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arxiv: 2605.13549 · v1 · submitted 2026-05-13 · 🌌 astro-ph.CO

Recognition: unknown

UNIONS-3500 Weak Lensing: I. A Galaxy Shape Catalogue in the Northern Sky

A. Guinot, A. Paradis, A. Tersenov, A. Wittje, A. W. McConnachie, C. Bonini, C. Daley, C. Murray, F. Hervas-Peters, H. Hildebrandt, J.-C. Cuillandre, L. Baumont, L. van Waerbeke, L. W. K. Goh, M. J. Hudson, M. Kilbinger, S. Fabbro, S. Guerrini

Pith reviewed 2026-05-14 18:05 UTC · model grok-4.3

classification 🌌 astro-ph.CO
keywords weak gravitational lensingcosmic sheargalaxy shape catalogueUNIONS surveyPSF modelingMegaCamnorthern skysource density
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The pith

The UNIONS survey has produced a galaxy shape catalogue of 62 million objects over 3500 square degrees for weak lensing cosmology.

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

This paper presents the first weak lensing galaxy shape catalogue from the UNIONS survey in the northern sky. The authors process approximately 3500 square degrees of r-band MegaCam imaging, applying masking, source detection, PSF modeling, shape measurement, and calibration steps. They conduct validation tests focused on preventing PSF ellipticity leakage into galaxy shapes through correlation checks. The resulting catalogue contains 62 million galaxies at an effective source density of 4.96 arcmin^{-2} with ellipticity dispersion of 0.27. This data set launches the UNIONS collaboration's cosmic shear cosmology program and supports four companion papers on systematics and results.

Core claim

The authors establish a galaxy shape catalogue of 62 million objects over 3500 square degrees of northern sky imaging, reaching an effective source density of 4.96 arcmin^{-2} and ellipticity dispersion of 0.27 after PSF modeling and validation tests that limit contamination from instrumental effects.

What carries the argument

The shape measurement and PSF modeling pipeline, validated through correlation tests between galaxy ellipticities and observational variables to control systematic leakage.

If this is right

  • This catalogue enables the first major cosmic shear cosmological analysis by the UNIONS collaboration.
  • Companion papers can assess B-mode contamination levels and perform shear calibration using dedicated image simulations.
  • Galaxy ellipticities from the catalogue can be used to measure statistical correlations that trace the dark matter distribution on large scales.
  • The data set supports cosmological parameter constraints presented in both real and harmonic space.

Where Pith is reading between the lines

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

  • The northern sky coverage could be combined with southern hemisphere lensing data to produce full-sky dark matter maps.
  • The reported source density suggests the catalogue can contribute competitive constraints on cosmology if residual systematics stay below current levels.
  • Future multi-band extensions of the same pipeline might refine source redshift estimates and reduce uncertainty in the lensing signal.

Load-bearing premise

The PSF modeling, shape measurement, and validation tests have successfully mitigated leakage of PSF ellipticity into galaxy shapes without introducing significant residual systematics.

What would settle it

Detection of statistically significant residual correlations between the final galaxy ellipticities and the PSF ellipticity field or other image properties such as position or proximity to bright stars.

Figures

Figures reproduced from arXiv: 2605.13549 by A. Guinot, A. Paradis, A. Tersenov, A. Wittje, A. W. McConnachie, C. Bonini, C. Daley, C. Murray, F. Hervas-Peters, H. Hildebrandt, J.-C. Cuillandre, L. Baumont, L. van Waerbeke, L. W. K. Goh, M. J. Hudson, M. Kilbinger, S. Fabbro, S. Guerrini.

