Jet-Feedback on kpc scales: a review

Dipanjan Mukherjee

REVIEW 2 major objections 5 minor 5 cited by

Jet-Feedback on kpc scales: a review

T0 review · 2 major / 5 minor · reviewed 2026-08-07 · deepseek-v4-flash

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Pith's one-line read Relativistic jets from active galactic nuclei couple strongly to their host galaxy's gas on kiloparsec scales, driving multi-phase outflows and altering star formation.

desk verdict A competent, honest review that consolidates the case for jets as kpc-scale ISM feedback agents; the central claim holds, but the quantitative coupling efficiencies should be labeled resolution-dependent. read the letter →

arxiv 2506.03888 v2 pith:YLGHFVH6 submitted 2025-06-04 astro-ph.GA astro-ph.HE

Dipanjan Mukherjee This is my paper · ORCID

classification astro-ph.GAastro-ph.HE

keywords AGNfeedbackrelativisticjetsjet-ISMinteractionmulti-phaseoutflowsinterstellarmediumgalacticturbulencestarformationnumericalsimulations

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

This review tries to establish that relativistic jets from active galactic nuclei couple strongly to the interstellar medium of their host galaxies on kiloparsec scales, in contrast to the older view that jets matter mainly for heating cluster-scale gas. The author traces three decades of numerical simulations, from early two-dimensional beam models to relativistic hydrodynamic runs with fractal, turbulent gas discs, and sets them beside spatially resolved observations of multi-phase gas. The synthesis points to a confinement phase, when the jet is trapped inside dense clumpy gas, as the stage of maximal energy transfer: jets can deposit roughly ten to twenty percent of their flux as kinetic energy in the ISM, raise gas turbulence by an order of magnitude, and drive fast outflows in several gas phases. The review concludes that jets therefore belong in the same feedback category as quasar winds, with consequences for how star formation and black hole growth are regulated.

What carries the argument

The organising mechanism is the three-phase life cycle of a jet in an inhomogeneous medium: the confined phase, the breakout phase, and the classical phase. During the confined phase, dense clouds act as obstacles that stall the jet head, and the jet plasma percolates through gaps in a 'flood-channel' pattern; the stalled beam's energy is redistributed into an overpressured bubble bounded by a forward shock. The review also carries an analytic estimate of the confinement timescale, obtained by equating the relativistic momentum flux of the jet to the ram pressure of clouds and writing the travel time through a scale height in terms of the jet power, cloud density, and volume filling factor. This machinery selects which jets stay trapped long enough to couple strongly with the ISM, and it is supplemented by a turbulence-regulated star formation prescription that converts local density, Mach number, and virial parameter into a star formation rate.

What would settle it

Run the same jet-and-galaxy setup at resolutions that resolve the 0.014–1 pc cooling lengths at cloud surfaces and compare outflow masses, velocities, and multi-phase structure; if the resolved runs show substantially weaker ablation or different cloud shredding than the existing simulations, the central claim about strong jet–ISM coupling would need to be scaled back.

Watch

Extended reading notes

Core claim

On the paper's own terms, the discovery being argued for is that a relativistic jet acts as a direct feedback agent on its host ISM rather than only as a heater of large-scale environments. During the confined phase before breakout, the jet beam is diverted through low-density channels between clouds, while its backflow inflates a quasi-spherical, pressurized bubble that sweeps the surrounding gas. This bubble ablates clouds, accelerates warm dense gas to hundreds of kilometres per second, and excites a hot tenuous outflow, producing the multi-phase outflow structure seen in observations of sources such as IC 5063 and B2 0258+35. A further claim is that jets can affect a volume of the ISM much larger than their apparent radio width, so the radio beam underestimates the footprint of feedback. The long-term outcome is usually not a blowout: only a small fraction of the ISM escapes the galaxy, and most uplifted gas falls back in a fountain, while star formation is modified both negatively and positively depending on local conditions.

Load-bearing premise

The load-bearing premise is that idealized numerical setups—static fractal gas distributions, pressure-equilibrated clouds, and single-fluid thermodynamics—capture the essential physics of how real jets couple to the clumpy interstellar medium, even though cloud-surface cooling is not resolved.

