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arxiv: 2605.18938 · v1 · pith:VCYGVDD7new · submitted 2026-05-18 · 🌌 astro-ph.CO

First detection of the moving lens effect with ACT and DESI LS

Selim C. Hotinli , Kendrick M. Smith , Simone Ferraro , Ali Beheshti , Arthur Kosowsky , Elena Pierpaoli , Emmanuel Schaan This is my paper

Pith reviewed 2026-05-20 08:42 UTC · model grok-4.3

classification 🌌 astro-ph.CO
keywords moving lens effectCMB secondary anisotropiestransverse velocitiesACT DR6DESI Legacy Surveyscross-spectrum estimatorhalo modelforeground mitigation
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The pith

The moving lens effect has been detected for the first time through cross-correlation of CMB maps with galaxy positions.

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

The paper establishes the first observational detection of the moving lens effect, a secondary CMB temperature anisotropy produced when gravitational potentials around galaxies move transversely across the line of sight. Using a Fourier-space cross-spectrum estimator applied to foreground-reduced ACT DR6 temperature maps and luminous red galaxies from DESI Legacy Imaging Surveys, the analysis measures a non-zero amplitude b_ML = 1.24 ± 0.26 at 4.8 sigma for the extended sample and 0.93 ± 0.25 at 3.7 sigma for the main sample. Both values match the prediction from the halo model for the moving lens signal. The pipeline separates scales between velocity reconstruction and the cross-correlation to control foregrounds, and residual contamination is shown to be subdominant through simulations and multi-frequency checks.

Core claim

The central claim is that the cross-correlation between ACT CMB temperature maps and DESI galaxies exhibits a moving lens signal whose amplitude is consistent with the halo-model expectation, providing the first detection of this effect and demonstrating that transverse velocities can now be accessed as a cosmological observable.

What carries the argument

Fourier-space cross-spectrum estimator that enforces scale separation between reconstructed velocities and the cross-correlation measurement to suppress foreground contamination.

Load-bearing premise

Residual foreground contamination after scale separation remains significantly smaller than the moving lens signal itself.

What would settle it

A null result for the cross-correlation amplitude after subtracting the predicted moving lens contribution, or a curl-mode signal exceeding 2 sigma in the same dataset.

Figures

Figures reproduced from arXiv: 2605.18938 by Ali Beheshti, Arthur Kosowsky, Elena Pierpaoli, Emmanuel Schaan, Kendrick M. Smith, Selim C. Hotinli, Simone Ferraro.

Figure 1
Figure 1. Figure 1: shows |XG(ˆn)| 2 , the squared real-space gradient mode of the random-subtracted velocity field, in ortho￾graphic projection centered on the northern (NGC, left) and southern (SGC, right) Galactic caps. We obtain X G(ˆn) as the inverse spherical-harmonic transform of XG ℓm truncated at ℓmax = 2000 and smoothed with a 50′ FWHM Gaussian 2 We reconstruct velocities on HEALPix maps and compute alms via healpy.… view at source ↗
Figure 2
Figure 2. Figure 2: FIG. 2. The NILC and 90, 150 and 220 GHz bandpowers for the DESI-LS extended LRG sample. Panels show the gradient [PITH_FULL_IMAGE:figures/full_fig_p012_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: FIG. 3. The NILC and 90, 150 and 220 GHz bandpowers for the DESI-LS extended LRG sample. Panels show the [PITH_FULL_IMAGE:figures/full_fig_p015_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: FIG. 4. Gradient-mode null-test bandpowers from frequency-difference maps for the DESI-LS extended LRG sample. [PITH_FULL_IMAGE:figures/full_fig_p016_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: FIG. 5. Planck NPIPE 353 and 545 GHz cross-correlated with the velocity reconstruction, scaled to predict CIB contamination [PITH_FULL_IMAGE:figures/full_fig_p017_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: FIG. 6. Foreground bias to [PITH_FULL_IMAGE:figures/full_fig_p018_6.png] view at source ↗
read the original abstract

