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arxiv: 2606.25801 · v1 · pith:CPE3SZV7new · submitted 2026-06-24 · 🌌 astro-ph.GA

AGN Jets from Formation to Dissipation

A.-K. Baczko , Eleni Vardoulaki , Etienne Bonnassieux , Manel Perucho , Marisa Brienza , Marcus Br\"uggen , Emmanuel K. Bempong-Manful , Robert Beswick
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Florian Eppel Damien Gratadour Jonas He{\ss}d\"orfer Kiara Hervella-Seoane Matthias Kadler Jae-Young Kim Aretaios Lalakos Leah K. Morabito Dhanya G. Nair Felix P\"otzl Jack Radcliffe Luca Ricci Eduardo Ros Jan R\"oder Florian R\"osch Ainara Saiz-P\'erez Hrishikesh Shetgaonkar Cyril Tasse Francesco Ubertosi Jun Yang J. Anton Zensus
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Pith reviewed 2026-06-25 20:24 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords AGN jetsSquare Kilometre Arrayjet formationjet dissipationgalaxy evolutionAGN feedbackVLBIradio observations
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The pith

The Square Kilometre Array will enable tracing of AGN jets from their launch near black holes to dissipation on megaparsec scales.

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

The paper claims that decades of study have left the full sequence of AGN jet formation, propagation, and dissipation poorly understood because existing telescopes lack the sensitivity, resolution, and continuous scale coverage needed. It positions the Square Kilometre Array, operating alone or combined with VLBI arrays and multi-wavelength facilities, as the instrument that removes these barriers. A sympathetic reader would care because jets regulate star formation and redistribute energy across galaxies and their environments. The central open question is therefore the co-evolution of jets with their host galaxies. If the claim holds, observers will for the first time connect sub-parsec launch physics directly to megaparsec feedback effects.

Core claim

The central claim is that the future capabilities of the Square Kilometre Array, as a standalone array as well as in combination with VLBI arrays and multi-wavelength facilities, will transform our capabilities to study the co-evolution of AGN jets and their host galaxies from jet formation to dissipation scales.

What carries the argument

Multi-scale radio imaging with the SKA, linked to VLBI and other wavelengths, which supplies the sensitivity and resolution to bridge sub-parsec to megaparsec regimes in a single observational framework.

If this is right

  • Direct mapping of jet launching regions near supermassive black holes to their large-scale lobes.
  • Quantitative tracking of energy and momentum transfer from jets into the interstellar and intergalactic medium.
  • Improved constraints on how jets suppress or trigger star formation in host galaxies.
  • Observation of jet dissipation processes at the largest scales for statistical samples of AGN.
  • Tighter integration of radio jet feedback into models of galaxy assembly.

Where Pith is reading between the lines

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

  • Galaxy evolution simulations could be recalibrated once jet feedback is measured across the full scale range.
  • Multi-messenger campaigns pairing SKA with X-ray or gamma-ray telescopes may reveal the particle acceleration sites that current data miss.
  • If the scale-bridging works as expected, similar logic could be applied to other extended radio sources such as radio galaxies in clusters.
  • A null result from SKA would indicate that theoretical gaps, rather than observational ones, are now the dominant limit.

Load-bearing premise

That the main obstacles to understanding jet formation through dissipation are current limits in sensitivity, resolution, and multi-scale coverage that SKA will directly remove.

What would settle it

SKA data that fail to show new, previously inaccessible links between jet properties measured on formation scales and those measured on dissipation scales, or that leave models of jet-host galaxy interaction unchanged.

Figures

Figures reproduced from arXiv: 2606.25801 by Ainara Saiz-P\'erez, A.-K. Baczko, Aretaios Lalakos, Cyril Tasse, Damien Gratadour, Dhanya G. Nair, Eduardo Ros, Eleni Vardoulaki, Emmanuel K. Bempong-Manful, Etienne Bonnassieux, Felix P\"otzl, Florian Eppel, Florian R\"osch, Francesco Ubertosi, Hrishikesh Shetgaonkar, Jack Radcliffe, Jae-Young Kim, Jan R\"oder, J. Anton Zensus, Jonas He{\ss}d\"orfer, Jun Yang, Kiara Hervella-Seoane, Leah K. Morabito, Luca Ricci, Manel Perucho, Marcus Br\"uggen, Marisa Brienza, Matthias Kadler, Robert Beswick.

