. If the modeling holds, the work supplies concrete forward predictions for the contribution of local galaxy clusters to the diffuse high-energy neutrino and gamma-ray backgrounds. The combination of MHD fields with Monte Carlo CR transport is a methodological strength that avoids direct fitting to the messenger data being compared, allowing falsifiable tests against current and future limits. This can help prioritize multi-messenger follow-up of clusters and refine source population models.

major comments (2)
  1. [§2] §2 (Numerical Methods, Monte Carlo CR propagation): The absolute normalization of the CR density—and therefore the secondary gamma-ray and neutrino fluxes—is set by the assumption that injection scales linearly with gas density. No sensitivity analysis to alternative scalings (e.g., with magnetic-field strength, turbulence amplitude, or shock Mach number) or independent calibration against radio synchrotron data is presented. Because an order-of-magnitude shift in normalization would directly affect whether the fluxes remain “well below” LHAASO limits and “consistent with” IceCube limits, this assumption is load-bearing for the central claims.
  2. [Results section] Results for individual clusters (Virgo/Perseus/Coma) and cumulative flux section: The comparisons to LHAASO, MAGIC, Fermi-LAT, and IceCube limits are presented as direct statements without propagated uncertainties arising from the CR injection scaling or from variations in the MHD density fields. Adding even a simple range of scaling factors would show whether the “well below” and “consistent with” conclusions are robust or marginal.
minor comments (2)
  1. [§2] The description of the Monte Carlo step would benefit from an explicit equation for the CR injection rate (currently described only in prose) to make the normalization choice transparent.
  2. [Figures] Figure captions for the flux spectra should state the exact energy range and integration aperture used for the LHAASO and IceCube comparisons.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the constructive and detailed comments on our manuscript. We address each major point below and outline the revisions we will make to strengthen the presentation of our results and the robustness of our conclusions.

read point-by-point responses

  1. Referee: §2 (Numerical Methods, Monte Carlo CR propagation): The absolute normalization of the CR density—and therefore the secondary gamma-ray and neutrino fluxes—is set by the assumption that injection scales linearly with gas density. No sensitivity analysis to alternative scalings (e.g., with magnetic-field strength, turbulence amplitude, or shock Mach number) or independent calibration against radio synchrotron data is presented. Because an order-of-magnitude shift in normalization would directly affect whether the fluxes remain “well below” LHAASO limits and “consistent with” IceCube limits, this assumption is load-bearing for the central claims.

    Authors: We appreciate the referee’s emphasis on the normalization choice. Our adoption of linear scaling with gas density is explicitly motivated in the manuscript by the physical association of high-density regions with strong turbulence and shocks, which are expected to be efficient CR acceleration sites. While a comprehensive sensitivity study across alternative scalings (e.g., with B-field strength or Mach number) would indeed be valuable, it would require additional Monte Carlo runs that exceed the scope and resources of the present work. In the revised manuscript we will add a dedicated paragraph in §2 and the results section that quantifies the effect of rescaling the injection normalization by factors of 0.1–10. This will demonstrate that the predicted fluxes remain below the LHAASO and IceCube limits for variations up to an order of magnitude, thereby addressing the robustness concern without new simulations. We will also include a short discussion noting that our model is not calibrated to radio synchrotron data and is intended as a forward prediction; any future joint radio–gamma-ray analysis would be a natural extension. revision: partial

  2. Referee: Results for individual clusters (Virgo/Perseus/Coma) and cumulative flux section: The comparisons to LHAASO, MAGIC, Fermi-LAT, and IceCube limits are presented as direct statements without propagated uncertainties arising from the CR injection scaling or from variations in the MHD density fields. Adding even a simple range of scaling factors would show whether the “well below” and “consistent with” conclusions are robust or marginal.

    Authors: We agree that explicit uncertainty ranges would improve clarity. In the revised results section we will propagate a representative range of CR injection scaling factors (0.1–10) into the gamma-ray and neutrino flux predictions for both the individual clusters and the cumulative flux. These ranges will be shown as shaded bands or tabulated limits in the comparisons with LHAASO, MAGIC, Fermi-LAT, and IceCube data. For the MHD density fields, we will add a brief statement that the adopted distributions already reflect the specific simulation outputs and that any residual variations are sub-dominant compared with the injection normalization uncertainty. This addition will make the robustness of our “well below” and “consistent with” statements quantitatively evident. revision: yes

Circularity Check

0 steps flagged

No significant circularity; forward predictions from simulations and stated assumption

full rationale

The derivation relies on MHD simulations supplying gas density, temperature, and B-field maps, followed by Monte Carlo CR propagation to compute secondaries. The key normalization choice (CR injection scaling linearly with gas density) is explicitly labeled a primary assumption and physically motivated by turbulence/shock associations, not obtained by fitting to the LHAASO, Fermi-LAT, MAGIC, or IceCube data against which predictions are compared. No equations reduce the reported fluxes to quantities fitted from those observational limits, no self-citation chain supplies a uniqueness theorem or ansatz, and no renaming of known results occurs. The outputs remain independent forward-model predictions whose absolute scale is set by the external assumption rather than by construction from the target measurements.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

The model depends on one key assumption about cosmic-ray injection and inherits standard MHD and particle-physics inputs; no new particles or forces are introduced.

free parameters (1)
  • CR injection normalization / scaling factor with gas density
    The primary assumption introduces an overall normalization that must be chosen to match expected cosmic-ray energy densities; its specific value is not stated in the abstract.
axioms (1)
  • domain assumption CR injection scales with the gas density of clusters
    Explicitly identified as the primary assumption; motivated by turbulence and shocks in high-density regions but not derived from first principles within the paper.

pith-pipeline@v0.9.0 · 5591 in / 1324 out tokens · 65136 ms · 2026-05-13T04:57:12.624905+00:00 · methodology

discussion (0)

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Reference graph

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