Simulating realistic radio morphologies of Fanaroff-Riley I jets in a self-regulating cool-core cluster

Christoph Pfrommer; Joseph Whittingham; L\'ena Jlassi; Maria Werhahn; Philipp Girichidis; Rainer Weinberger

REVIEW 2 major objections 1 minor 2 cited by

Simulating realistic radio morphologies of Fanaroff-Riley I jets in a self-regulating cool-core cluster

T0 review · 2 major / 1 minor · reviewed 2026-06-28 · grok-4.3

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗

Pith's one-line read Self-regulated AGN jets in cool-core clusters produce realistic Fanaroff-Riley I radio morphologies and prevent cooling flows.

desk verdict Self-regulated jets here give disturbed FRI morphologies and explain equal lobe extents across frequencies via the tracer-evolved electrons, but the result rests on an uncalibrated sub-grid CR acceleration model. read the letter →

arxiv 2606.04084 v1 pith:5D7BVWWL submitted 2026-06-02 astro-ph.GA astro-ph.HE

Léna Jlassi , Rainer Weinberger , Christoph Pfrommer , Maria Werhahn , Joseph Whittingham , Philipp Girichidis This is my paper · ORCID

classification astro-ph.GAastro-ph.HE

keywords AGNjetscool-coregalaxyclustersFanaroff-RileyImorphologiescosmicrayelectronsradiosynchrotronemissionself-regulatedfeedbackFokker-Planckevolution

verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

The paper uses magneto-hydrodynamical simulations of an idealized Perseus-like galaxy cluster where accretion powers low-density jets. These jets accelerate cosmic rays via a sub-grid model, and cosmic ray electron spectra are evolved along Lagrangian tracers with the Crest Fokker-Planck solver to generate synchrotron radio emission. The central result is that self-regulated jets stabilize the cluster core against cooling flows and yield complex, disturbed Fanaroff-Riley I lobe shapes. In contrast, a single fixed-power outburst produces only symmetrical lobes. Mock observations viewed along the jet axis still display complex structures because light jets are deflected by cold gas structures, and the model accounts for similar radio lobe extents across 150 MHz to 1.4 GHz frequencies in the simulated 1-50 microGauss magnetic fields.

What carries the argument

Self-regulating accretion-powered low-density AGN jets with a sub-grid cosmic ray acceleration model, using the Crest Fokker-Planck solver to evolve electron spectra along Lagrangian tracers and compute radio synchrotron emission.

What would settle it

If multi-frequency radio maps of cool-core clusters like Perseus show symmetric lobes despite ongoing AGN activity, or if lobe spatial extents differ markedly between 150 MHz and 1.4 GHz in regions with 1-50 microGauss fields, the central claims would be challenged.

Watch

Extended reading notes

Core claim

Self-regulated AGN jets stabilize the cool-core cluster against cooling flows and produce realistic Fanaroff-Riley I (FRI) and disturbed lobe morphologies, in contrast to symmetrical lobe structures obtained with a single jet outburst of fixed power. Our mock radio observations are viewed in a blazar configuration - along the jet axis - and exhibit complex radio-emitting lobe structures despite this. This highlights the strong deflection of light jets by cold gas structures and suggests that small-scale black hole and jet properties cannot be inferred from kpc-scale FRI radio lobe morphologies. Combining self-consistently evolved magnetic fields and electron spectra enables us to explain a k

Load-bearing premise

The sub-grid model used to accelerate cosmic ray protons and electrons by the jets, when combined with the Fokker-Planck evolution in Crest along Lagrangian tracers, produces radio synchrotron emission that accurately represents real observations.

Editorial extensions

If this is right

Self-regulated jets maintain thermal balance in the cluster core by responding to accretion rates.
Disturbed FRI morphologies arise primarily from jet deflection by cold gas rather than variations in jet power.
Small-scale properties of the central black hole and jets cannot be directly read from observed kpc-scale lobe shapes.
Both young and old cosmic ray electrons contribute to radio emission across 150 MHz to 1.4 GHz in typical cool-core magnetic fields.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

Jet deflection by cold gas structures may be a general process limiting what can be inferred about jet launching from large-scale radio maps.
The same simulation framework could be used to predict how radio morphologies evolve in clusters with different masses or dynamical states.
If the sub-grid cosmic ray model is accurate, these simulations provide a way to interpret upcoming wide-field radio surveys of galaxy clusters.