Figure 1
Figure 1. Figure 1: Sketch of all scales of AGN jets observable at radio wavelengths. a) jet propagation and interaction region; b) jet formation and launching region; c) black hole accretion and jet formation region d) jet dissipation and feedback region Radio astronomy has been instrumental in probing different aspects of AGN jet physics. Very Long Baseline Interferometry (VLBI) has enabled detailed studies of the innermost… view at source ↗
Figure 2
Figure 2. Figure 2: (𝑢𝑣)-plot of a global VLBI array consisting of EVN+eMERLIN+VLBA including the SKA (red) for a source at declination of +30 degree (left) and zoom-into the SKA-only coverage, +10 degree (middle), and −10 degree (right). The middle and right plots highlight LBA telescopes as well (blue). Other progress has been made, e.g. with the BRAND receiver, that is under commissioning at the Effelsberg telescopes, foll… view at source ↗
Figure 3
Figure 3. Figure 3: Examples of two radio AGN at 144 MHz and 3 GHz from the COSMOS field, showing large-scale diffuse emission at MHz frequencies that are missed with GHz observations (Vardoulaki et al., 2021a, and Vardoulaki in prep.) the intracluster medium (ICM), jets deposit energy that inflates cavities, drives shock fronts, and generate turbulence (e.g. Ubertosi et al., 2023; Prunier et al., 2025). With ∼30 mas resoluti… view at source ↗
Figure 4
Figure 4. Figure 4: 3D-RHD simulation of a 5×1044 erg/s relativistic jet propagating (from left to right) through an inhomogeneous galactic-to-cluster ambient medium, derived from cosmological simulations (Planelles et al., 2014). Jet mass fraction contours (yellow-red scale) track the propagation and mixing of injected material. Pressure contours (blue-green scale) for the environment gas included to show both the environmen… view at source ↗
Figure 5
Figure 5. Figure 5: Examples of two radio AGN from the COSMOS field (Vardoulaki et al., 2019, 2021a, and Vardoulaki in prep.) as targets for early science with SKA-Mid AA*, ranging frequencies from 144 MHz to 3 GHz, including 1.4 GHz VLBA observations (Herrera Ruiz et al., 2017) In order to allow for the study of jet expansion profiles from close to the formation region, covering the collimation, the break point to free expan… view at source ↗
Figure 6
Figure 6. Figure 6: Example of the low luminosity AGN M 84 observed with the VLA and VLBA at multiple frequencies between 1.4 and 43 GHz (Fariyanto et al., 2025) as target for early science with SKA-Mid AA*. which dominates AGN activity over cosmic time. SKA will be transformative for the study of AGN jets in the following ways: • Continuous mapping of the radio structure of jets and distinction from winds from parsec to kilo… view at source ↗
read the original abstract

Active Galactic Nuclei (AGN) are among the most energetic phenomena in the Universe, capable of launching powerful relativistic jets that extend from sub-parsec to megaparsec scales. These jets play a crucial role in regulating star formation, redistributing energy and matter, and shaping the evolution of galaxies and their environments. Despite decades of study, a comprehensive understanding of how AGN jets form, propagate, and dissipate remains elusive. The aim of this chapter is to highlight how the future capabilities of the the Square Kilometre Array (SKA), as a standalone array as well as in combination with Very Long Baseline Interferometry (VLBI) arrays and multi-wavelength facilities, will transform our capabilities to study the co-evolution of AGN jets and their host galaxies from jet formation to dissipation scales.

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. The manuscript is a perspective chapter arguing that the Square Kilometre Array (SKA), deployed standalone or in combination with VLBI arrays and multi-wavelength facilities, will transform observational capabilities for studying AGN jet formation, propagation, dissipation, and co-evolution with host galaxies across sub-parsec to megaparsec scales.

Significance. If the described sensitivity, resolution, and multi-scale coverage gains are realized, the perspective usefully frames how SKA can address open questions in jet physics and galaxy evolution; it provides a high-level roadmap rather than new data or derivations.

minor comments (1)
  1. [Abstract] Abstract contains a typographical error: 'the the Square Kilometre Array'.

Simulated Author's Rebuttal

0 responses · 0 unresolved

We thank the referee for their positive review and recommendation to accept the manuscript. No major comments were raised that require point-by-point responses.

Circularity Check

0 steps flagged

No circularity: qualitative perspective on future observational capabilities

full rationale

The paper is a review chapter whose central claim is that SKA (standalone and with VLBI/multi-wavelength facilities) will transform studies of AGN jet co-evolution from formation to dissipation scales. No equations, derivations, fitted parameters, predictions, or uniqueness theorems are present. The text frames observational gaps as motivation rather than a testable premise whose failure would invalidate the argument. No self-citation chain or ansatz is invoked to support any quantitative result. The derivation chain is empty by construction; the document contains no load-bearing steps that reduce to their own inputs.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

No mathematical derivations, free parameters, or new physical entities are introduced. The text relies on standard domain knowledge about AGN jets and SKA specifications already published elsewhere.

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Reference graph

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