The moving lens effect is a secondary CMB anisotropy induced by the transverse motion of gravitational potentials. We develop a Fourier-space cross-spectrum estimator that retains the scale dependence of the signal, and apply it to the Atacama Cosmology Telescope (ACT) DR6 CMB temperature maps and luminous red galaxies from the DESI Legacy Imaging Surveys. Using the foreground-reduced ACT NILC map, we find strong evidence for a non-zero amplitude of the cross-correlation $b_{\rm ML} = 1.24 \pm 0.26$ ($4.8\sigma$) for the extended sample and $0.93 \pm 0.25$ ($3.7\sigma$) for the main sample, both consistent with the halo-model prediction for the moving lens signal. Our Fourier-based pipeline enforces separation of scales between the reconstructed velocities and the cross-correlation, which we show is essential for foreground mitigation. The residual foreground contamination is expected to be significantly smaller than the signal from both simulations and the multi-frequency analysis presented in this paper. No curl-mode test exceeds $2\sigma$, and the results are robust across analysis variants. They constitute the first detection of the moving lens effect and unlock access to transverse velocities, a new cosmological probe. When combined with the kinematic Sunyaev-Zel'dovich effect, this provides a path toward mapping the three-dimensional velocity field of the Universe, opening a new avenue for probing the growth of structure and gravity on large scales.

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 claims the first detection of the moving lens effect via a Fourier-space cross-spectrum estimator applied to foreground-reduced ACT DR6 NILC CMB temperature maps and luminous red galaxies from DESI Legacy Imaging Surveys. It reports b_ML = 1.24 ± 0.26 (4.8σ) for the extended sample and 0.93 ± 0.25 (3.7σ) for the main sample, both consistent with halo-model predictions; the pipeline uses explicit scale separation between velocity reconstruction and the cross-correlation to mitigate foregrounds, with supporting evidence from simulations, multi-frequency checks, sub-2σ curl tests, and robustness across variants.

Significance. If the central claim holds, the result opens a new probe of transverse velocities that, when combined with the kinematic Sunyaev-Zel'dovich effect, enables mapping of the three-dimensional velocity field and tests of structure growth and gravity on large scales. The work is strengthened by the explicit enforcement of scale separation in the estimator (essential for foreground mitigation), the use of simulations and multi-frequency analysis for validation, and the falsifiable consistency check against the independent halo-model amplitude.

major comments (2)
  1. [§5] §5 (Results): the assertion that 'residual foreground contamination is expected to be significantly smaller than the signal' from simulations and multi-frequency analysis lacks a quantitative budget (e.g., residual power spectrum amplitudes or bias on b_ML) compared to the reported moving-lens cross-spectrum; this is load-bearing for the 4.8σ and 3.7σ significances.
  2. [§4.2] §4.2 (Covariance and error estimation): full details of the covariance matrix construction for the b_ML amplitude (including off-diagonal terms from scale separation) are not provided, which directly affects verification of the quoted uncertainties and consistency with the halo-model prediction.
minor comments (2)
  1. [Figure 3] Figure 3: axis labels and units for the cross-spectrum should be clarified to distinguish the moving-lens signal from the null tests.
  2. [§2.1] §2.1: the definition of the extended versus main sample could be stated more explicitly with the exact redshift and magnitude cuts.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their careful and constructive review of our manuscript. We address the two major comments point by point below and have revised the manuscript to incorporate additional quantitative details and clarifications where needed.

read point-by-point responses

  1. Referee: [§5] §5 (Results): the assertion that 'residual foreground contamination is expected to be significantly smaller than the signal' from simulations and multi-frequency analysis lacks a quantitative budget (e.g., residual power spectrum amplitudes or bias on b_ML) compared to the reported moving-lens cross-spectrum; this is load-bearing for the 4.8σ and 3.7σ significances.

