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arxiv: 2605.13543 · v1 · submitted 2026-05-13 · 🌌 astro-ph.CO

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UNIONS-3500 Weak Lensing: IV. 2D cosmological constraints in harmonic space

S. Guerrini , L. W. K. Goh , F. Hervas-Peters , C. Daley , M. Kilbinger , A. Wittje , C. Murray , S. Fabbro
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H. Hildebrandt M. J. Hudson L. van Waerbeke A. H. Wright T. de Boer J.-C. Cuillandre E. Magnier A. W. McConnachie
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Pith reviewed 2026-05-14 18:21 UTC · model grok-4.3

classification 🌌 astro-ph.CO
keywords cosmic shearweak lensingUNIONSharmonic spaceS8cosmological constraintsintrinsic alignmentsbaryonic feedback
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The pith

UNIONS survey cosmic shear in harmonic space constrains S8 to 0.891 consistent with Planck at 0.79 sigma

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

This paper applies a harmonic-space pseudo-C_ℓ estimator to non-tomographic cosmic shear data from the UNIONS r-band photometric survey to constrain cosmological parameters in flat LambdaCDM. It models baryonic feedback and intrinsic galaxy alignments while confirming that point spread function systematics have negligible impact and that results hold across varied scale cuts. The analysis returns S8 ≡ σ8 √(Ωm/0.3) = 0.891+0.057−0.084, which matches Planck CMB constraints at 0.79 sigma and other weak lensing surveys between 0.87 and 1.51 sigma. Lognormal simulations show 2.18 sigma agreement between the harmonic-space and configuration-space statistics. The work provides the first cosmological shear result from UNIONS and supplies a baseline for future tomographic and 3x2-point analyses that exploit the survey's northern overlap with spectroscopic samples.

Core claim

In a non-tomographic analysis of UNIONS r-band shape measurements, the pseudo-C_ℓ cosmic shear estimator yields S_8 ≡ σ_8 √(Ω_m / 0.3) = 0.891^{+0.057}_{-0.084} under standard ΛCDM cosmology after modeling baryonic feedback and intrinsic alignments, remaining consistent with Planck at the 0.79σ level.

What carries the argument

The pseudo-C_ℓ estimator for the cosmic shear power spectrum in harmonic space, which extracts the signal while incorporating the survey mask and geometry.

If this is right

  • The S8 constraint is robust to changes in scale cuts and modeling choices for baryonic feedback and intrinsic alignments.
  • Configuration-space and harmonic-space statistics agree at 2.18 sigma when tested with lognormal simulations.
  • The main uncertainty source is the degeneracy between S8 and the intrinsic alignment amplitude A_IA.
  • The non-tomographic result establishes a foundation for planned tomographic and 3x2-point cross-correlation analyses using UNIONS spectroscopic overlaps.

Where Pith is reading between the lines

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

  • Tomographic binning of the same dataset could separate redshift information and tighten the S8 error bars by reducing present degeneracies.
  • The Planck-level agreement suggests that any S8 tension reported by other lensing surveys may trace to survey-specific systematics or modeling differences rather than new physics.
  • Repeating the analysis with alternative independent priors on A_IA measured directly in the UNIONS footprint would test and potentially narrow the current uncertainty.
  • The harmonic-space pipeline can be combined with other northern-hemisphere imaging to cross-check structure-growth measurements across hemispheres.

Load-bearing premise

The prior on the intrinsic alignment amplitude A_IA drawn from direct measurements, together with the baryonic feedback modeling and chosen scale cuts, does not introduce significant bias into the S8 posterior.

What would settle it

An independent measurement of A_IA in the UNIONS fields lying well outside the adopted prior range, which would shift the S8 posterior, or an external S8 determination inconsistent with 0.891 at more than 3 sigma.

Figures

Figures reproduced from arXiv: 2605.13543 by A. H. Wright, A. Wittje, A. W. McConnachie, C. Daley, C. Murray, E. Magnier, F. Hervas-Peters, H. Hildebrandt, J.-C. Cuillandre, L. van Waerbeke, L. W. K. Goh, M. J. Hudson, M. Kilbinger, S. Fabbro, S. Guerrini, T. de Boer.

