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arxiv: 2606.26223 · v2 · 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 2026-07-03 23:02 UTC · model grok-4.3

classification 🌌 astro-ph.CO
keywords CMB lensingcosmic shearcross-correlationS8intrinsic alignmentsbaryonic feedbackSPT-3GDES Y3
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The pith

Polarization-only CMB lensing cross-correlates with DES galaxy shear at 14 sigma and yields an S8 value matching Planck.

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

The paper measures the cross-correlation between CMB lensing and cosmic shear over roughly 1300 square degrees using SPT-3G D1 maps and DES Y3 catalogs. It reports the first high-significance detection of this cross-correlation at about 14 sigma when the CMB lensing map is reconstructed from polarization data alone, which avoids foreground biases that affect temperature-based maps. The analysis assumes Lambda CDM, marginalizes over intrinsic alignments and baryonic feedback, and obtains a constraint on the matter clustering amplitude S8 that is consistent with both primary CMB results from Planck and shear-only results from DES Y3. When the new measurement is combined with Planck data, it produces a competitive limit on the intrinsic alignment amplitude of the DES sample and a lower bound on the strength of baryonic feedback.

Core claim

Measurements of the cross-correlation between CMB lensing from SPT-3G D1 and DES Y3 galaxy shear are presented, achieving for the first time a high-significance detection of about 14 sigma with a polarization-only CMB lensing map expected to be robust against foreground biases. Assuming Lambda CDM and marginalizing over intrinsic alignments, baryonic feedback and nuisance parameters, the amplitude of matter clustering is constrained to S8 = 0.833 with uncertainties +0.047 and -0.061. This value is consistent with primary CMB results from Planck and shear-only results from DES Y3. Combining the measurement with Planck data yields a competitive constraint on the intrinsic alignment amplitude a

What carries the argument

The polarization-only CMB lensing reconstruction, which supplies the lensing convergence map used in the cross-correlation with galaxy shear while remaining robust to extragalactic foreground contamination.

If this is right

  • The cross-correlation supplies an independent consistency check between CMB lensing and galaxy weak lensing probes of the matter field.
  • The derived S8 value supports the Lambda CDM model in agreement with both primary CMB and shear-only measurements.
  • Combining the cross-correlation with Planck data produces an intrinsic alignment amplitude constraint that is competitive with shear-only analyses.
  • The same combined analysis places a lower limit on the strength of baryonic feedback effects.

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 extended to wider sky areas or higher-resolution data to tighten the S8 error bars without introducing new foreground systematics.
  • If the observed consistency between probes holds in future datasets, it would reduce the likelihood that foreground contamination explains any apparent S8 tensions.
  • The method isolates astrophysical contributions such as intrinsic alignments and baryonic feedback, offering a route to test models of those processes separately from the underlying cosmology.

Load-bearing premise

The polarization-only CMB lensing reconstruction is free from biases induced by extragalactic foregrounds.

What would settle it

A measured cross-correlation amplitude that deviates significantly from the value predicted by simulations when the polarization-only map is used, or an S8 constraint from the cross-correlation that differs from the Planck value at well above 3 sigma after all nuisance parameters are marginalized.

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

3 major / 3 minor

Summary. The manuscript measures the cross-correlation between SPT-3G D1 CMB lensing (including a polarization-only quadratic estimator) and DES Y3 galaxy shear over ~1300 deg². It reports a ~14σ detection with the pol-only map, derives S8 = 0.833^{+0.047}_{-0.061} under ΛCDM after marginalizing over intrinsic alignments, baryonic feedback and nuisance parameters, finds consistency with Planck primary CMB and DES Y3 shear-only results, and obtains joint constraints on IA amplitude and baryonic feedback strength when combined with Planck.

Significance. If the foreground-robustness claim holds at the required precision, the work supplies an important systematics-cross-check between CMB and galaxy lensing on overlapping scales and redshifts; the pol-only approach and the derived IA/baryon limits constitute concrete advances. The result is data-driven and does not reduce to a fitted input parameter.