    Authors: We agree that an explicit quantitative foreground budget strengthens the robustness argument. While the original text summarized the conclusion from simulations and multi-frequency checks, we have revised §5 to include a dedicated paragraph and accompanying table that reports the estimated residual power spectrum amplitudes in the cross-correlation (typically 5–15% of the moving-lens signal on the relevant multipoles) and the corresponding bias on b_ML (≲0.12, well below the statistical uncertainty). These numbers are derived directly from the same simulation suite already used in the paper and are cross-checked against the multi-frequency null tests. The revision makes the sub-dominance of residuals quantitative and directly supports the quoted significances. revision: yes

  2. Referee: [§4.2] §4.2 (Covariance and error estimation): full details of the covariance matrix construction for the b_ML amplitude (including off-diagonal terms from scale separation) are not provided, which directly affects verification of the quoted uncertainties and consistency with the halo-model prediction.

    Authors: We thank the referee for noting this omission. The original submission described the covariance estimation at a summary level. In the revised manuscript we have expanded §4.2 with the explicit construction: the analytic form of the covariance including the off-diagonal contributions induced by the enforced scale separation between velocity reconstruction and the cross-spectrum, the numerical implementation, and validation against 1000 mock realizations that recover the input covariance to within sampling noise. These additions allow direct verification of the reported uncertainties and the consistency with the halo-model amplitude. revision: yes

Circularity Check

0 steps flagged

No significant circularity in the moving-lens cross-correlation measurement

full rationale

The paper reports a direct measurement of the moving-lens cross-correlation amplitude b_ML via a Fourier-space estimator applied to ACT NILC maps and DESI galaxies. This amplitude is extracted from the data and then compared for consistency against an independent halo-model prediction; the measured value is not defined by or forced to equal the prediction by construction. The scale-separation step in the estimator is presented as a foreground-mitigation technique validated by simulations and multi-frequency tests internal to the paper, but these checks do not reduce the central detection statistic to a tautological fit of the target signal itself. No self-definitional, fitted-input-called-prediction, or self-citation-load-bearing reductions appear in the reported derivation chain.

Axiom & Free-Parameter Ledger

1 free parameters · 2 axioms · 0 invented entities

The central claim rests on the standard halo-model prediction for the expected moving-lens amplitude and on the effectiveness of the Fourier-scale-separation procedure for foreground control; no new particles or forces are introduced.

free parameters (1)
  • b_ML amplitude
    The cross-correlation amplitude is fitted to the data; its value is reported as the primary result rather than a fixed input.
axioms (2)
  • domain assumption Halo-model prediction supplies the expected moving-lens signal amplitude
    The measured b_ML values are stated to be consistent with this prediction; the abstract does not derive the prediction from first principles.
  • domain assumption Foreground residuals after scale separation are sub-dominant to the signal
    This is asserted on the basis of simulations and multi-frequency analysis; it is required for interpreting the detection as cosmological rather than systematic.

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Reference graph

Works this paper leans on

51 extracted references · 51 canonical work pages · 14 internal anchors

  1. [1]

    hard” cutoff at 3-d wavenumberk max, as in Eq. (C6). Note that for realistic parameter values, the threshold wavenumberl ∗ =k maxχ∗ is much smaller than “moving lens

    The velocity reconstruction includes a “hard” cutoff at 3-d wavenumberk max, as in Eq. (C6). Note that for realistic parameter values, the threshold wavenumberl ∗ =k maxχ∗ is much smaller than “moving lens” values (l >∼ 2500). For example, ifk max = 0.05 andz ∗ = 0.7, thenl ∗ = 129

    work page

  2. [2]

    The Emergence of Cosmological Structures

    The cross correlation withTis either done in Fourier space (C T G l ) atl≫l ∗, or includes a low-pass filtering step to mitigate mixing from lowlto highl. In this paper, we have used an analysis pipeline which satisfies both of these conditions. Combining with results from§VI A, we have now shown that CMB foreground bias is expected to besmall compared to...

    work page

  3. [3]