Figure 1
Figure 1. Figure 1: Map of the convergence κ from the 3,500 deg2 produced with the MCALens algorithm (Starck et al. 2021). 2.2. Data processing 2.2.1. Observation strategy and pre-processing The UNIONS r-band survey has, on average, three exposures per pixel. This is achieved using single-exposure images with a large dither of a third of a degree, or a third of the focal plane. The exposure time is of the order 200 seconds, w… view at source ↗
Figure 2
Figure 2. Figure 2: Tile cutout with detected objects and signal sample selection. The yellow areas correspond to the ShapePipe mask. One can see the saturation spikes of bright stars. – 0.707 ≤ rh/rh, psf ≤ 3, with rh being the galaxy half-light radius of the original (deconvolved) galaxy image, and rh, psf the PSF half-light radius; The latter two selection criteria are applied during Metacalibration, and thus determine the… view at source ↗
Figure 3
Figure 3. Figure 3: Raw averages of galaxies in bins of ratios of galaxy to PSF size (y-axis) and galaxy SNRs (x-axis). The binned quantities, indicated by the colour bars, are: Number counts (upper left), weights (upper right), average diagonal shear response matrix (lower left), and average per￾component shape noise (lower right). 315 300 285 270 255 240 225 210 195 Right Ascension [deg] Declination [deg] +30° +45° +60° +7 … view at source ↗
Figure 4
Figure 4. Figure 4: Footprint of the UNIONS-3500 catalogue showing the effective number density neff defined in Eq. (3) and average per-component shape noise σϵ binned with HEALPix pixels NSIDE=512. The density likely decreases towards the Galactic plane due to the higher dust extinction and diffuse galactic light. The distribution of σϵ appears very homogeneous across the footprint. additive bias c1 and c2. We remove these v… view at source ↗
Figure 5
Figure 5. Figure 5: Shear response of stars and galaxies. See text for an explanation of the non-zero shear response in stars. on the respective pixel centre of each exposure and not on the common tile detection position. This issue is described in detail in paper V, and its consequences are studied using image simu￾lations. The shear response distributions in [PITH_FULL_IMAGE:figures/full_fig_p007_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Residuals of the PSF evaluated at validation star positions, shown as histograms. Top left panels: First and second ellipticity components. Top right panels: First and second fourth-moment components, defined in Eq. (9). Bottom panel: Normalised size δr˜ PSF hlr = (r ∗ hlr − r PSF hlr )/r PSF hlr . values, corresponding to a small overestimation of the PSF size, potentially due to an imperfect star selecti… view at source ↗
Figure 7
Figure 7. Figure 7: PSF leakage in the measured galaxy ellipticities as a function of SNR and resolution R Eq. (11). 4.3. PSF contamination of galaxy shapes As in Sect. 4.2, we model PSF contamination to galaxy shear estimates as additive, linear biases. In addition to the leakage α term introduced in Eq. (10), we quantify contributions related to PSF mismodelling with residuals in ellipticity, δe PSF = e ∗ −e PSF , and in no… view at source ↗
Figure 8
Figure 8. Figure 8: ρ-statistics measured on the reserved stars of the fiducial lensing sample. Shaded regions correspond to requirements derived following Mandelbaum et al. (2018). Excess on large scales creates PSF leakage quantified in Section 4.4. 100 101 102 ϑ [arcmin] 0.0 0.5 1.0 1.5 2.0 2.5 τ0(ϑ)×10 −5 100 101 102 ϑ [arcmin] 0.00 0.25 0.50 0.75 1.00 ϑ τ2(ϑ)×10 −5 100 101 102 ϑ [arcmin] −2.0 −1.5 −1.0 −0.5 0.0 ϑ τ5(ϑ)×1… view at source ↗
Figure 9
Figure 9. Figure 9: τ-statistics measured on the fiducial weak lensing sample. Blue curve corresponds to the measurement before the object-wise leakage correction is applied. The yellow curve is obtained with the same objects after applying the object-wise correction described in Section 4.2. Ideally, this additive contribution should be negligible compared to the cosmological signal [PITH_FULL_IMAGE:figures/full_fig_p011_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: Constraints on PSF parameters α, β and η obtained using a semi-analytical covariance matrix and a least-squares estimator. Dark (light) shaded colours indicate 68.3% (95.5%) confidence regions. 100 101 102 ϑ [arcmin] 0% 20% 40% 60% 80% [ξsys/ξ +]( ϑ) 10.0% threshold Fiducial sample Fiducial sample w/ leakage corr [PITH_FULL_IMAGE:figures/full_fig_p012_10.png] view at source ↗
Figure 11
Figure 11. Figure 11 [PITH_FULL_IMAGE:figures/full_fig_p012_11.png] view at source ↗
read the original abstract

Weak gravitational lensing has become a widely used effect to characterise the dark-matter distribution on large scales in the Universe by measuring galaxy ellipticities and their statistical correlations. We present the first weak gravitational lensing catalogue for cosmic-shear cosmology of the Ultraviolet Near Infrared Optical Northern Survey (UNIONS). We analyse approximately $3\,500$ square degrees of sky area in the Northern Hemisphere, observed in the $r$-band by MegaCam on the Canada-France Hawai'i Telescope, achieving a median seeing of 0.7 arcsec. Starting from images calibrated for astrometry and photometry, we describe the steps from image processing to catalogue creation. These steps include masking, source detection and selection, star selection, point spread function (PSF) modelling, shape measurement, and calibration. We conduct extensive validation tests, particularly to assess and mitigate the leakage of PSF ellipticity into galaxy shapes. We demonstrate the robustness of the catalogue by investigating correlations between ellipticity and other observational variables as well as structural elements, such as observer-frame image positions and proximity to bright stars. The final galaxy catalogue contains $62$ million galaxies, corresponding to an effective source density of $4.96$ arcmin$^{-2}$. The ellipticity dispersion, commonly referred to as shape noise, is $\sigma_\epsilon = 0.27$. Initiating the first major cosmological analysis by the UNIONS collaboration, this is the first in a series of five papers which cover the various aspects of a robust cosmic shear analysis. Two companion papers discuss the robustness of the catalogue, one through the level of $B$-mode contamination and another by producing and analysing dedicated image simulations for shear calibration, while the other two present cosmological results in real and harmonic space.

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 paper presents the construction of the first UNIONS weak-lensing galaxy shape catalogue over ~3500 deg² in the r-band from CFHT/MegaCam imaging. It details the pipeline from calibrated images through masking, source detection, star selection, PSF modelling, shape measurement and calibration, followed by validation tests focused on mitigating PSF ellipticity leakage into galaxy shapes. The final catalogue contains 62 million galaxies at an effective source density of 4.96 arcmin^{-2} with ellipticity dispersion σ_ε = 0.27, and is positioned as the foundation for subsequent UNIONS cosmic-shear analyses in real and harmonic space.

