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arxiv: 2606.25081 · v1 · pith:6MZVJH72new · submitted 2026-06-23 · 🌌 astro-ph.CO

Cosmology from Clustering of Continuum Galaxies

Jacobo Asorey , Catherine L. Hale , Sebastian von Hausegger , David Parkinson , Chandra Shekhar Saraf , Jonah D. Wagenveld , Benedict Bahr-Kalus , Syed Faisal ur Rahman
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Ziad Sakr
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Pith reviewed 2026-06-25 22:51 UTC · model grok-4.3

classification 🌌 astro-ph.CO
keywords radio continuum galaxiesangular clusteringSKAO surveycosmologyredshift distributiongalaxy biasmagnification biastelescope systematics
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The pith

A 20,000 square degree SKAO survey reaches microJansky sensitivity and can detect 300-400 million radio continuum galaxies whose angular clustering probes cosmology.

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

Radio continuum galaxies trace the large-scale matter distribution and can inform initial conditions, dark matter, and dark energy. Their use requires models for redshift distribution, galaxy bias, and magnification bias because sources lack easy radial positions and cross-identifications are difficult. The paper examines a specific SKAO survey covering 20,000 square degrees with 10,000 hours of integration in AA4 configuration. This setup reaches O(μJy/beam) depth and yields the largest radio continuum sample to date, exceeding prior SKA Red Book assumptions. Mocks that incorporate telescope systematics are used to forecast the angular clustering signal and to identify needed data corrections.

Core claim

The distribution of radio continuum galaxies is a useful probe of the matter distribution. For the described 20,000 sq. deg. SKAO survey in AA4 configuration with 10,000 hours, O(μJy/beam) sensitivities are reached and O(300-400 million) radio sources are detected. This sample size surpasses the number assumed for the previous SKA cosmology Red Book. Angular clustering is predicted from mocks that include potential telescope systematics, and the paper discusses data corrections required when those systematics cannot be fully modeled.

What carries the argument

Mocks that incorporate potential telescope systematics to forecast the angular clustering of the radio continuum sources.

If this is right

  • The survey yields the largest sample of radio continuum galaxies assembled to date.
  • The sample exceeds the source numbers used in the prior SKA cosmology Red Book.
  • Angular clustering predictions from the mocks indicate which telescope systematics must be corrected to extract cosmology.
  • Reliable cosmological inferences from the clustering require accurate inputs for redshift distribution, galaxy bias, and magnification bias.

Where Pith is reading between the lines

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

  • If the required population models prove accurate, cross-correlations between this radio sample and optical or infrared catalogs could supply the missing radial information.
  • The same mock-based forecasting approach could be repeated for deeper or wider configurations of other radio arrays to test scalability.
  • Deviations between observed and predicted clustering after corrections would point to unmodeled evolution in the radio galaxy population itself.

Load-bearing premise

Accurate measurements or models of the redshift distribution of radio sources, the galaxy bias, and the flux distribution are available so that reliable cosmological inferences can be made from the clustering signal.

What would settle it

A measured source count well below 300 million or an angular clustering amplitude that deviates from the mock predictions after all modeled corrections would show the survey does not deliver the forecasted cosmological information.

Figures

Figures reproduced from arXiv: 2606.25081 by Benedict Bahr-Kalus, Catherine L. Hale, Chandra Shekhar Saraf, David Parkinson, Jacobo Asorey, Jonah D. Wagenveld, Sebastian von Hausegger, Syed Faisal Ur Rahman, Ziad Sakr.