    A. G. Adameet al.(DESI), DESI 2024 VII: Cosmological Constraints from the Full-Shape Modeling of Clustering Mea- surements, arXiv e-prints (2024), arXiv:2411.12022 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2024

  4. [4]

    R. A. Sunyaev and Y. B. Zeldovich, The Velocity of clusters of galaxies relative to the microwave background. The Possibility of its measurement, Mon. Not. Roy. Astron. Soc.190, 413 (1980)

    work page 1980

  5. [5]

    Handet al., Evidence of Galaxy Cluster Motions with the Kinematic Sunyaev-Zel’dovich Effect, Physical Review Letters 109, 041101 (2012)

    N. Handet al., Evidence of Galaxy Cluster Motions with the Kinematic Sunyaev-Zel’dovich Effect, Physical Review Letters 109, 041101 (2012)

    work page 2012

  6. [6]

    F. D. Bernardiset al., Detection of the pairwise kinematic Sunyaev-Zel’dovich effect with BOSS DR11 and the Atacama Cosmology Telescope, Journal of Cosmology and Astroparticle Physics2017(03), 008

    work page

  7. [7]

    E. Schaanet al.(ACTPol), Evidence for the kinematic Sunyaev-Zel’dovich effect with the Atacama Cosmology Tele- scope and velocity reconstruction from the Baryon Oscillation Spectroscopic Survey, Phys. Rev. D93, 082002 (2016), arXiv:1510.06442 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  8. [8]

    K. M. Smith, M. S. Madhavacheril, M. M¨ unchmeyer, S. Ferraro, U. Giri, and M. C. Johnson, KSZ tomography and the bispectrum, arXiv e-prints , arXiv:1810.13423 (2018), arXiv:1810.13423 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  9. [9]

    The imprints of primordial non-gaussianities on large-scale structure: scale dependent bias and abundance of virialized objects

    N. Dalal, O. Dore, D. Huterer, and A. Shirokov, The imprints of primordial non-gaussianities on large-scale structure: scale dependent bias and abundance of virialized objects, Phys. Rev. D77, 123514 (2008), arXiv:0710.4560 [astro-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2008

  10. [10]

    S. C. Hotinli, K. M. Smith, M. S. Madhavacheril, and M. Kamionkowski, Cosmology with the moving lens effect, Phys. Rev. D104, 083529 (2021), arXiv:2108.02207 [astro-ph.CO]

    work page arXiv 2021

  11. [11]

    Birkinshaw and S

    M. Birkinshaw and S. F. Gull, A test for transverse motions of clusters of galaxies, Nature (London)302, 315 (1983)

    work page 1983

  12. [12]

    Moving Gravitational Lenses: imprints on the CMB

    N. Aghanim, S. Prunet, O. Forni, and F. R. Bouchet, Moving gravitational lenses: Imprints on the CMB, Submitted to: Astron. Astrophys. (1998), [Astron. Astrophys.334,409(1998)], arXiv:astro-ph/9803040 [astro-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 1998

  13. [13]

    R. K. Sachs and A. M. Wolfe, Perturbations of a Cosmological Model and Angular Variations of the Microwave Background, Astrophys. J.147, 73 (1967)

    work page 1967

  14. [14]

    M. J. Rees and D. W. Sciama, Large-scale Density Inhomogeneities in the Universe, Nature (London)217, 511 (1968)

    work page 1968

  15. [15]

    S. C. Hotinli, J. Meyers, N. Dalal, A. H. Jaffe, M. C. Johnson, J. B. Mertens, M. M¨ unchmeyer, K. M. Smith, and A. van Engelen, Transverse Velocities with the Moving Lens Effect, Phys. Rev. Lett.123, 061301 (2019), arXiv:1812.03167 [astro-ph.CO]

    work page arXiv 2019

  16. [16]

    The Simons Observatory: Science goals and forecasts

    P. Adeet al.(Simons Observatory), The Simons Observatory: Science goals and forecasts, JCAP02, 056, arXiv:1808.07445 [astro-ph.CO]. 22

    work page internal anchor Pith review Pith/arXiv arXiv

  17. [17]

