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arxiv: 2606.25746 · v1 · pith:K54E3HX2new · submitted 2026-06-24 · 🌌 astro-ph.GA

Exploring the physics of ram pressure stripping with radio continuum observations in the SKA era

Alessandro Ignesti , Ian D. Roberts , Henrik W. Edler , Myriam Gitti , Reinout J. van Weeren , Paolo Serra , Pavel Jachym This is my paper

Pith reviewed 2026-06-25 20:20 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords ram pressure strippingradio continuumSKAgalaxy clusterssynchrotron emissionenvironmental quenchingintracluster mediumsatellite galaxies
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The pith

The Square Kilometre Array will extend radio studies of ram pressure stripping to the southern sky and to redshift 0.5.

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

Satellite galaxies in clusters experience ram pressure stripping when the intracluster medium removes their interstellar gas. This stripped material produces synchrotron radio emission that is steep-spectrum and therefore easiest to observe at low frequencies. Current work relies on LOFAR and is confined to the northern sky. SKA-Low will open the southern sky and allow coordination with other southern facilities including the ELT. SKA-Mid will add sub-arcsecond resolution to map polarization and filaments in the tails and to detect them at greater distances.

Core claim

Continuum studies of the RPS effect are currently mostly carried out with LOFAR, limiting them to the northern hemisphere. SKA-Low will permit us to extend them to the southern sky, where they will synergize with the southern observatories and the upcoming ELT. The sub-arcsecond resolution provided by SKA-Mid will facilitate the exploration of the polarization and filamentary structure of RPS radio tails and allow us to detect them up to z≃0.5, advancing our understanding of the impact of RPS on satellite galaxies in clusters and groups.

What carries the argument

Synchrotron emission produced by magnetic fields and relativistic electrons in the stripped interstellar medium, observed at low radio frequencies.

If this is right

  • RPS radio studies will cover the southern sky with SKA-Low.
  • Multi-wavelength synergy will increase between radio data and southern optical and X-ray facilities including the ELT.
  • Polarization and filamentary structure of RPS tails will become accessible with SKA-Mid.
  • RPS tails will be detectable up to redshift approximately 0.5.
  • Statistical understanding of RPS effects on satellite galaxies in clusters and groups will improve.

Where Pith is reading between the lines

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

  • Polarization measurements could constrain the magnetic field geometry within the stripped tails.
  • Southern-sky coverage may allow direct comparison of RPS efficiency across clusters with different dynamical histories.
  • Detections at higher redshift could indicate whether RPS efficiency changes with look-back time.

Load-bearing premise

The synchrotron emission from stripped ISM is sufficiently bright, steep-spectrum, and morphologically distinct to be reliably detected and interpreted with SKA at the stated redshifts and resolutions.

What would settle it

Non-detection of the predicted steep-spectrum radio tails in southern clusters with SKA-Low or absence of resolved tails at z approximately 0.5 with SKA-Mid would falsify the expected performance.

Figures

Figures reproduced from arXiv: 2606.25746 by Alessandro Ignesti, Henrik W. Edler, Ian D. Roberts, Myriam Gitti, Paolo Serra, Pavel Jachym, Reinout J. van Weeren.

Figure 1
Figure 1. Figure 1: Composite optical-radio image of the RPS galaxy JW39 from Ignesti et al. (2022a). Here are reported the stellar continuum (greyscale), stellar disk (silver contour), H𝛼 emission (yellow-to-red contours) and radio continuum emission at 144 MHz (blue-filled contours). They can be divided into two main categories, those driven by gravitational forces between galaxies, such as mergers and tidal interaction (Ba… view at source ↗
Figure 2
Figure 2. Figure 2: Composite optical (CFHT, RGB) and radio (LOFAR, 144 MHz) images of eight LoTSS jellyfish galaxies from Roberts et al. (2021a,b) at 𝑧 < 0.04. The galaxy celestial coordinates are reported in the top-left corner, and the white scalebar corresponds to a size of 20 kpc at the hosting cluster redshift. Condon, 1992, for a review). Given the connection between star-formation and CRe and the fact that galaxies ar… view at source ↗
Figure 3
Figure 3. Figure 3: Top: Reference evolution of radio tail scale length (green) and polarization fraction (silver, darker shades correspond to increasing ICM rotation measure levels of -10, -15, -30, -45, and -60 rad m−2 ) with the observed frequency. The horizontal bars indicate the frequency band observed by LOFAR HBA (purple), SKA-Low (blue), SKA-Mid band 1 (red) and band 2 (orange). Bottom: Recovered RPS radio tail observ… view at source ↗
read the original abstract