Editorial extensions

If this is right

During the confined phase, jets transfer on the order of 10–20% of their energy flux into the kinetic energy of ISM gas, making this phase the main channel of kpc-scale jet feedback.
A jet can stir a volume of the gas much larger than its radio beam, so narrow jets in observed galaxies do not imply weak feedback.
The efficiency of coupling is set by four parameters: jet power, orientation relative to the gas disk, volume filling factor of dense gas, and cloud density; low-power jets can remain confined for many megayears.
Only about ten percent of the ISM escapes the galaxy in such simulations; the rest returns in a galactic fountain, so jet feedback predominantly redistributes gas rather than ejecting it.
Applying turbulence-regulated star formation models, the jet mildly suppresses global star formation at onset while creating local, shock-compressed regions of enhanced star formation until breakout.

Reading between the lines

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

If the confined-phase coupling is as strong as this review argues, the traditional split between quasar-mode and radio-mode feedback needs revision: low-power, radio-quiet jets may contribute as much as winds to establishment-mode feedback in gas-rich hosts.
Because the simulated cooling lengths at cloud surfaces are one to two orders of magnitude below current resolution, converged simulations will likely revise the quoted 10–20% coupling efficiency; targeted observations of outflow energetics could provide the empirical anchor for that calibration.
The predicted enhancement of velocity dispersion perpendicular to the jet axis is a clean, testable diagnostic: existing IFU surveys already show it, and a systematic comparison between jet inclination and measured line widths would confirm whether the flood-channel mechanism operates as modelled.

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Editorial analysis

A structured set of objections, weighed in public.

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

Desk Editor's Note

read the letter

The thing to know: this is a review, not a new result, but it's a good one. It makes the case that relativistic jets act as local feedback agents in the host ISM on kpc scales, beyond their well-known role as cluster-scale heaters, and the case holds.

What it does well: the historical sweep from early jet-beam simulations through to current relativistic jet-ISM work is clear and well organized. The three-phase picture (confined, breakout, classical) gives a useful framework. The discussion of multiphase outflows, turbulence, and star formation effects is grounded in the cited literature, including independent groups (Gaibler, Tanner and Weaver, Talbot et al.), so the core claim doesn't rest solely on the author's own simulations. Appendix A's confinement-time estimate is a modest but clean extension of standard jet-head advance scalings with a volume-filling-weighted average, and it matches the simulation results quoted. The observational table in Appendix B is a genuinely handy resource.

Soft spots: the paper is honest about its biggest caveat, and it's a real one. Section 5.5 states that cooling lengths at cloud surfaces are ~0.014-1 pc, well below the grid resolution (typically >10 pc). That means the simulated ablation, cloud shredding, and multiphase structure are not converged. The main text still quotes ~10-20% kinetic energy coupling and shows the phase-space distribution (Fig. 4) as established findings; those numbers should be labeled as resolution-dependent. The caveat is in the paper, but it's separated from the numbers. That's the one substantive thing I'd want fixed. Also, the review leans on the author's own series, though not problematically, and there are minor production artifacts (template formatting, a reference-numbering jump) that don't affect content.

For whom: a graduate student or a researcher entering this area will get a lot out of it; someone working in jet-ISM interaction will find a useful summary and a good reference list. It deserves a serious referee. I'd recommend accepting it with a revision that moves the resolution caveat closer to the figures and tables that depend on it.

Referee Report

2 major / 5 minor

Summary. This review synthesizes numerical simulation studies and observations of relativistic AGN jets interacting with the host galaxy ISM on kiloparsec scales. It traces the historical development from 1980s beam simulations to modern relativistic hydrodynamics with static fractal and turbulent ISM setups, defines three jet evolutionary phases (confined, breakout, classical), and summarizes simulated impacts on ISM kinematics, multiphase gas, turbulence, and star formation. It also compiles observational evidence in a table (Appendix B) and presents an analytical estimate of the confined-phase duration (Appendix A). The paper's central claim is that jets couple strongly to the kpc-scale ISM, particularly during the confined phase, transferring about 10-20% of their kinetic energy to the gas and driving multiphase outflows; this is supported by both simulations and observations.

