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arxiv: 2607.02342 · v1 · pith:VNKGG45Snew · submitted 2026-07-02 · 🌌 astro-ph.GA

The VLA-COSMOS 3 GHz Large Project: Polarised source counts and catalogue

S. Ranchod , S. A. Mao , R. P. Deane , V. Smol\v{c}i\'c , J. D. Wagenveld , M. Bondi , K. Mooley , E. Schinnerer This is my paper

Pith reviewed 2026-07-03 09:30 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords polarised sourcessource countsstar-forming galaxiesradio continuumrotation measure synthesis3 GHzVLA-COSMOSdepolarisation
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The pith

Deepest 3 GHz polarised survey detects 65 sources but no star-forming galaxies.

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

The paper processes the VLA-COSMOS 3 GHz polarisation data to produce the deepest polarised source counts at this frequency and resolution. After rotation measure synthesis on known total-intensity sources, 65 polarised sources are found above the 2.6 microJy per beam threshold, yielding 51 sources per square degree. No star-forming galaxies appear among them, which sets a 2-sigma upper limit of less than 2.0 per square degree on their polarised density. The counts match those reported at 1.4 GHz, which the authors trace to the combined action of spectral index and depolarisation. The result indicates that detecting polarised emission from star-forming galaxies will require substantially deeper observations than those used here.

Core claim

With a sensitivity of 2.6 μJy/beam in Faraday depth, we detect 65 polarised sources (51 deg^{-2}) above our threshold. We find that our cumulative and Euclidean-normalised source counts at 3 GHz are consistent with those in the literature at 1.4 GHz, which we attribute to the combined effect of spectral index and depolarisation in the detected sources. We detect no SFGs in our sample and derive a 2σ upper limit on the density of polarised SFGs of <2.0 deg^{-2}. This implies that significantly deeper observations will be required to readily detect this population in the SKA-era.

What carries the argument

3D rotation measure synthesis on Stokes Q and U maps of pre-selected total-intensity sources, combined with an empirically determined polarisation detection threshold.

If this is right

  • Polarised source counts at 3 GHz remain consistent with 1.4 GHz results after accounting for spectral index and depolarisation.
  • No star-forming galaxies are detected in polarisation at the achieved sensitivity.
  • The 2-sigma upper limit on the surface density of polarised star-forming galaxies is less than 2.0 per square degree.
  • Significantly deeper observations will be required to detect the polarised star-forming galaxy population in the SKA era.

Where Pith is reading between the lines

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

  • The non-detection at 3 GHz indicates that depolarisation effects in star-forming galaxies remain strong enough to suppress detectable polarisation even at this frequency.
  • Current polarised samples are dominated by AGN rather than star-forming galaxies, setting a benchmark sensitivity target for future instruments.
  • Higher-frequency data alone may still be insufficient without corresponding gains in depth to reveal the magnetic-field properties of typical galaxies.

Load-bearing premise

The empirically determined polarisation detection threshold reliably separates real signals from noise, and selecting known total-intensity sources captures essentially all potential polarised emitters without substantial incompleteness at faint levels.

What would settle it

Finding even one polarised star-forming galaxy in the present dataset, or measuring a polarised SFG density above 2 per square degree in a survey of comparable depth and resolution, would falsify the reported upper limit.

Figures

Figures reproduced from arXiv: 2607.02342 by E. Schinnerer, J. D. Wagenveld, K. Mooley, M. Bondi, R. P. Deane, S. A. Mao, S. Ranchod, V. Smol\v{c}i\'c.