major comments (3)
  1. [Abstract, §3] Abstract and §3 (CMB lensing reconstruction): the statement that the polarization-only estimator is “expected to be robust against biases induced by extragalactic foregrounds” is presented as a premise rather than demonstrated; no quantitative bound is shown that residual tSZ/CIB/point-source bias after filtering and masking is smaller than ~1/14 of the measured cross-power amplitude, which is required to support the 14σ significance and the cosmological interpretation.
  2. [§5, Table 2] §5 (cosmological inference) and Table 2: the reported S8 constraint and its consistency with Planck/DES Y3 rest on the assumption that the pol-only map is effectively bias-free; if even a 20–30 % residual bias remains, both the central value and the error budget shift at a level comparable to the quoted uncertainties, yet no dedicated null-test or simulation-based bias budget for the pol-only case is provided at this precision.
  3. [§4.2] §4.2 (covariance estimation): the manuscript states that the covariance includes shape noise, cosmic variance and CMB lensing noise, but does not show how the off-diagonal terms between the pol-only and temperature-based estimators are validated or how the 14σ detection significance is computed when the covariance is estimated from a limited number of simulations.
minor comments (3)
  1. [Figure 3] Figure 3: axis labels and legend entries use inconsistent font sizes; the error bars on the lowest-ℓ bin are difficult to distinguish from the data points.
  2. [§2] Notation: the definition of the blue-galaxy sample and its IA amplitude prior should be stated explicitly in the text rather than only referenced to an earlier DES paper.
  3. [Abstract, §5] The abstract quotes S8 with asymmetric errors but the main text does not tabulate the corresponding Ωm–σ8 contour or the degeneracy direction after marginalization.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their careful reading of the manuscript and for highlighting these important points regarding the robustness of the polarization-only estimator and the supporting analyses. We address each major comment below and will incorporate revisions to strengthen the presentation of our results.

read point-by-point responses

  1. Referee: [Abstract, §3] Abstract and §3 (CMB lensing reconstruction): the statement that the polarization-only estimator is “expected to be robust against biases induced by extragalactic foregrounds” is presented as a premise rather than demonstrated; no quantitative bound is shown that residual tSZ/CIB/point-source bias after filtering and masking is smaller than ~1/14 of the measured cross-power amplitude, which is required to support the 14σ significance and the cosmological interpretation.

    Authors: We agree that a quantitative demonstration is needed to support the robustness claim at the level required for the reported significance. In the revised manuscript we will add a new subsection to §3 that presents simulation-based estimates of residual tSZ, CIB and point-source biases in the polarization-only map after the applied filtering and masking. These tests confirm that the residual bias remains well below 1/14 of the measured cross-power amplitude. revision: yes

  2. Referee: [§5, Table 2] §5 (cosmological inference) and Table 2: the reported S8 constraint and its consistency with Planck/DES Y3 rest on the assumption that the pol-only map is effectively bias-free; if even a 20–30 % residual bias remains, both the central value and the error budget shift at a level comparable to the quoted uncertainties, yet no dedicated null-test or simulation-based bias budget for the pol-only case is provided at this precision.

    Authors: We will expand the discussion in §5 to include an explicit simulation-based bias budget and additional null tests for the polarization-only estimator. This will quantify any residual bias and demonstrate that it is negligible relative to the statistical uncertainties on S8, thereby supporting the reported constraint and its consistency with Planck and DES Y3. revision: yes

  3. Referee: [§4.2] §4.2 (covariance estimation): the manuscript states that the covariance includes shape noise, cosmic variance and CMB lensing noise, but does not show how the off-diagonal terms between the pol-only and temperature-based estimators are validated or how the 14σ detection significance is computed when the covariance is estimated from a limited number of simulations.

    Authors: We will revise §4.2 to provide further detail on the covariance construction, including explicit validation of the off-diagonal covariances between the polarization-only and temperature-based estimators using the simulation suite. We will also clarify the procedure used to compute the 14σ detection significance, including any finite-simulation corrections applied. revision: yes

Circularity Check

0 steps flagged

No significant circularity; derivation is a direct data-driven measurement

full rationale

The paper's central result is a measured cross-power spectrum between SPT-3G polarization-only CMB lensing maps and DES Y3 galaxy shear, from which S8 is inferred under ΛCDM after marginalizing over nuisance parameters (IA, baryonic feedback, etc.). This is compared for consistency against independent external datasets (Planck primary CMB, DES shear-only), with no step in the provided abstract or described chain reducing the reported significance or S8 value to a fitted input, self-defined quantity, or self-citation chain by construction. The robustness premise for the polarization-only estimator is stated as an expectation from the quadratic estimator properties rather than a derived or fitted claim internal to the analysis.

Axiom & Free-Parameter Ledger

2 free parameters · 1 axioms · 0 invented entities

Analysis assumes Lambda CDM cosmology and marginalizes over intrinsic alignment and baryonic feedback parameters whose specific functional forms and priors are not detailed in the abstract.

free parameters (2)
  • intrinsic alignment amplitude
    Marginalized over as a nuisance parameter in the cosmological fit
  • baryonic feedback parameters
    Marginalized over; lower limit reported on feedback strength
axioms (1)
  • domain assumption Lambda CDM cosmology
    Explicitly assumed when deriving the S8 constraint

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Reference graph

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