Figure 1
Figure 1. Figure 1: Left: Comparisons of this simulated survey (blue) compared to continuum surveys from SKA precursors of the effective 1.4 GHz rms (assuming 𝑆𝜈 ∝ 𝜈 −0.7 ) and area covered. Points are coloured by their frequency and the marker size indicates the resolution. Right: Expected source numbers with flux density limit in this survey (grey, using simulations outlined in Section 5) to previous/current surveys (dashed… view at source ↗
Figure 2
Figure 2. Figure 2: Estimated rms distribution of a planned 20 000 sq deg, 10 000 h AA4 survey (incl. galaxy). Firstly, we generate a selection of potentially detectable input sources across the potential field of view for such a survey with the SKAO. We sample source positions across the field of view from cosmological matter density fields simulated with GLASS (Tessore et al., 2023), a simulation framework that efficiently … view at source ↗
Figure 3
Figure 3. Figure 3: Comparison of the over-density (𝛿) as in Equation 1 for a 20 000 deg2 survey which includes (left) or excludes (right) the Galactic plane with increasing flux density for no flux cut (top), 20𝜇Jy cut (middle) and 40 𝜇Jy (bottom). Included in the title of each plot is the number of sources expected in the survey. Hale et al., 2025) - thus overcoming the effects of confusion which affects deep surveys such a… view at source ↗
Figure 4
Figure 4. Figure 4: Redshift distribution (𝑁(𝑧)) of the expected radio sources (grey) and split into SFGs (blue) and AGN (red). 6.2 𝐶ℓ predictions for the SKAO In this section we present predictions for the large￾scale structure measurements from the proposed sur￾vey with SKAO AA4 configuration. For that, we have measured the angular power spectra for the dif￾ferent simulated maps described in Section 5. As outlined above, th… view at source ↗
Figure 5
Figure 5. Figure 5: Comparison of the 𝐶ℓ for a variety of flux density (𝑆) and galactic latitude (𝑏) cuts. Solid lines indicate 𝐶ℓ measured from the output catalogue (solid lines) and the dotted lines indicate the 𝐶ℓ measured using weights which account for incompleteness. Shown are: top left: comparison when no galactic cut is applied; top right: when a ±10◦ galactic cut is applied; and bottom: results for flux densities abo… view at source ↗
Figure 6
Figure 6. Figure 6: Relative error on the estimated angular power spectrum for the proposed SKAO AA4 continuum survey and an EMU-like survey. The grey area represents the non-linear scales. Whilst the 1-halo clustering of galaxies (see e.g. Zheng et al., 2005) has been explored thoroughly in the optical and IR (see e.g. Zehavi et al., 2011; Hatfield et al., 2016), this is relatively unexplored in the case of radio continuum s… view at source ↗
read the original abstract

The distribution of radio continuum galaxies is a useful, fast, and accessible probe of the matter distribution in the Universe, enlightening us about the Universe's initial conditions, the physics of dark matter, and the nature of the mysterious dark energy. However, radio continuum galaxies alone cannot easily be localised in the radial direction, and cross-identification of host sources from optical catalogues is challenging across wide area surveys. Moreover, there are several redshift-dependent properties of radio galaxy populations that all need accurate modelling to make reliable inferences about fundamental physics. These include accurate measurements of the redshift distribution of radio sources ($dN/dz$), the coupling between radio galaxies and the underlying matter distribution (quantified by the galaxy bias, $b(z)$), and the true flux distribution $N(S,z)$ of the radio sources (magnification bias). The amount of encoded cosmological information depends on the survey properties and the level of homogeneity across its footprint. In this chapter, we demonstrate the cosmological potential of a 20,000 sq. deg survey with the SKAO in AA4 configuration, using 10,000 hours of observations. Such a survey will reach $\mathcal{O}(\mu\mathrm{Jy/beam)}$ sensitivities and detect $\mathcal{O}$(300-400 million) radio sources, the largest sample of radio continuum galaxies to date. This surpasses the number of sources assumed for the previous SKA cosmology Red Book. We predict the angular clustering of such a survey, using mocks accounting for potential telescope systematics, and discuss which data corrections may be needed when these systematics cannot be accurately modelled.}

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 / 1 minor

Summary. The manuscript forecasts the cosmological potential of angular clustering from radio continuum galaxies in a 20,000 sq. deg. SKAO AA4 survey using 10,000 hours of integration. It claims this survey reaches O(μJy/beam) sensitivity and detects O(300-400 million) sources—exceeding prior SKA Red Book assumptions—and predicts the angular clustering signal via mocks that incorporate telescope systematics while discussing required data corrections. The work emphasizes that reliable cosmological inferences require accurate models of dN/dz, galaxy bias b(z), and magnification bias N(S,z).