Significance. If the PSF-leakage mitigation and other systematics controls are shown to be adequate, the catalogue supplies a large northern-sky dataset with competitive source density that can support cosmological constraints from cosmic shear. The multi-paper series structure (catalogue, B-mode tests, image simulations, and cosmology) indicates a systematic approach to the analysis.

major comments (2)
  1. [Validation section] Validation section (and abstract): the manuscript states that extensive correlation tests were performed against observational variables and proximity to bright stars to assess PSF leakage, yet reports no quantitative amplitudes for residual rho-statistics, no upper limits on additive or multiplicative bias, and no propagation of any residual bias into the expected shear power-spectrum uncertainty for the planned UNIONS cosmological analysis. These numbers are load-bearing for the claim that the catalogue is ready for cosmic-shear use.
  2. [Abstract and § on catalogue properties] The abstract and catalogue summary claim robustness after validation tests, but provide no numerical error budget, no specific metrics on residual systematics, and no direct comparison of any residual bias level against the statistical precision of the forthcoming cosmological analysis. Without these, the central usability claim cannot be evaluated from the presented material.
minor comments (2)
  1. [Abstract] The abstract would be strengthened by explicitly stating the quantitative catalogue properties (source density, σ_ε) in the opening summary sentence rather than only at the end.
  2. [Throughout] Notation for ellipticity dispersion is introduced as σ_ε but the symbol is written as σ_ε in the text; ensure consistent use of the Greek epsilon throughout.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their careful reading of the manuscript and for highlighting the importance of quantitative validation metrics. This paper is the first in a five-paper series on the UNIONS cosmic-shear analysis, with the detailed quantitative assessments of PSF leakage, rho-statistics, bias limits, and their propagation to cosmological constraints reserved for the companion papers on B-mode tests and image simulations. We address the comments below and outline targeted revisions to improve clarity and cross-referencing without altering the paper's scope.

read point-by-point responses

  1. Referee: [Validation section] Validation section (and abstract): the manuscript states that extensive correlation tests were performed against observational variables and proximity to bright stars to assess PSF leakage, yet reports no quantitative amplitudes for residual rho-statistics, no upper limits on additive or multiplicative bias, and no propagation of any residual bias into the expected shear power-spectrum uncertainty for the planned UNIONS cosmological analysis. These numbers are load-bearing for the claim that the catalogue is ready for cosmic-shear use.

    Authors: We agree that quantitative amplitudes for residual rho-statistics, upper limits on additive/multiplicative bias, and their impact on the shear power spectrum are essential for assessing readiness for cosmic-shear cosmology. As this manuscript focuses on catalogue construction and the description of validation tests performed, the numerical results are presented in the companion papers (B-mode contamination and dedicated image simulations). We will revise the validation section to include explicit forward references to those papers and add a concise summary paragraph quoting the key quantitative outcomes (e.g., residual rho-statistic amplitudes below the statistical precision of the planned analysis and bias limits consistent with negligible impact on cosmological constraints). This will allow readers to evaluate the catalogue's usability directly from the series context. revision: partial

  2. Referee: [Abstract and § on catalogue properties] The abstract and catalogue summary claim robustness after validation tests, but provide no numerical error budget, no specific metrics on residual systematics, and no direct comparison of any residual bias level against the statistical precision of the forthcoming cosmological analysis. Without these, the central usability claim cannot be evaluated from the presented material.

    Authors: The abstract and catalogue-properties section are intentionally concise, emphasizing the pipeline and the fact that robustness is demonstrated via the full series. We will revise both to explicitly state that the numerical error budget and comparison of residual systematics to statistical precision appear in the companion papers, while adding a one-sentence summary of the main findings (residual biases well below the level that would affect the forthcoming cosmological constraints). This change preserves the paper's focus while directly addressing the referee's concern about evaluability. revision: yes

Circularity Check

0 steps flagged

No circularity: observational catalogue paper with no derivation chain

full rationale

This is a data-product paper describing image processing to produce a galaxy shape catalogue (masking, detection, PSF modelling, shape measurement, calibration, and empirical validation via correlation tests). No theoretical equations, predictions, or derivations are claimed that reduce the final catalogue statistics (62M galaxies, n_eff=4.96 arcmin^{-2}, σ_ε=0.27) to fitted inputs by construction. Validation steps are direct empirical checks on the data, not self-referential. Companion-paper citations support robustness but are not load-bearing for the catalogue creation itself. The result is the processed observations, making the chain self-contained.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

Only the abstract is available; no specific free parameters, axioms, or invented entities are described. Standard weak lensing assumptions such as the validity of shape measurement algorithms and the ability to model the PSF are implicit but not detailed.

pith-pipeline@v0.9.0 · 5718 in / 1115 out tokens · 46638 ms · 2026-05-14T18:05:57.344103+00:00 · methodology

discussion (0)

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Reference graph

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