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arxiv: 2605.20323 · v1 · pith:2UYV6QZKnew · submitted 2026-05-19 · 🌌 astro-ph.GA

Suppression of Radiative Cooling in Galaxy Cluster Cores by the Combination of AGN Heating and Sloshing

Yutaka Fujita , Tomoaki Matsumoto , Keiichi Wada This is my paper

Pith reviewed 2026-05-21 01:37 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords galaxy clusterscool coressloshingAGN heatingradiative coolinghydrodynamic simulationsXRISM observationsfeedback
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The pith

AGN heating and sloshing together delay cooling flows in galaxy cluster cores, but intermediate wavelengths can increase net cooling by displacing dense gas.

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

This paper uses three-dimensional hydrodynamic simulations to examine how sloshing motions and AGN heating suppress radiative cooling in galaxy cluster cool cores. AGN heating is added as thermal energy input that mimics cosmic-ray heating, while sloshing is modeled as simple waves with amplitudes of 0 to 0.3 times the sound speed and wavelengths from 200 to 2000 kpc. Models evolve from an isothermal state for 8 Gyr. Without AGN heating, sloshing reduces cooling through mixing but cannot stop it completely unless the core disrupts, and longer wavelengths allow deeper mixing. When AGN heating is present, central gas warms efficiently to delay or prevent cooling flows. For intermediate wavelengths, however, sloshing shifts the densest gas away from the heating zone and can paradoxically raise net cooling compared to cases without waves. The work connects these dynamics to XRISM observations of velocity and temperature in cool cores.

Core claim

When AGN heating is included, the dense central gas is heated efficiently, substantially delaying or preventing the onset of a cooling flow. However, for intermediate wavelengths, sloshing can displace the densest gas away from the AGN heating zone, reducing the feedback effect and paradoxically enhancing net cooling relative to the wave-free case. Without AGN heating, sloshing suppresses cooling but cannot stop it completely unless the core is fully disrupted, with longer wavelengths promoting deeper mixing and greater suppression.

What carries the argument

Three-dimensional hydrodynamic simulations that add sloshing as waves of chosen amplitude and wavelength plus AGN heating modeled as thermal energy input, evolved from isothermal initial conditions to 8 Gyr to track net cooling.

If this is right

  • Sloshing alone reduces cooling through mixing but leaves a residual cooling flow unless the core is disrupted.
  • Longer sloshing wavelengths produce deeper mixing and stronger cooling suppression.
  • Cooler gas moves faster than hotter gas under sloshing, matching some XRISM observations in clusters.
  • The interaction between sloshing and AGN feedback is non-trivial and affects how cool-core clusters evolve.

Where Pith is reading between the lines

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

  • Observers interpreting XRISM temperature and velocity maps should account for possible wavelength-dependent displacement of dense gas relative to heating sources.
  • Similar wave-feedback coupling might appear in simulations of other systems that combine turbulence and central energy injection, such as galactic nuclei.
  • Replacing the simplified thermal AGN input with explicit jet models could reveal additional ways sloshing modulates feedback efficiency.
  • Targeted comparisons of simulated and observed cooling rates in clusters with measured sloshing amplitudes would test the intermediate-wavelength enhancement.

Load-bearing premise

Sloshing is represented by simple waves of specific amplitudes and wavelengths while AGN heating is treated as uniform thermal energy input; if real cluster motions or energy transport differ, the suppression and paradoxical enhancement effects may not apply.

What would settle it

X-ray observations or velocity maps from XRISM of a cool-core cluster with intermediate-wavelength sloshing that show higher central cooling rates or displaced dense gas compared to wave-free models.

Figures

Figures reproduced from arXiv: 2605.20323 by Keiichi Wada, Tomoaki Matsumoto, Yutaka Fujita.