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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit.

Desk Editor's Note

read the letter

The main thing to know is that these simulations of a Perseus-like cool-core cluster show self-regulated AGN jets stabilizing the core while producing complex, deflected FRI-like radio lobes when viewed along the axis, in contrast to the symmetric structures from a single fixed-power outburst. They also account for the observed similar spatial extents at 150 MHz and 1.4 GHz because both fresh and aged electrons radiate in the 1-50 μG fields.

What is new is the combination of accretion-responsive jet feedback with Lagrangian tracers running the Crest Fokker-Planck solver to evolve cosmic-ray electron spectra alongside the MHD fields. This produces the mock observations and highlights how cold gas deflects the light jets, so kpc-scale lobe shapes do not reveal small-scale black-hole or jet details.

The setup works well for demonstrating that contrast and for linking the magnetic-field and electron evolution to the frequency-independent extents. The method is a clear step past simpler fixed-power or single-outburst runs.

The soft spot is the sub-grid prescription that accelerates cosmic-ray protons and electrons at the jet. The morphological realism and the equal-extent claim both depend on whether that injection plus the subsequent losses accurately populate the ~GeV electrons that emit in the observed bands. The abstract supplies no quantitative spectral-index or luminosity matches to real Perseus sources, so the stress-test concern about the accuracy of the synchrotron maps stands. Without calibration or direct comparison metrics, the interpretation for observations stays provisional.

This is for people running or using AGN feedback simulations in clusters and for observers who want mock radio data. A reader focused on methodological advances in tracer-based CR evolution would find it useful. The work shows clear engagement with the modeling problem and deserves peer review to examine the sub-grid choices and any validation added in the full text.

Referee Report

2 major / 1 minor

Summary. The manuscript presents MHD simulations of an idealized Perseus-like cool-core cluster in which accretion-powered jets self-regulate via a sub-grid cosmic-ray acceleration model. Electron spectra are evolved along Lagrangian tracers with the Crest Fokker-Planck solver to generate mock synchrotron maps viewed along the jet axis; the central claims are that these self-regulated jets stabilize the core against cooling flows, produce realistic FRI and disturbed lobe morphologies (unlike symmetric lobes from fixed-power outbursts), and explain the observational fact of similar lobe extents at 150 MHz–1.4 GHz in the simulated 1–50 μG fields.

Significance. If the mock radio images are shown to be quantitatively consistent with observations, the work would strengthen the case that self-regulated AGN feedback can simultaneously quench cooling flows and reproduce complex FRI structures. A clear strength is the self-consistent coupling of evolved magnetic fields with the Crest-evolved electron spectra, which directly addresses the frequency-extent puzzle without ad-hoc assumptions about electron populations.

major comments (2)

[Abstract] Abstract: the headline claim that the simulations 'produce realistic Fanaroff-Riley I (FRI) and disturbed lobe morphologies' is load-bearing for the paper's main result, yet the abstract (and the provided summary) supplies no quantitative metrics such as lobe asymmetry indices, surface-brightness profiles, or direct spectral-index comparisons to observed Perseus FRI sources; without these, it is impossible to assess whether the sub-grid CR model plus Crest evolution actually reproduces the target morphologies.
[Abstract] Abstract: the explanation that 'both freshly accelerated and hundreds-of-Myr-old electrons are able to contribute to the 150 MHz–1.4 GHz frequency range' in 1–50 μG fields rests on the accuracy of the unspecified sub-grid CR acceleration efficiency and the subsequent Fokker-Planck losses; no calibration, sensitivity tests, or comparison of predicted luminosities/spectral indices against real Perseus data are described, directly affecting the robustness of both the morphological and frequency-extent claims.

minor comments (1)

[Abstract] The term 'blazar configuration' for the line-of-sight viewing angle should be defined or replaced with a clearer description of the projection geometry.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive comments on our manuscript. We respond to each major comment below.

read point-by-point responses

Referee: [Abstract] Abstract: the headline claim that the simulations 'produce realistic Fanaroff-Riley I (FRI) and disturbed lobe morphologies' is load-bearing for the paper's main result, yet the abstract (and the provided summary) supplies no quantitative metrics such as lobe asymmetry indices, surface-brightness profiles, or direct spectral-index comparisons to observed Perseus FRI sources; without these, it is impossible to assess whether the sub-grid CR model plus Crest evolution actually reproduces the target morphologies.