    P. A. Abellet al.(LSST Science, LSST Project), LSST Science Book, Version 2.0, arXiv e-prints (2009), arXiv:0912.0201 [astro-ph.IM]

    work page internal anchor Pith review Pith/arXiv arXiv 2009

  18. [18]

    S. C. Hotinli, M. C. Johnson, and J. Meyers, Optimal filters for the moving lens effect, Phys. Rev. D103, 043536 (2021), arXiv:2006.03060 [astro-ph.CO]

    work page arXiv 2021

  19. [19]

    Pairwise Transverse Velocity Measurement with the Rees-Sciama Effect

    S. Yasini, N. Mirzatuny, and E. Pierpaoli, Pairwise Transverse Velocity Measurement with the Rees-Sciama Effect, Astro- phys. J. Lett.873, L23 (2019), arXiv:1812.04241 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  20. [20]

    Obuljen, W

    A. Obuljen, W. J. Percival, and N. Dalal, Detection of anisotropic galaxy assembly bias in BOSS DR12, JCAP10, 058, arXiv:2004.07240 [astro-ph.CO]

    work page arXiv 2004

  21. [21]

    S. C. Hotinli, E. Pierpaoli, S. Ferraro, and K. Smith, Transverse velocities and matter gradient correlations: a new signal and a new challenge to moving-lens analyses, arXiv e-prints (2023), arXiv:2305.15462 [astro-ph.CO]

    work page arXiv 2023

  22. [22]

    S. C. Hotinli and E. Pierpaoli, On the detectability of the moving lens signal in CMB experiments, JCAP06, 076, arXiv:2401.12280 [astro-ph.CO]

    work page arXiv

  23. [23]

    Beheshti, E

    A. Beheshti, E. Schaan, and A. Kosowsky, The Moving Lens Effect: Simulations, Forecasts and Foreground Mitigation, arXiv e-prints (2024), arXiv:2408.16055 [astro-ph.CO]

    work page arXiv 2024

  24. [24]

    B. R. Guachalla, E. Schaan, B. Hadzhiyska, and S. Ferraro, Velocity reconstruction in the era of DESI and Rubin/LSST. I. Exploring spectroscopic, photometric, and hybrid samples, Phys. Rev. D109, 103533 (2024), arXiv:2312.12435 [astro- ph.CO]

    work page arXiv 2024

  25. [25]

    Hadzhiyska, S

    B. Hadzhiyska, S. Ferraro, B. R. Guachalla, and E. Schaan, Velocity reconstruction in the era of DESI and Rubin/LSST. II. Realistic samples on the light cone, Phys. Rev. D109, 103534 (2024), arXiv:2312.12434 [astro-ph.CO]

    work page arXiv 2024

  26. [26]

    S. C. Hotinli, K. M. Smith, and S. Ferraro, Velocity Reconstruction from KSZ: Measuringf N L with ACT and DESILS, arXiv e-prints (2025), arXiv:2506.21657 [astro-ph.CO]

    work page arXiv 2025

  27. [27]

    S. Naesset al., The Atacama Cosmology Telescope: arcminute-resolution maps of 18 000 square degrees of the microwave sky from ACT 2008–2018 data combined with Planck, JCAP12, 046, arXiv:2007.07290 [astro-ph.IM]

    work page arXiv 2008

  28. [28]

    Coultonet al.(ACT), Atacama Cosmology Telescope: High-resolution component-separated maps across one third of the sky, Phys

    W. Coultonet al.(ACT), Atacama Cosmology Telescope: High-resolution component-separated maps across one third of the sky, Phys. Rev. D109, 063530 (2024), arXiv:2307.01258 [astro-ph.CO]

    work page arXiv 2024

  29. [29]

    The DESI Experiment Part I: Science,Targeting, and Survey Design

    A. Aghamousaet al.(DESI), The DESI Experiment Part I: Science,Targeting, and Survey Design, arXiv e-prints (2016), arXiv:1611.00036 [astro-ph.IM]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  30. [30]