Figure 1
Figure 1. Figure 1: shows the final calibrated distribution n(z). 3. Methods This work aims to extract cosmological constraints from the measurements of the angular power spectrum of the non￾tomographic cosmic shear field inferred from the UNIONS data. This section describes the estimation of the angular power spec￾trum from the data, the theoretical modelling of the power spec￾trum, and the covariance matrix used in the mult… view at source ↗
Figure 2
Figure 2. Figure 2: The cosmic shear power spectrum from the UNIONS weak lensing sample. Data points are computed with NaMaster using a catalogue-based estimator (see Sect. 3.1). Error bars are obtained using the Gaussian covariance estimator of NaMaster with added non-Gaussian contributions from OneCovariance (see Sect. 3.3). The solid red line corresponds to the best fit ob￾tained using our fiducial setup described in Sect.… view at source ↗
Figure 3
Figure 3. Figure 3: Correlation matrix of the non-tomographic cosmic shear power spectrum. The covariance matrix is estimated using two theory prescriptions, iNKA and OneCovariance. It is com￾pared to the covariance estimated from GLASS mocks. Top pan￾els: Gaussian parts of the theory covariance compared to the simulation covariance. Bottom: Full covariance, including the non-Gaussian part of OneCovariance. The bottom right p… view at source ↗
Figure 5
Figure 5. Figure 5: shows the EB and BB power spectra measured on the non-tomographic UNIONS data, using the procedure de￾scribed in Sect. 3.1. The covariance is estimated using iNKA (see Sect. 3.3 for details). For the EB power spectrum, we obtain a χ 2 of 20 for 32 degrees of freedom, leading to a probability-to￾exceed (PTE) of 0.95. For the BB power spectrum, we measure a χ 2 of 41 for 32 degrees of freedom, amounting to a… view at source ↗
Figure 6
Figure 6. Figure 6: 1D and 2D posteriors on S 8 ≡ σ8(Ωm/0.3)0.5 and Ωm obtained using our fiducial analysis setup in harmonic space (this work, blue contours), configuration space (Goh et al. 2026, orange contours). This is compared to constraints from Planck (pink contours). The consistency between configuration and har￾monic space constraints on S 8 is discussed in Sect. 5.3. Our re￾sults are consistent with Planck at the 0… view at source ↗
Figure 7
Figure 7. Figure 7: Comparison of 1D marginal posterior distributions over the parameters S 8 ≡ σ8(Ωm/0.3)0.5 , σ8, and Ωm from UNIONS (this work), other experiments and consistency tests. (i) Constraints obtained from the harmonic space (this work) and configuration space (Goh et al. 2026) analyses of UNIONS data are shown in red and orange, respectively. (ii) Comparison with constraints obtained from other experiments, incl… view at source ↗
Figure 8
Figure 8. Figure 8: Distribution of χ 2 values obtained on the GLASS mocks at each evaluated best-fit. The vertical dashed line shows the χ 2 value obtained on the data for our fiducial analysis setup. The PTE is computed as the fraction of mocks with a χ 2 larger than the one obtained on the data. −0.100 −0.075 −0.050 −0.025 0.000 0.025 0.050 0.075 0.100 ∆S8 = S8,config − S8,harm 0 2 4 6 8 10 12 Density PTE = 1.5 × 10−2 Nσ =… view at source ↗
Figure 9
Figure 9. Figure 9 [PITH_FULL_IMAGE:figures/full_fig_p011_9.png] view at source ↗
read the original abstract

The Ultraviolet Near Infrared Optical Northern Survey (UNIONS) is a photometric survey in the northern sky. The quality of the data in the $r$ band provides precise shape measurements to measure the growth of structures using cosmic shear. This work aims to constrain cosmological parameters using a harmonic-space estimator of the cosmic shear signal, known as pseudo-$C_\ell$, in a non-tomographic analysis. We perform our analysis in the context of the standard $\Lambda$CDM cosmology. We model astrophysical systematic effects such as baryonic feedback and intrinsic alignments of galaxies. We verify that the point spread function systematic contribution does not affect our results. We assess the impact of different scale cuts and modelling choices on the constraints. We find $S_8 \equiv \sigma_8 \sqrt{\Omega_{\rm m}/0.3} = 0.891^{+0.057}_{-0.084}$, consistent at the $0.79 \, \sigma$ level with \emph{Planck} and between $0.87$ to $1.51 \, \sigma$ with other weak lensing surveys. Our results are robust to analysis choices, and we use lognormal simulations to assess the consistency between configuration and harmonic space results, finding a $2.18 \, \sigma$ agreement between the two statistics. The degeneracy between $S_8$ and the amplitude of the intrinsic alignment, $A_{\rm IA}$, sampled from a prior obtained from direct measurements, is one of the largest sources of uncertainty. This work is part of the first cosmological analysis of the UNIONS survey using cosmic shear and paves the way for future tomographic and $3 \times 2$ point cross-correlation analyses, exploiting the unique overlap of UNIONS with deep spectroscopic surveys in the northern hemisphere.

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.

Circularity Check

0 steps flagged

No significant circularity in the derivation chain

full rationale

The paper reports a standard Bayesian fit of S8 to UNIONS cosmic shear data via the pseudo-C_ℓ estimator in a non-tomographic analysis. The central constraint is obtained after marginalizing over nuisance parameters (including A_IA drawn from an external direct-measurement prior) and after applying scale cuts and baryonic feedback modeling. No equation or step reduces a claimed prediction to a fitted input by construction, no uniqueness theorem is imported from self-citation, and no ansatz is smuggled via prior work. The result is data-driven and externally falsifiable against Planck and other surveys; the noted S8–A_IA degeneracy is a standard uncertainty source rather than a circular reduction.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

The result is a standard Bayesian fit of cosmological and nuisance parameters to observed shear correlations under LambdaCDM; free parameters are the fitted S8 and IA amplitude.

free parameters (2)
  • S8 = 0.891
    Primary fitted cosmological parameter combining sigma8 and Omega_m
  • A_IA
    Intrinsic alignment amplitude sampled from external prior
axioms (2)
  • domain assumption Standard flat LambdaCDM cosmology governs the matter power spectrum and growth
    Invoked for all modeling of the shear signal
  • domain assumption Baryonic feedback and intrinsic alignments can be modeled with existing parametric forms
    Used to marginalize astrophysical systematics

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