Significance. If accepted, the review provides a useful and timely synthesis of a field that has moved from 'jets heat clusters' to 'jets also affect host galaxies.' Its main strengths are the explicit treatment of simulation technique limitations (Section 5.5), a self-contained analytical model of confinement timescales (Appendix A), and a carefully compiled observational catalogue (Table A1). It draws on independent simulation groups (Gaibler, Dugan, Tanner and Weaver, Talbot et al., Cielo et al.) in addition to the author's own series, and the qualitative conclusions are consistent with resolved observations such as IC 5063 and B2 0258+35. The review is honest about open questions, including unresolved cooling lengths, short runtimes, missing magnetic fields and cosmic rays. Because it is a review, the numerical efficiency figures it quotes are not new results; the main risk is that readers may over-interpret resolution-dependent numbers as robust.

major comments (2)

[Section 3.1 and Section 3.3.1 (Figure 4)] The quoted kinetic-energy coupling efficiencies (10-20%) and the multiphase phase-space classification are load-bearing for the paper's emphasis on the confined phase, but the simulations from which they are drawn do not resolve the cooling lengths (0.014-1 pc) quoted in Section 5.5. The main text should explicitly caveat these numbers as resolution-dependent at the point of first use (e.g., 'in the currently achievable resolution regime'), with a cross-reference to Section 5.5, rather than presenting them as established values.
[Appendix A, Equation (A5)] The numerical coefficient 1.75e3 km/s does not follow from Equation (A4) with the stated fiducial values unless the ambient density includes a mean molecular weight mu approximately 0.6. The text never defines whether na is hydrogen number density or total gas number density, nor the assumed mu. Please state the assumed mu (or correct the coefficient); this affects the quantitative values in Figure A1, although the qualitative scaling is unchanged.

minor comments (5)

[Section 3.3.1 (Hot tenuous outflow)] The text refers to 'the phase-space distributions of Fig. 3' but the quantity being described is shown in Figure 4; please correct the cross-reference.
[Reference list and citation [486]] Reference [486] appears between [206] and [208] with no [207], and the citation to 'shock precursors [486]' in Section 3.3.1 uses this out-of-sequence number; a global renumbering pass would be helpful.
[Appendix B, row 41] The source name is given as 'PKS 2152-69' in the main text and Table A1 but as 'PKS B2152-699' in reference [221]; please unify the name.
[Figure 4 caption] The caption contains the typo 'Several distinct phases have been be identified'; please remove the repeated 'be'.
[Header metadata] The Received/Accepted dates and copyright year (copyright 2024) are inconsistent with the 2025 submission/acceptance dates; please check issue metadata at production.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: central claims are supported by independent simulations and observations; the analytical appendix is derived from standard momentum-flux balance, not from the simulations it is compared with.

full rationale

This paper is a review, so its 'derivation chain' is mainly a synthesis of the literature. The central claim that relativistic jets couple strongly to the kpc-scale ISM and drive multiphase outflows is supported by non-overlapping groups (Gaibler et al., Dugan et al., Tanner & Weaver, Talbot et al.) and by independent observations of IC 5063, B2 0258+35, and 4C 31.04, among others. The quantitative coupling efficiencies (~10-20% kinetic energy transfer) are presented as simulation outputs, not as predictions derived from fitted parameters, so no fitted-input-renamed-as-prediction pattern occurs. Appendix A derives jet confinement timescales from a standard jet-head momentum-flux balance, citing Martí et al. 1997 and Bicknell 1994, and then compares the analytic estimate with simulations as a consistency check; the comparison is not used to calibrate the formula. The self-citations (e.g., Mukherjee et al. 2020 for typical jet parameters) are minor literature references and are not load-bearing; no uniqueness theorem, ansatz, or known result is smuggled in via self-citation. The acknowledged resolution limitation in Section 5.5 (cooling lengths 0.014-1 pc below grid resolution) is a genuine correctness risk for quantitative efficiencies, but it is not a circularity: the review explicitly flags it rather than assuming it away. The analytical derivation in Appendix A is self-contained and independent of the simulation results it later agrees with, so the review does not reduce to its own inputs.