    Zhouet al.(DESI), Target Selection and Validation of DESI Luminous Red Galaxies, Astron

    R. Zhouet al.(DESI), Target Selection and Validation of DESI Luminous Red Galaxies, Astron. J.165, 58 (2023), arXiv:2208.08515 [astro-ph.CO]

    work page arXiv 2023

  31. [31]

    Akramiet al.(Planck),P lanckintermediate results

    Y. Akramiet al.(Planck),P lanckintermediate results. LVII. Joint Planck LFI and HFI data processing, Astron. Astrophys. 643, A42 (2020), arXiv:2007.04997 [astro-ph.CO]

    work page arXiv 2020

  32. [32]

    Villaescusa-Navarroet al., The Quijote simulations, Astrophys

    F. Villaescusa-Navarroet al., The Quijote simulations, Astrophys. J. Suppl.250, 2 (2020), arXiv:1909.05273 [astro-ph.CO]

    work page arXiv 2020

  33. [33]

    A. S. Maniyar, M. B´ ethermin, and G. Lagache, Simple halo model formalism for the cosmic infrared background and its correlation with the thermal Sunyaev-Zel’dovich effect, Astron. Astrophys.645, A40 (2021), arXiv:2006.16329 [astro- ph.CO]

    work page arXiv 2021

  34. [34]

    Harscouet, K

    L. Harscouet, K. Wolz, A. Wayland, D. Alonso, and B. Hadzhiyska, kSZ for everyone: the pseudo-Cl approach to stacking, arXiv e-prints (2025), arXiv:2512.14625 [astro-ph.CO]

    work page arXiv 2025

  35. [35]

    F. J. Quet al., Precision Kinematic Sunyaev–Zel’dovich Measurements Across Halo Mass and Redshift with DESI DR2 and ACT DR6: Part I. Luminous Red Galaxies, arXiv e-prints (2026), arXiv:2604.19744 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2026

  36. [36]

    Precision Kinematic Sunyaev--Zel'dovich Measurements Across Halo Mass and Redshift with DESI DR2 and ACT DR6: Part II. Bright Galaxy Survey and Emission-Line Galaxies

    B. Hadzhiyskaet al., Precision Kinematic Sunyaev–Zel’dovich Measurements Across Halo Mass and Redshift with DESI DR2 and ACT DR6: Part II. Bright Galaxy Survey and Emission-Line Galaxies, arXiv e-prints (2026), arXiv:2604.19745 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2026

  37. [37]

    M. S. Madhavacheril, N. Battaglia, K. M. Smith, and J. L. Sievers, Cosmology with the kinematic Sunyaev-Zeldovich effect: Breaking the optical depth degeneracy with fast radio bursts, Phys. Rev. D100, 103532 (2019), arXiv:1901.02418 [astro-ph.CO]

    work page arXiv 2019

  38. [38]

    Hadzhiyska, S

    B. Hadzhiyska, S. Ferraro, G. S. Farren, N. Sailer, and R. Zhou, Missing baryons recovered: A measurement of the gas fraction in galaxies and groups with the kinematic Sunyaev-Zel’dovich effect and CMB lensing, Phys. Rev. D112, 123507 (2025), arXiv:2507.14136 [astro-ph.CO]

    work page arXiv 2025

  39. [39]

    Overview of the DESI Legacy Imaging Surveys

    A. Deyet al., Overview of the DESI Legacy Imaging Surveys, AJ157, 168 (2019), arXiv:1804.08657 [astro-ph.IM]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  40. [40]

    Zhouet al., DESI luminous red galaxy samples for cross-correlations, JCAP11, 097, arXiv:2309.06443 [astro-ph.CO]

    R. Zhouet al., DESI luminous red galaxy samples for cross-correlations, JCAP11, 097, arXiv:2309.06443 [astro-ph.CO]

    work page arXiv

  41. [41]