Satellite galaxies in clusters are significantly more likely to be red and passive than similar mass galaxies in the field. This fact is known as the environmental quenching of galaxy star formation, which is believed to be driven by ram pressure stripping (RPS). The large velocity differences between the infalling galaxies and the intracluster medium (ICM) result in a strong ram pressure on their interstellar medium (ISM), which can strip it from the stellar disk. The stripped ISM can be studied at various wavelengths, including the radio band, thanks to the synchrotron emission produced by the magnetic fields and relativistic electrons embedded in them. This emission is typically steep-spectrum and thus best observed at low frequencies. Thus, continuum studies of the RPS effect are currently mostly carried out with LOFAR, limiting them to the northern hemisphere. SKA-Low will permit us to extend them to the southern sky, where they will synergize with the southern observatories and the upcoming ELT. Lastly, the sub-arcsecond resolution provided by SKA-Mid will facilitate the exploration of the polarization and filamentary structure of RPS radio tails and allow us to detect them up to $z\simeq0.5$, advancing our understanding of the impact of RPS on satellite galaxies in clusters and groups.

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

1 major / 1 minor

Summary. The manuscript argues that radio continuum observations of ram pressure stripping (RPS) tails via steep-spectrum synchrotron emission are currently limited to LOFAR in the northern sky. It claims that SKA-Low will extend such studies to the southern hemisphere for synergy with southern facilities and the ELT, while SKA-Mid's sub-arcsecond resolution will enable polarization and filamentary mapping of RPS tails and allow detections up to z≃0.5, thereby advancing understanding of environmental quenching in clusters and groups.

Significance. If the detectability assumptions hold, the perspective correctly identifies an important observational niche for SKA in multi-wavelength RPS studies and highlights synergies with upcoming southern facilities. However, the absence of any quantitative predictions or sensitivity analysis limits its immediate impact as a research contribution.

major comments (1)
  1. [Abstract] Abstract: The central claim that SKA-Mid sub-arcsecond resolution 'will ... allow us to detect them up to z≃0.5' is unsupported by any sensitivity scaling, flux-density extrapolation from published LOFAR RPS detections, or comparison against SKA-Mid noise curves after cosmological surface-brightness dimming ((1+z)^-4), steep-spectrum k-correction, and beam dilution at fixed physical scales. This quantitative gap is load-bearing for the paper's primary forward-looking assertion.
minor comments (1)
  1. The text is entirely prospective and would benefit from an explicit statement of the assumptions required for the z≃0.5 detection claim (e.g., minimum surface brightness, spectral index range, and morphological distinctness against ICM turbulence).

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their thoughtful review and for highlighting the need for quantitative support behind the forward-looking claims in our perspective article. We address the single major comment below and will revise the manuscript accordingly.

read point-by-point responses

  1. Referee: [Abstract] Abstract: The central claim that SKA-Mid sub-arcsecond resolution 'will ... allow us to detect them up to z≃0.5' is unsupported by any sensitivity scaling, flux-density extrapolation from published LOFAR RPS detections, or comparison against SKA-Mid noise curves after cosmological surface-brightness dimming ((1+z)^-4), steep-spectrum k-correction, and beam dilution at fixed physical scales. This quantitative gap is load-bearing for the paper's primary forward-looking assertion.

    Authors: We agree that the claim regarding detections up to z≃0.5 requires quantitative backing to be robust. In the revised manuscript we will add a dedicated subsection (likely in Section 3 or a new Section 4) that performs order-of-magnitude sensitivity calculations. These will extrapolate flux densities from published LOFAR RPS tail detections, apply the (1+z)^-4 surface-brightness dimming, include a steep-spectrum k-correction, account for beam dilution at fixed physical scales, and compare the resulting surface brightnesses against the expected SKA-Mid noise curves at the relevant frequencies and resolutions. This addition will directly support (or qualify) the z≃0.5 statement while preserving the perspective nature of the paper. revision: yes

Circularity Check

0 steps flagged

No circularity; paper contains no derivations, fits, or self-referential claims

full rationale

The manuscript is a forward-looking perspective on SKA capabilities for RPS studies. It states observational expectations (e.g., detection to z≃0.5) without any equations, parameter fitting, or reduction of claims to prior self-citations. No load-bearing steps reduce by construction to inputs. The absence of quantitative sensitivity calculations is a separate issue of evidence strength, not circularity.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

This is a perspective paper on observational prospects with no physical model, derivation, or new data presented, so the ledger is empty.

pith-pipeline@v0.9.1-grok · 5784 in / 961 out tokens · 17463 ms · 2026-06-25T20:20:37.390337+00:00 · methodology

discussion (0)

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Reference graph

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