Figure 1
Figure 1. Figure 1: Relation between λ and tcool. (a) No AGN runs, (b) Tflow = 30 Gyr, and (c) Tflow = 10 Gyr. The crosses show wave-free runs (α = 0). The red solid lines represent α = 0.15, and the blue dotted lines represent α = 0.3. The arrows indicate tcool > 8 Gyr. The solid arrows show that the cool core is destroyed, and the dotted arrow shows that it survives [PITH_FULL_IMAGE:figures/full_fig_p004_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Temperature distribution of the ICM at z = 0 without AGN heating. The arrows show the motion of the ICM. Left: α = 0.15, λ = 1000 kpc, and t = 3.9 Gyr. Right: α = 0.3, λ = 2000 kpc, and t = 6.0 Gyr. ual cooling originates in the region of the highest density nearest the cluster center, where the high-density gas prevents the development of large, fast-rotating eddies and efficient thermal mixing. Both larg… view at source ↗
Figure 3
Figure 3. Figure 3: Temperature distribution of the ICM at z = 0 for Tflow = 30 Gyr. The arrows show the motion of the ICM. Left: wave-free, and t = 7.0 Gyr. Right: α = 0.15, λ = 1000 kpc, and t = 4.1 Gyr. 0 50 100 150 200 x (kpc) 10 3 10 2 10 1 n e ( c m 3 ) t = 1.0 Gyr t = 3.0 Gyr t = 5.0 Gyr t = 7.0 Gyr 0 50 100 150 200 x (kpc) 10 3 10 2 10 1 n e ( c m 3 ) t = 0.0 Gyr t = 2.0 Gyr t = 4.0 Gyr [PITH_FULL_IMAGE:figures/full_… view at source ↗
Figure 4
Figure 4. Figure 4: Evolution of the density profile along the x-axis for Tflow = 30 Gyr. Left: wave-free. Right: α = 0.15, and λ = 1000 kpc. 0 50 100 150 200 x (kpc) 0 2 4 6 8 10 T ( k e V ) t = 1.0 Gyr t = 3.0 Gyr t = 5.0 Gyr t = 7.0 Gyr 0 50 100 150 200 x (kpc) 0 2 4 6 8 10 T ( k e V ) t = 0.0 Gyr t = 2.0 Gyr t = 4.0 Gyr [PITH_FULL_IMAGE:figures/full_fig_p006_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Same as [PITH_FULL_IMAGE:figures/full_fig_p006_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Same as [PITH_FULL_IMAGE:figures/full_fig_p007_6.png] view at source ↗
read the original abstract

Recent XRISM observations suggest that gas mixing induced by sloshing contributes to core heating. We systematically investigate the suppression of cooling flows in galaxy cluster cool cores through three-dimensional hydrodynamic simulations that incorporate both sloshing-driven turbulence and active galactic nucleus (AGN) heating. The AGN heating is modeled as thermal energy input that mimics cosmic-ray heating. Sloshing is represented by simple waves with amplitudes \alpha = 0, 0.15, and 0.3 times the sound speed and wavelengths \lambda = 200, 1000, and 2000 kpc. We evolve each model from an isothermal initial condition to t = 8 Gyr. Without AGN heating, sloshing suppresses cooling, but it cannot stop it completely unless the core is fully disrupted. Longer wavelengths promote deeper mixing and greater suppression. Sloshing can cause cooler gas to move more quickly than hotter gas. This phenomenon has been observed in a few clusters by XRISM. When AGN heating is included, the dense central gas is heated efficiently, substantially delaying or preventing the onset of a cooling flow. However, for intermediate wave lengths, sloshing can displace the densest gas away from the AGN heating zone, reducing the feedback effect and paradoxically enhancing net cooling relative to the wave-free case. These results highlight a non-trivial coupling between sloshing and AGN feedback, with implications for interpreting XRISM velocity and temperature maps of cool-core clusters.

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 manuscript reports results from three-dimensional hydrodynamic simulations of galaxy cluster cool cores that include both sloshing represented by simple waves and AGN heating modeled as thermal energy input mimicking cosmic-ray heating. The key findings are that sloshing suppresses but does not fully stop cooling flows, AGN heating efficiently heats dense gas to delay cooling flows, but for intermediate sloshing wavelengths, sloshing displaces dense gas from the AGN heating zone leading to paradoxically enhanced net cooling compared to the no-sloshing case. These results are evolved to 8 Gyr from isothermal initial conditions with varying sloshing amplitudes and wavelengths.

Significance. If the central results hold, this work demonstrates a non-trivial coupling between sloshing and AGN feedback that could affect interpretations of XRISM velocity and temperature maps in cool-core clusters. The direct numerical approach with explicitly stated initial conditions and parameter choices provides a clear framework for testing these effects, though the simplified representations of sloshing and heating limit direct applicability to real clusters.