Figure 1
Figure 1. Figure 1: Mean rms noise per frequency channel for Stokes I [PITH_FULL_IMAGE:figures/full_fig_p003_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: rms noise maps for the central frequency ( [PITH_FULL_IMAGE:figures/full_fig_p004_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Typical RMSF obtained through RM synthesis for the [PITH_FULL_IMAGE:figures/full_fig_p005_3.png] view at source ↗
Figure 5
Figure 5. Figure 5: Example of extracted spectra and images for source ID [PITH_FULL_IMAGE:figures/full_fig_p006_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Cumulative source counts based on the peak polarised in [PITH_FULL_IMAGE:figures/full_fig_p007_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Euclidean-normalised differential source counts for the polarised source population in the VLA-COSMOS 3 GHz survey. The completeness-corrected counts are plotted as filled circles at 3 GHz (blue) and extrapolated to 1.4 GHz (orange). We plot the source counts from the following recent deep surveys (grey): Lockman Hole field (Berger et al. 2021, open squares), MeerKAT Fornax Survey (Loi et al. 2025, filled … view at source ↗
Figure 8
Figure 8. Figure 8: Spectral index (α) against depolarisation index (β) for the Ppeak of all sources. Histograms of the α and β distributions are shown at the top and on the right, respectively. The solid black lines indicate their median values, as provided in the legend. resolved in total intensity, we can visually identify from which part of the source the peak spectrum is extracted. In the case of the flat-spectrum source… view at source ↗
Figure 9
Figure 9. Figure 9: Peak total intensity plotted against the number of pixels, [PITH_FULL_IMAGE:figures/full_fig_p010_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: Modelled cumulative source counts, as in Fig. 6. The [PITH_FULL_IMAGE:figures/full_fig_p011_10.png] view at source ↗
read the original abstract

The exploration of the faint polarised radio source population is essential for interpreting the nature and evolution of magnetic fields in galaxies. While recent studies have provided insight into source counts for the $\mu$Jy polarised source population at 1.4 GHz, higher frequency surveys may be more sensitive to new populations that are depolarised at lower frequencies (i.e. due to internal or external depolarisation effects). We present the deepest polarised source counts at 3 GHz to date, at an angular resolution of $1.5''$. With these relatively higher frequency observations, we aim to probe the faint polarised star-forming galaxy (SFG) population. Furthermore, through spectral modelling, we aim to provide further insight into the frequency evolution of polarised source counts. We processed the polarisation data of the VLA-COSMOS 3 GHz Large Project, one of the deepest high-resolution radio continuum surveys. We produced Stokes Q and U mosaicked channel maps. After selecting known sources in total intensity, we performed 3D rotation measure synthesis and searched for polarised emission using an empirically determined threshold. With a sensitivity of 2.6 $\mu$Jy/beam in Faraday depth, we detect 65 polarised sources (51 deg$^{-2}$) above our threshold. We find that our cumulative and Euclidean-normalised source counts at 3 GHz are consistent with those in the literature at 1.4 GHz, which we attribute to the combined effect of spectral index and depolarisation in the detected sources. We detect no SFGs in our sample and derive a 2$\sigma$ upper limit on the density of polarised SFGs of $<2.0~\mathrm{deg}^{-2}$. This implies that significantly deeper observations will be required to readily detect this population in the SKA-era.

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

2 major / 2 minor

Summary. The manuscript presents a polarisation analysis of the VLA-COSMOS 3 GHz Large Project, producing Stokes Q/U mosaics, applying 3D RM synthesis to total-intensity pre-selected sources, and detecting 65 polarised sources (51 deg^{-2}) above an empirically determined 2.6 μJy/beam threshold in Faraday depth. Source counts at 3 GHz are reported as consistent with 1.4 GHz literature after spectral-index and depolarisation effects; no polarised SFGs are found, yielding a 2σ upper limit of <2.0 deg^{-2} on their surface density, with the implication that deeper SKA-era observations will be required.

Significance. If the non-detection and upper limit are robust, the result quantifies the rarity of detectable polarised emission from SFGs at current 3 GHz sensitivities and supplies a concrete benchmark for SKA survey planning. The reported source counts add a higher-frequency anchor point to the polarised population, though their consistency with lower-frequency work is attributed to a combination of spectral index and depolarisation whose separate contributions are not separated in the analysis.

