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arxiv: 2606.26223 · v1 · pith:IPDSDCWLnew · submitted 2026-06-24 · 🌌 astro-ph.CO

Cross-correlation of SPT-3G D1 CMB lensing and DES Y3 galaxy lensing

A. Ouellette , Y. Omori , E. Anderes , A. J. Anderson , B. Ansarinejad , M. Archipley , L. Balkenhol , D. R. Barron
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K. Benabed A. N. Bender B. A. Benson F. Bianchini L. E. Bleem S. Bocquet F. R. Bouchet E. Camphuis M. G. Campitiello J. E. Carlstrom J. Carron C. Chang C. L. Chang P. M. Chichura A. Chokshi T.-L. Chou A. Coerver T. M. Crawford C. Daley T. de Haan K. R. Dibert M. A. Dobbs M. Doohan D. Dutcher C. Feng K. R. Ferguson N. C. Ferree K. Fichman A. Foster S. Galli A. E. Gambrel A. K. Gao F. Ge F. Guidi S. Guns N. W. Halverson E. Hivon G. P. Holder W. L. Holzapfel J. C. Hood A. Hryciuk N. Huang T. Jhaveri F. K\'eruzor\'e A. R. Khalife L. Knox K. Kornoelje C.-L. Kuo K. Levy Y. Li A. E. Lowitz C. Lu G. P. Lynch T. J. Maccarone A. S. Maniyar E. S. Martsen F. Menanteau M. Millea J. Montgomery Y. Nakato T. Natoli Z. Pan P. Paschos K. A. Phadke A. W. Pollak K. Prabhu W. Quan M. Rahimi A. Rahlin C. L. Reichardt M. Rouble J. E. Ruhl A. C. Silva Oliveira A. Simpson J. A. Sobrin A. A. Stark J. Stephen C. Tandoi C. Trendafilova J. D. Vieira A. G. Vieregg A. Vitrier Y. Wan N. Whitehorn W. L. K. Wu M. R. Young J. A. Zebrowski
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Pith reviewed 2026-06-26 01:39 UTC · model grok-4.3

classification 🌌 astro-ph.CO
keywords CMB lensingcosmic shearcross-correlationS8weak lensingDES Y3SPT-3Gintrinsic alignments
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The pith

Cross-correlation of CMB lensing and galaxy lensing measured at 14 sigma with polarization-only maps

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

This paper measures the cross-correlation between CMB lensing from SPT-3G and galaxy weak lensing from DES Y3 over about 1300 square degrees of sky. It achieves roughly 14 sigma significance for the first time by relying on a polarization-only CMB lensing reconstruction that avoids biases from extragalactic foregrounds in temperature data. The analysis yields an S8 value of 0.833 with asymmetric uncertainties that matches both Planck primary CMB results and DES shear-only results. The cross-correlation therefore functions as a consistency test between two lensing probes while also placing limits on intrinsic alignments and baryonic feedback.

Core claim

We present measurements of the cross-correlation between CMB lensing and cosmic shear over ~1,300 deg2 of the sky using the SPT-3G D1 CMB lensing maps and the Dark Energy Survey Year 3 (DES Y3) shear catalogs. For the first time, we measure this cross-correlation at high significance (~14σ) when using a polarization-only CMB lensing reconstruction that is expected to be robust against biases induced by extragalactic foregrounds. We test a variety of other CMB lensing estimators that include temperature information and exhibit different tradeoffs between foreground biases and noise, as well as a shear sample that consists of blue, star-forming galaxies and has been shown to be less impacted b

What carries the argument

Polarization-only CMB lensing reconstruction crossed with the DES Y3 galaxy shear catalog to form the cross-power spectrum; this estimator uses only E and B polarization modes to map the lensing potential and thereby sidesteps temperature foreground contamination.

If this is right

  • The cross-correlation supplies an independent S8 constraint that matches both Planck and DES shear-only values.
  • It returns a constraint on the intrinsic alignment amplitude of the DES sample that is competitive with shear-only analyses.
  • Combining the cross-correlation with Planck data produces a lower limit on the strength of baryonic feedback.
  • Multiple CMB lensing estimators display distinct tradeoffs between foreground bias and noise levels.
  • A blue, star-forming galaxy shear sample reduces the impact of intrinsic alignments relative to the full sample.

Where Pith is reading between the lines

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

  • The polarization-only approach could be applied to other overlapping CMB and optical surveys to reduce foreground-related systematics in lensing cross-checks.
  • Prioritizing blue galaxy samples in future shear analyses may lower the modeling burden from intrinsic alignments.
  • The observed consistency between probes suggests that cross-correlations can help isolate the contribution of specific astrophysical effects such as feedback.
  • Testing the same cross-correlation on independent sky patches would provide a direct check on the stability of the 14 sigma detection.