Authors: We agree that the abstract's use of 'realistic' would be strengthened by quantitative metrics. The manuscript demonstrates the key physical result through direct comparison: self-regulated jets produce complex, disturbed lobe structures via deflection by cold gas, in contrast to the symmetric lobes from fixed-power outbursts. This qualitative distinction is shown in the figures and arises self-consistently from the simulation physics. We will revise the abstract to state that the simulations 'produce complex FRI-like and disturbed lobe morphologies' to more accurately reflect the nature of the comparison presented. revision: partial
Referee: [Abstract] Abstract: the explanation that 'both freshly accelerated and hundreds-of-Myr-old electrons are able to contribute to the 150 MHz–1.4 GHz frequency range' in 1–50 μG fields rests on the accuracy of the unspecified sub-grid CR acceleration efficiency and the subsequent Fokker-Planck losses; no calibration, sensitivity tests, or comparison of predicted luminosities/spectral indices against real Perseus data are described, directly affecting the robustness of both the morphological and frequency-extent claims.

Authors: The sub-grid cosmic-ray acceleration model, including the efficiency parameter, is fully specified in the methods section, with values drawn from standard AGN jet models. Magnetic fields are evolved self-consistently in the MHD simulation and reach 1–50 μG in the lobe regions. The Crest Fokker-Planck solver then evolves the electron spectra including all relevant losses. This setup directly shows that, for these B-field strengths, synchrotron frequencies in the 150 MHz–1.4 GHz range receive contributions from both young and old electrons. The simulation is idealized and not tuned to match specific Perseus luminosities or spectral indices; the goal is to illustrate the mechanism for frequency-independent extents. We will add a short paragraph in the revised manuscript discussing the model assumptions and parameter choices. revision: partial

Circularity Check

0 steps flagged · score 0.0 of 10

No circularity: forward simulation chain is self-contained

full rationale

The derivation proceeds via explicit MHD simulations of a Perseus-like cluster, sub-grid jet-powered CR acceleration, Lagrangian tracer evolution with the external Crest Fokker-Planck solver, and post-processed synchrotron maps. No parameter is fitted to the target FRI morphologies, no self-citation supplies a uniqueness theorem or ansatz that forces the outcome, and the contrast to fixed-power outbursts follows directly from the self-regulated accretion model rather than from re-labeling inputs. The central claims therefore remain independent of the reported results.

Assumptions & free parameters 2 free parameters · 2 assumptions · 0 invented entities

The central claim rests on standard MHD and cosmic-ray transport physics plus several sub-grid modeling choices whose parameters are not specified in the abstract. No new particles or forces are introduced.

free parameters (2)

jet power response function
Self-regulation requires a prescription linking jet power to local accretion or cooling rate; this is a fitted or chosen functional form.
cosmic-ray acceleration efficiency
Sub-grid model parameter controlling the fraction of jet energy converted into CR protons and electrons.

assumptions (2)

domain assumption Idealised Perseus-like initial conditions accurately represent a real cool-core cluster
The simulation begins from a specific, simplified cluster setup.
domain assumption Crest Fokker-Planck solver correctly evolves electron spectra under the simulated conditions
Relies on the numerical accuracy and physical completeness of the solver.