Significance. If the input population models prove robust and the mocks accurately capture both systematics and clustering, the result would update expectations for the largest radio-continuum sample available for cosmology, potentially strengthening forecasts for constraints on dark energy and initial conditions beyond previous SKA planning documents. The explicit identification of the three key population parameters as prerequisites for inference is a useful clarification.

major comments (2)
  1. [Abstract] Abstract: the central demonstration consists of predicting angular clustering from mocks that must incorporate dN/dz, b(z) and N(S,z) as inputs, yet no validation, robustness tests against current observational uncertainties, or variation of these inputs is described; because both the quoted source count (300-400 million) and the clustering amplitude derive directly from the same N(S,z) and bias assumptions, any systematic error in those inputs propagates to the claimed cosmological potential and the comparison with the SKA Red Book.
  2. [Abstract] Abstract: the statement that the survey 'surpasses the number of sources assumed for the previous SKA cosmology Red Book' is presented without a quantitative side-by-side comparison of either the predicted clustering amplitude or the resulting cosmological forecast precision, leaving the improvement in cosmological utility unsubstantiated.
minor comments (1)
  1. The manuscript is described as 'this chapter'; the relation to any larger volume or book should be clarified for readers.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their careful reading and constructive feedback. The comments correctly identify that our forecasts rely on input population models and that the abstract claim of improvement over the SKA Red Book would benefit from more explicit support. We respond to each point below.

read point-by-point responses

  1. Referee: [Abstract] Abstract: the central demonstration consists of predicting angular clustering from mocks that must incorporate dN/dz, b(z) and N(S,z) as inputs, yet no validation, robustness tests against current observational uncertainties, or variation of these inputs is described; because both the quoted source count (300-400 million) and the clustering amplitude derive directly from the same N(S,z) and bias assumptions, any systematic error in those inputs propagates to the claimed cosmological potential and the comparison with the SKA Red Book.

    Authors: We agree that the forecasts are tied to the chosen fiducial models for dN/dz, b(z) and N(S,z). The manuscript adopts standard literature values for these quantities to generate the mocks and explicitly states in the introduction that accurate modeling of all three is required for reliable cosmological inference. No robustness tests or parameter variations are performed in the current work, as the emphasis is on survey geometry, depth, and telescope systematics rather than population-model uncertainty. We will revise the abstract and discussion to qualify the results as forecasts under current best-estimate inputs, noting that systematic errors in these inputs would propagate to the quoted source counts and clustering amplitude. This clarification will be added without changing the core analysis. revision: partial

  2. Referee: [Abstract] Abstract: the statement that the survey 'surpasses the number of sources assumed for the previous SKA cosmology Red Book' is presented without a quantitative side-by-side comparison of either the predicted clustering amplitude or the resulting cosmological forecast precision, leaving the improvement in cosmological utility unsubstantiated.

    Authors: We accept that the claim would be stronger with a direct comparison. The Red Book used earlier sensitivity assumptions that yielded fewer sources than the updated AA4 configuration and 10,000-hour integration considered here. We will insert a brief quantitative comparison (source numbers and, where straightforward, a note on clustering amplitude scaling) in the revised abstract or main text. A full side-by-side cosmological-parameter forecast is outside the present scope but can be flagged as desirable future work. revision: yes

Circularity Check

0 steps flagged

No significant circularity; forward modeling from standard inputs

full rationale

The paper forecasts source counts and angular clustering for a future SKAO survey by constructing mocks that incorporate external models for dN/dz, b(z) and N(S,z). This is standard forward modeling rather than fitting any parameter to the clustering signal being predicted and then re-presenting the fit as a prediction. No equations or steps in the abstract reduce the output to the inputs by construction, no self-citation chain is load-bearing, and no uniqueness theorem is invoked. The derivation remains independent of the target result and is therefore self-contained.

Axiom & Free-Parameter Ledger

3 free parameters · 1 axioms · 0 invented entities

Only abstract available; ledger reflects the modeling requirements explicitly named as necessary for the central claim.

free parameters (3)
  • redshift distribution dN/dz
    Stated as required for reliable inferences but no specific functional form or fitting procedure given.
  • galaxy bias b(z)
    Stated as required for reliable inferences but no specific functional form or fitting procedure given.
  • magnification bias N(S,z)
    Stated as required for reliable inferences but no specific functional form or fitting procedure given.
axioms (1)
  • domain assumption Radio continuum galaxies trace the underlying matter distribution sufficiently well for clustering to encode cosmological information.
    Abstract opens by calling the distribution 'a useful, fast, and accessible probe of the matter distribution'.

pith-pipeline@v0.9.1-grok · 5845 in / 1433 out tokens · 27740 ms · 2026-06-25T22:51:11.701920+00:00 · methodology

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Reference graph

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