Load-bearing premise

The analysis assumes a flat LambdaCDM cosmology and that the modeled uncertainties in intrinsic alignments, baryonic feedback, and nuisance parameters fully capture the relevant systematics.

What would settle it

A future measurement of the same cross-correlation using improved foreground modeling that yields an S8 value in significant tension with 0.833 would indicate that unaccounted biases remain in the polarization-only result.

Figures

Figures reproduced from arXiv: 2606.26223 by A. A. Stark, A. Chokshi, A. Coerver, A. C. Silva Oliveira, A. E. Gambrel, A. E. Lowitz, A. Foster, A. G. Vieregg, A. Hryciuk, A. J. Anderson, A. K. Gao, A. N. Bender, A. Ouellette, A. Rahlin, A. R. Khalife, A. Simpson, A. S. Maniyar, A. Vitrier, A. W. Pollak, B. A. Benson, B. Ansarinejad, C. Chang, C. Daley, C. Feng, C. L. Chang, C.-L. Kuo, C. L. Reichardt, C. Lu, C. Tandoi, C. Trendafilova, D. Dutcher, D. R. Barron, E. Anderes, E. Camphuis, E. Hivon, E. S. Martsen, F. Bianchini, F. Ge, F. Guidi, F. K\'eruzor\'e, F. Menanteau, F. R. Bouchet, G. P. Holder, G. P. Lynch, J. A. Sobrin, J. A. Zebrowski, J. Carron, J. C. Hood, J. D. Vieira, J. E. Carlstrom, J. E. Ruhl, J. Montgomery, J. Stephen, K. A. Phadke, K. Benabed, K. Fichman, K. Kornoelje, K. Levy, K. Prabhu, K. R. Dibert, K. R. Ferguson, L. Balkenhol, L. E. Bleem, L. Knox, M. A. Dobbs, M. Archipley, M. Doohan, M. G. Campitiello, M. Millea, M. Rahimi, M. Rouble, M. R. Young, N. C. Ferree, N. Huang, N. W. Halverson, N. Whitehorn, P. M. Chichura, P. Paschos, S. Bocquet, S. Galli, S. Guns, T. de Haan, T. Jhaveri, T. J. Maccarone, T.-L. Chou, T. M. Crawford, T. Natoli, W. L. Holzapfel, W. L. K. Wu, W. Quan, Y. Li, Y. Nakato, Y. Omori, Y. Wan, Z. Pan.

Figure 1
Figure 1. Figure 1: FIG. 1. Survey footprints for the SPT-3G Main field and DES [PITH_FULL_IMAGE:figures/full_fig_p003_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: FIG. 2 [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: FIG. 3. Measured [PITH_FULL_IMAGE:figures/full_fig_p008_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: FIG. 4. Same as Fig [PITH_FULL_IMAGE:figures/full_fig_p008_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: FIG. 5. Normalized data covariance matrix for the [PITH_FULL_IMAGE:figures/full_fig_p010_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: FIG. 6. Measurement validation on the [PITH_FULL_IMAGE:figures/full_fig_p013_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: FIG. 7. Distributions of [PITH_FULL_IMAGE:figures/full_fig_p014_7.png] view at source ↗
Figure 9
Figure 9. Figure 9: FIG. 9 [PITH_FULL_IMAGE:figures/full_fig_p014_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: FIG. 10. Marginalized posteriors in the Ω [PITH_FULL_IMAGE:figures/full_fig_p016_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: FIG. 11. Effect of different analysis choices on the resulting [PITH_FULL_IMAGE:figures/full_fig_p017_11.png] view at source ↗
Figure 12
Figure 12. Figure 12: FIG. 12. Cosmological and astrophysical constraints from the combination of [PITH_FULL_IMAGE:figures/full_fig_p019_12.png] view at source ↗
Figure 13
Figure 13. Figure 13: FIG. 13. Top row [PITH_FULL_IMAGE:figures/full_fig_p021_13.png] view at source ↗
Figure 14
Figure 14. Figure 14: FIG. 14. Full posteriors for the [PITH_FULL_IMAGE:figures/full_fig_p022_14.png] view at source ↗
read the original abstract