Assumptions & free parameters 0 free parameters · 3 assumptions · 0 invented entities

The review uses standard relativistic hydrodynamics and domain assumptions about ISM structure. No data are fitted and no new entities are introduced; the Appendix A estimate uses illustrative jet and ISM parameters rather than fitted values.

assumptions (3)

standard math Momentum balance at the jet working surface determines the jet-head advance speed (Equations A3-A5).
Standard shock and ram-pressure balance used across the jet literature, inherited from Begelman and Cioffi 1989 and Marti et al. 1997.
domain assumption A static fractal density distribution with pressure-equilibrated clouds represents the clumpy ISM of the host galaxy.
Introduced by Sutherland and Bicknell 2007 and Wagner et al. 2012; the review's conclusions inherit this idealized representation of the ISM.
domain assumption Single-fluid approximation with tabulated cooling captures the multi-phase outflow structure.
The paper admits in Sections 3.3.1 and 5.5 that explicit chemistry and cooling length resolution are missing; the phase-averaged picture rests on this approximation.

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Cite this review

Pith. "Pith review of Jet-Feedback on kpc scales: a review." pith.science (2026). https://pith.science/paper/YLGHFVH6

@misc{pith2026250603888,
  author       = {Pith},
  title        = {Pith review of: Jet-Feedback on kpc scales: a review},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/YLGHFVH6}},
  note         = {Machine review of arXiv:2506.03888}
}

read the original abstract

Relativistic jets from AGN are an important driver of feedback in galaxies. They interact with their environments over a wide range of physical scales during their lifetime, and an understanding of these interactions is crucial for unraveling the role of supermassive blackholes in shaping galaxy evolution. The impact of such jets have been traditionally considered in the context of heating the large-scale environments. However, in the last few decades there has been additional focus on the immediate impact of jet feedback on the host galaxy itself. In this review we outline the development of various numerical simulations since the onset of studies of jets to the present day, where sophisticated numerical techniques have been employed to study jet feedback including a range of physical processes. The jets can act as an important agent of injecting energy in the host's ISM, as confirmed both in observations of multi-phase gas, as well as in simulations. Such interactions have the potential to impact the kinematics of the gas as well as its star formation. We summarize the recent results from simulations of jet feedback on kpc scales, and outline the broader implications for observations and galaxy evolution.

Figures

Figures reproduced from arXiv: 2506.03888 by the authors.

**Figure 1.** A cartoon of a jet and its cocoon evolving in a homogeneous medium (left) and clumpy ISM (right). The jet in a smooth homogeneous medium has a collimated beam with recollimation shocks, a conical forward shock, followed by contact discontinuity corresponding to the density jump between the cocoon filled by the non-thermal jet material and the swept-up gas from the external medium. A jet in an inhomogeneous ISM resul… view at source ↗

**Figure 2.** Three-dimensional visualizations of density distribution of a fractal cloud being impacted by an AGN-driven wind, from the simulation GC45_K3 of Mandal et al. [166]. The top right panel corresponds to the initial compression phase, which is followed by the onset of ablation due to Kelvin–Helmholtz instabilities and shear flows (lower left panel). The cloud is seen to eventually disperse several mini-cloudlets, which… view at source ↗

**Figure 3.** Evolution of a jet through a dense kpc scale gas disk, depicting the three phases of evolution outlined in Section 3.1. The 3D visualizations show the gas temperature (log(T)) and the jet tracer in blue at different times. The results are from simulation B of Mukherjee et al. 2018b [172], where a jet of power Pj = 1045 erg s−1 is launched perpendicular to the disk plane. The red-colored contours trace the cocoon of … view at source ↗

Figures from the paper (2 more)

**Figure 4.** Figure 4: A 3D visualization of mass distribution as a function of positive radial velocity (vr), density (n) and temperature (T), to depict the multi-phase nature of the jet-impacted ISM. The results are from the data corresponding to the last panel of [PITH_FULL_IMAGE:figures…

**Figure 5.** Figure 5: Top: Representation of the top two panels of Figures 5 and 6 from Girdhar et al. [230] showing enhanced kinematics in ionized and molecular gas of J1316+1753, a prototype of multiphase observation of jet–ISM interaction. Bottom: Representation of the middle panel of …

Discussion (0). Continue with ORCID to comment.

Forward citations

Cited by 5 Pith papers

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Reference graph

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