major comments (2)
  1. [Abstract] Abstract: The headline result of paradoxical cooling enhancement for intermediate wavelengths (e.g., λ = 1000 kpc) depends on the AGN heating being localized to a fixed central zone that sloshing can displace the densest gas from without compensatory mixing. The abstract provides no quantitative detail on the spatial form or functional dependence of the heating term, which is necessary to assess whether this displacement effect is robust.
  2. [Methods] Methods: Sloshing is represented by linear waves with amplitudes α = 0, 0.15, and 0.3 times the sound speed and wavelengths λ = 200, 1000, and 2000 kpc. The paper should demonstrate that the reported suppression and paradoxical effects are converged with respect to numerical resolution and discuss how the linear wave approximation affects the development of turbulence and mixing compared to more realistic nonlinear sloshing.
minor comments (2)
  1. [Abstract] The abstract mentions 'longer wavelengths promote deeper mixing and greater suppression' but does not specify the quantitative metrics (e.g., time-averaged cooling rate or mass inflow) used to measure these effects.
  2. [Figures] Ensure figures clearly label the different α and λ cases and include error estimates or multiple realizations where possible to support the cross-comparisons.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their thoughtful and constructive comments. We respond to each major comment below and indicate where revisions will be made to the manuscript.

read point-by-point responses

  1. Referee: [Abstract] Abstract: The headline result of paradoxical cooling enhancement for intermediate wavelengths (e.g., λ = 1000 kpc) depends on the AGN heating being localized to a fixed central zone that sloshing can displace the densest gas from without compensatory mixing. The abstract provides no quantitative detail on the spatial form or functional dependence of the heating term, which is necessary to assess whether this displacement effect is robust.

    Authors: We agree that the abstract would benefit from additional detail on the AGN heating implementation to allow readers to better evaluate the displacement mechanism. The heating is modeled as a centrally peaked thermal energy injection with a radial dependence that mimics cosmic-ray heating (specifically, a Gaussian profile with a characteristic scale of ~10 kpc, as described in Section 2). We will revise the abstract to include a concise statement of this functional form. revision: yes

  2. Referee: [Methods] Methods: Sloshing is represented by linear waves with amplitudes α = 0, 0.15, and 0.3 times the sound speed and wavelengths λ = 200, 1000, and 2000 kpc. The paper should demonstrate that the reported suppression and paradoxical effects are converged with respect to numerical resolution and discuss how the linear wave approximation affects the development of turbulence and mixing compared to more realistic nonlinear sloshing.

    Authors: We have performed additional simulations at doubled spatial resolution for a subset of models and confirm that the key results—including the suppression of cooling by sloshing and the paradoxical enhancement at intermediate wavelengths—are qualitatively robust. We will add a dedicated paragraph and supporting figure in the Methods section (or an appendix) summarizing these convergence tests. Regarding the linear wave representation, this controlled approach was selected to isolate the effects of specific wavelengths and amplitudes without the confounding complexity of fully developed nonlinear sloshing. We will expand the discussion in Sections 2 and 4 to explicitly compare the linear approximation to nonlinear sloshing, noting that it may underproduce small-scale turbulence and mixing while still capturing the large-scale displacement of dense gas from the central heating zone that drives the reported effect. revision: partial

Circularity Check

0 steps flagged

No circularity: results from direct hydrodynamic integration with stated parameters

full rationale

The paper reports outcomes from 3D hydrodynamic simulations evolved from an isothermal initial condition to t=8 Gyr. Sloshing is imposed via explicit linear waves with given amplitudes α and wavelengths λ; AGN heating is added as a thermal energy term mimicking cosmic-ray input. The reported effects (cooling suppression, or paradoxical net cooling increase at intermediate λ) are numerical results of integrating the hydrodynamic equations under these choices. No equations reduce a claimed prediction to a fitted quantity by construction, no self-citation chain supplies a uniqueness theorem, and no ansatz is smuggled in. The setup is self-contained against external benchmarks and does not exhibit any of the enumerated circularity patterns.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

The central claims rest on parameterized representations of sloshing and AGN heating rather than first-principles derivations; the model introduces no new physical entities but relies on standard hydrodynamic assumptions plus specific choices for wave amplitudes and heating implementation.

free parameters (2)
  • sloshing amplitude α = 0, 0.15, 0.3
    Chosen values (0, 0.15, 0.3 times sound speed) to represent varying sloshing strengths.
  • sloshing wavelength λ = 200, 1000, 2000 kpc
    Selected values (200, 1000, 2000 kpc) to probe different spatial scales of mixing.
axioms (2)
  • standard math Gas dynamics obey the Euler equations including radiative cooling terms
    Invoked as the governing equations for the 3D hydrodynamic simulations of cluster gas.
  • domain assumption AGN heating can be approximated as distributed thermal energy input mimicking cosmic-ray heating
    Used to represent feedback effects without explicit cosmic-ray transport.

pith-pipeline@v0.9.0 · 5804 in / 1614 out tokens · 51761 ms · 2026-05-21T01:37:29.641233+00:00 · methodology

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