major comments (2)
  1. [Abstract, §3] Abstract and §3 (data processing / source selection): the polarisation detection threshold is stated as 'empirically determined' at 2.6 μJy/beam, yet no quantitative validation (false-positive rate, Monte Carlo noise realisations, or completeness curves) is supplied. Because the 65 detections and the SFG upper limit rest directly on this threshold, the absence of these diagnostics leaves the reliability of both the count and the <2.0 deg^{-2} limit unverifiable from the text.
  2. [Abstract, §4] Abstract and §4 (SFG non-detection): the upper limit assumes that every polarised SFG above the threshold would have been captured by the total-intensity pre-selection catalogue. No completeness assessment at the faint end, discussion of possible missed low-surface-brightness SFGs, or test of the pre-selection efficiency is provided; this assumption is load-bearing for the claimed density limit and the SKA-era implication.
minor comments (2)
  1. [Abstract] The abstract states the sensitivity as 2.6 μJy/beam 'in Faraday depth' without clarifying whether this is the rms in the Faraday spectrum or a peak threshold; a brief parenthetical definition would remove ambiguity.
  2. [§3] Figure captions and text should explicitly state the exact total-intensity catalogue used for pre-selection (e.g., reference to the VLA-COSMOS 3 GHz catalogue paper) so that readers can assess selection biases.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the constructive comments, which highlight important aspects of our analysis that require clarification and additional support. We respond to each major comment below and indicate where revisions will be made.

read point-by-point responses

  1. Referee: [Abstract, §3] Abstract and §3 (data processing / source selection): the polarisation detection threshold is stated as 'empirically determined' at 2.6 μJy/beam, yet no quantitative validation (false-positive rate, Monte Carlo noise realisations, or completeness curves) is supplied. Because the 65 detections and the SFG upper limit rest directly on this threshold, the absence of these diagnostics leaves the reliability of both the count and the <2.0 deg^{-2} limit unverifiable from the text.

    Authors: We agree that the manuscript would benefit from explicit quantitative validation of the 2.6 μJy/beam threshold. Although the threshold was derived from the noise properties of the Faraday dispersion function and cross-checked against the distribution of negative peaks, we did not include Monte Carlo realisations or completeness curves in the submitted version. In the revised manuscript we will add these diagnostics, including the false-positive rate estimated from noise-only realisations and a completeness curve versus polarised intensity, so that the reliability of the 65 detections and the upper limit can be directly assessed. revision: yes

  2. Referee: [Abstract, §4] Abstract and §4 (SFG non-detection): the upper limit assumes that every polarised SFG above the threshold would have been captured by the total-intensity pre-selection catalogue. No completeness assessment at the faint end, discussion of possible missed low-surface-brightness SFGs, or test of the pre-selection efficiency is provided; this assumption is load-bearing for the claimed density limit and the SKA-era implication.

    Authors: The referee correctly notes that the <2.0 deg^{-2} upper limit rests on the assumption that the total-intensity catalogue is complete for any polarised SFGs above our Faraday-space threshold. The VLA-COSMOS 3 GHz total-intensity catalogue is >95 % complete for point sources at the relevant flux densities, but we did not explicitly quantify completeness for low-surface-brightness or extended SFGs in polarisation. In the revision we will add a dedicated paragraph discussing the pre-selection efficiency, citing the total-intensity completeness limits from the parent survey paper, and stating that the upper limit applies strictly to the population that would be detected in total intensity; we will also note the possible impact of any missed diffuse sources as a caveat. revision: yes

Circularity Check

0 steps flagged

No circularity: direct observational extraction of counts and upper limit from maps

full rationale

The paper processes Stokes Q/U maps, applies 3D RM synthesis to pre-selected total-intensity sources, and counts detections above an empirically set Faraday-depth threshold of 2.6 μJy/beam. The reported 65 sources, zero SFGs, and <2.0 deg^{-2} upper limit are obtained by direct application of this threshold to the data; no equation, fit, or self-citation is invoked that would make the count or limit equivalent to its own inputs by construction. The derivation chain remains data-to-result without tautological reduction.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

Observational radio-astronomy study; relies on standard techniques and survey data rather than new theoretical constructs.

free parameters (1)
  • polarised emission detection threshold = empirically determined
    Empirically determined value used to select the 65 sources above the 2.6 μJy/beam Faraday-depth sensitivity.
axioms (1)
  • standard math Rotation measure synthesis correctly recovers Faraday depth under the assumption of a single thin-screen or simple Faraday structure
    Invoked when performing 3D RM synthesis on the Stokes Q and U channel maps.

pith-pipeline@v0.9.1-grok · 5909 in / 1337 out tokens · 43241 ms · 2026-07-03T09:30:49.762586+00:00 · methodology

discussion (0)

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Reference graph

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