REVIEW 1 major objections 1 minor 299 references
Exploring the physics of ram pressure stripping with radio continuum observations in the SKA era
T0 review · 1 major / 1 minor · reviewed 2026-06-25 · grok-4.3
Pith's one-line read The Square Kilometre Array will extend radio studies of ram pressure stripping to the southern sky and to redshift 0.5.
desk verdict A short perspective on SKA prospects for radio RPS studies that states expected capabilities but supplies no sensitivity calculations or scaling to support the z~0.5 claim. read the letter →
The pith
A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.
The reading
What carries the argument
Synchrotron emission produced by magnetic fields and relativistic electrons in the stripped interstellar medium, observed at low radio frequencies.
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.
Extended reading notes
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.
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.
Editorial extensions
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.
Reading between the lines
- 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.
Editorial analysis
A structured set of objections, weighed in public.
Referee Report
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)
- [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)
- 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
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
-
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
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.
Assumptions & free parameters
Cite this review
Pith. "Pith review of Exploring the physics of ram pressure stripping with radio continuum observations in the SKA era." pith.science (2026). https://pith.science/paper/K54E3HX2
@misc{pith2026260625746,
author = {Pith},
title = {Pith review of: Exploring the physics of ram pressure stripping with radio continuum observations in the SKA era},
year = {2026},
howpublished = {\url{https://pith.science/paper/K54E3HX2}},
note = {Machine review of arXiv:2606.25746}
}
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.
Figures
Reference graph
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