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Cite this review

Pith. "Pith review of Simulating realistic radio morphologies of Fanaroff-Riley I jets in a self-regulating cool-core cluster." pith.science (2026). https://pith.science/paper/5D7BVWWL

@misc{pith2026260604084,
  author       = {Pith},
  title        = {Pith review of: Simulating realistic radio morphologies of Fanaroff-Riley I jets in a self-regulating cool-core cluster},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/5D7BVWWL}},
  note         = {Machine review of arXiv:2606.04084}
}

abstract

Active galactic nucleus (AGN) jets radiate radio synchrotron emission displaying a wide range of morphologies. At the same time, they provide heat to prevent cooling flows in cool-core galaxy clusters. We produce mock radio observations of AGN jets in a self-regulating cool-core galaxy cluster. To this end, we employ magneto-hydrodynamical simulations of an idealised Perseus-like galaxy cluster, in which accretion-powered low-density jets accelerate cosmic ray protons and electrons by means of a sub-grid model. Cosmic ray electron spectra are spatially and temporally evolved along Lagrangian tracer trajectories using the Fokker-Planck solver Crest to produce radio synchrotron emission. Self-regulated AGN jets stabilize the cool-core cluster against cooling flows and produce realistic Fanaroff-Riley I (FRI) and disturbed lobe morphologies, in contrast to symmetrical lobe structures obtained with a single jet outburst of fixed power. Our mock radio observations are viewed in a blazar configuration - along the jet axis - and exhibit complex radio-emitting lobe structures despite this. This highlights the strong deflection of light jets by cold gas structures and suggests that small-scale black hole and jet properties cannot be inferred from kpc-scale FRI radio lobe morphologies. Combining self-consistently evolved magnetic fields and electron spectra enables us to explain a known observational phenomenon, whereby radio observations of AGN lobes on galaxy cluster scales occasionally display similar spatial extents at different frequencies: in 1-50 $\mu$G magnetic fields obtained in our cool-core environment, both freshly accelerated and hundreds-of-Myr-old electrons are able to contribute to the 150 MHz - 1.4 GHz frequency range.

Figures

Figures reproduced from arXiv: 2606.04084 by the authors.

**Figure 1.** Projections of self-regulated AGN jets in a Perseus-like galaxy cluster at t = 1.44 Gyr. Top: From left to right, volume-weighted gas mass density, magnetic field strength, CR proton energy density, and the CR electron energy density multiplied by 1/ξcre = 100, where ξcre is our chosen efficiency of CR proton to CR electron energy conversion (Sect. 2.5.1). Bottom: From left to right, we show the volume-weighted jet … view at source ↗

**Figure 2.** Synchrotron intensity maps at 150 MHz of self-regulated AGN jets at different epochs, in comparison with the single jet outburst in the bottom right corner presented in J26. We smooth the image using a symmetric 2D beam with FWHM = 7 ′′ ≈ 2.7 kpc (depicted in panel A at the bottom right) to mock observationally motivated angular resolutions, and use the conversion 1 Jy beam−1 = 0.018 Jy arcsec−2 . We draw contours a… view at source ↗

**Figure 3.** Synchrotron intensity maps projected along three different axes at 150 MHz of a single snapshot at t = 1.46 Gyr (see movie), and smoothed with a 2D Gaussian beam FWHM = 4 kpc. The cartoon in the upper right illustrates the jet launching direction. The bottom left image in the cube is obtained by projecting along the jet launching axis, as is the case for the mock images shown in [PITH_FULL_IMAGE:figures/full_fig_p0… view at source ↗

Figures from the paper (3 more)

**Figure 4.** Figure 4: Bottom: Time evolution of the jet luminosity (black line) and 1.4 GHz radio luminosity (coloured line). The black and red dashed lines indicate the mean jet and radio luminosities, respectively. The jets are initially in an ‘intermittent’ phase with short, weak outburs…

**Figure 5.** Figure 5: Spatial and spectral distributions of different electron ages, defined as the time since last injection tsince inj, at t = 1.5 Gyr. We differentiate between young (age ≤ 4 Myr) and old (4 < age ≤ 400 Myr) CR electrons on the left and right, respectively. Electrons unde…

**Figure 6.** Figure 6: Multi-panel view of the AGN jet outburst at t = 1.5 Gyr (same time as [PITH_FULL_IMAGE:figures/full_fig_p013_6.png]

Discussion (0). Continue with ORCID to comment.

Forward citations

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Pith tools

Reviewed June 28, 2026 · model on record in the stance chip above.

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