Measurements of the weak lensing of galaxies and of the cosmic microwave background (CMB) provide direct probes of the cosmic matter density field, but the two observables are sensitive to different spatial scales, redshift ranges, and survey systematics. Their cross-correlation thus enables consistency checks of the theoretical model and of potential systematics in either dataset. We present measurements of the cross-correlation between CMB lensing and cosmic shear over $\sim$1,300 deg$^2$ of the sky using the SPT-3G D1 CMB lensing maps and the Dark Energy Survey Year 3 (DES Y3) shear catalogs. For the first time, we measure this cross-correlation at high significance ($\sim 14\sigma$) when using a polarization-only CMB lensing reconstruction that is expected to be robust against biases induced by extragalactic foregrounds. We test a variety of other CMB lensing estimators that include temperature information and exhibit different tradeoffs between foreground biases and noise, as well as a shear sample that consists of blue, star-forming galaxies and has been shown to be less impacted by galaxy intrinsic alignments. Assuming $\Lambda$CDM and marginalizing over uncertainties in intrinsic alignments, baryonic feedback, and various nuisance parameters, we obtain a constraint on the amplitude of matter clustering $S_8 \equiv \sigma_8 \sqrt{\Omega_m / 0.3} = 0.833^{+0.047}_{-0.061}$, consistent with both the primary CMB results from Planck and shear-only results from DES Y3. By combining our measurement with Planck, we find mild constraints on the astrophysical processes that impact the cross-correlation. We obtain a constraint on the intrinsic alignment amplitude of the DES sample that is competitive with that from shear-only analyses, and we find a lower limit on the strength of baryonic feedback.

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

0 major / 4 minor

Summary. The manuscript reports a cross-correlation measurement between SPT-3G D1 CMB lensing (using a polarization-only reconstruction) and DES Y3 galaxy shear catalogs over ~1300 deg². It claims a ~14σ detection significance, derives the constraint S_8 = 0.833^{+0.047}_{-0.061} under ΛCDM after marginalizing over intrinsic alignments, baryonic feedback, and nuisance parameters, and finds consistency with Planck primary CMB results and DES Y3 shear-only results. The analysis also combines the cross-correlation with Planck data to obtain a competitive constraint on the DES intrinsic alignment amplitude and a lower limit on the strength of baryonic feedback, while testing alternative CMB lensing estimators (including those with temperature information) and a blue-galaxy shear sample.

Significance. If the central measurement and modeling hold, this work supplies a valuable consistency test between two independent weak-lensing probes that are sensitive to different redshifts and scales. The polarization-only CMB lensing map is a clear strength because it is expected to be robust against extragalactic foreground biases; the explicit comparison of multiple estimators and the use of a blue-galaxy sample (less affected by intrinsic alignments) further strengthen the robustness claims. The derived S_8 constraint is competitive, and the joint analysis with Planck yields astrophysical constraints on intrinsic alignments and baryonic feedback that are not available from either dataset alone.

minor comments (4)
  1. [Abstract] Abstract: the reported detection significance (~14σ) is given without stating whether it is computed from the signal-to-noise ratio of the binned cross-power spectrum, from a χ² test against the null hypothesis, or from another estimator; adding this detail would clarify the claim.
  2. [Methods / Modeling section] The text refers to “various nuisance parameters” that are marginalized over, but does not list them explicitly in one place (e.g., multiplicative bias, photo-z shifts, shear calibration); a compact table or paragraph summarizing all marginalized parameters and their priors would improve readability.
  3. [Results figures] Figure captions for the cross-power spectrum plots should state the exact multipole binning, the covariance estimation method (jackknife, simulations, or analytic), and whether the plotted errors include the full covariance or only diagonal terms.
  4. [Shear sample section] The blue-galaxy sample is stated to be “less impacted by galaxy intrinsic alignments,” but the quantitative reduction in the IA amplitude relative to the full sample is not shown; a short comparison plot or table would support this statement.

Simulated Author's Rebuttal

0 responses · 0 unresolved

We thank the referee for their positive assessment of our manuscript, accurate summary of the results, and recommendation for minor revision. We appreciate the recognition of the robustness provided by the polarization-only CMB lensing reconstruction and the value of the consistency test between probes.

Circularity Check

0 steps flagged

No significant circularity; direct data-driven measurement

full rationale

The paper reports a cross-correlation measurement between two independent observational datasets (SPT-3G polarization-only CMB lensing maps and DES Y3 galaxy shear catalogs) over ~1300 deg², achieving ~14σ significance. The S8 constraint is obtained by fitting the measured correlation function under ΛCDM while marginalizing over IA, baryonic feedback, and nuisance parameters. No load-bearing step reduces by construction to a fitted input, self-citation chain, or ansatz smuggled from prior work; the central result is externally falsifiable against Planck and DES Y3 shear-only analyses. The derivation chain is self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

2 free parameters · 1 axioms · 0 invented entities

The measurement rests on the assumption that the polarization-only lensing map is unbiased after foreground mitigation and that the DES shear catalog systematics are adequately captured by the marginalized nuisance parameters.

free parameters (2)
  • S8
    Amplitude of matter clustering fitted from the cross-power spectrum after marginalization.
  • intrinsic alignment amplitude
    Nuisance parameter marginalized over in the fit to the cross-correlation.
axioms (1)
  • domain assumption ΛCDM background cosmology
    Used to model the expected cross-correlation signal.

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Reference graph

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