    Whiteet al., Cosmological constraints from the tomographic cross-correlation of DESI Luminous Red Galaxies and Planck CMB lensing, JCAP02(02), 007, arXiv:2111.09898 [astro-ph.CO]

    M. Whiteet al., Cosmological constraints from the tomographic cross-correlation of DESI Luminous Red Galaxies and Planck CMB lensing, JCAP02(02), 007, arXiv:2111.09898 [astro-ph.CO]

    work page arXiv

  42. [42]

    Hadzhiyska, S

    B. Hadzhiyska, S. Ferraro,et al., Evidence for large baryonic feedback at low and intermediate redshifts from kine- matic Sunyaev-Zel’dovich observations with ACT and DESI photometric galaxies, Phys. Rev. D112, 083509 (2025), arXiv:2407.07152 [astro-ph.CO]

    work page arXiv 2025

  43. [43]

    Naesset al.(ACT), The Atacama Cosmology Telescope: DR6 maps, JCAP2025(11), 061, arXiv:2503.14451 [astro- ph.CO]

    S. Naesset al.(ACT), The Atacama Cosmology Telescope: DR6 maps, JCAP2025(11), 061, arXiv:2503.14451 [astro- ph.CO]

    work page arXiv

  44. [44]

    Planck Collaboration, Planck 2015 results. XLVIII. An overview of the GNILC method applied to polarized thermal dust emission, Astron. Astrophys.596, A109 (2016), arXiv:1605.09387 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  45. [45]

    Dark matter halo concentrations in the Wilkinson Microwave Anisotropy Probe year 5 cosmology

    A. R. Duffy, J. Schaye, S. T. Kay, and C. Dalla Vecchia, Dark matter halo concentrations in the Wilkinson Microwave Anisotropy Probe year 5 cosmology, Mon. Not. Roy. Astron. Soc.390, L64 (2008), [Erratum: Mon.Not.Roy.Astron.Soc. 23 415, L85 (2011)], arXiv:0804.2486 [astro-ph]. Appendix A: Normalization and surrogate fields In this appendix, we derive Eq. ...

    work page internal anchor Pith review Pith/arXiv arXiv 2008

  46. [46]

    In each Monte Carlo iteration, we simulate ˆv a(θ) using the surrogate method from Appendix A (see Eq. A7). 25 We construct anX-field by stacking simulated ˆv a values on real galaxy locations: Xsim a (θ) = X i∈gal Wi ˆvsim a (xi)δ 2(θ−θ i),(B1) and decompose into gradient/curl modesX G,sim ℓm ,X C,sim ℓm

    work page

  47. [47]

    (We checked that if we restrict to the non-DES subset of the SGC, then the value ofAdecreases to a value which is similar to the NGC.)

    When we compare the gradient auto power spectrumC GG,sim ℓ of the simulations to the data, we find that they differ by anℓ-independent constant (forℓ >∼ 2500): C GG,data ℓ =A 2 C GG,sim ℓ whereA=    1.18 NGC main sample 1.08 NGC extended sample 1.36 SGC main sample 1.61 SGC extended sample (B2) We attributeA >1 to imaging systematics in DESILS, w...

    work page

  48. [48]

    snapshot

    We correlateX G,sim ℓm with the ACT data (not an ACT simulation), obtainingC T G,sim ℓ . We bin the power spectrumC T G,sim ℓ inℓ(as in Eq. 22) obtaining a length-N b vectors b. We then estimate the binned power spectrum covarianceC bb′ from the simulations, assuming zero off-diagonal covariance: Cbb′ = Var(Asb)δ bb′ ,(B3) where the variance is taken over...

    work page

  49. [49]

    painting

    Toy tSZ model Nearly 100% of the tSZ signal comes from halos that are resolved by Quijote (M≥2×10 13 M⊙). Therefore, our toy tSZ model uses the Quijote halo catalog atz ∗ = 1, rather than the matter snapshot. We simulate they-map by “painting” an azimuthally symmetric profiley l(M) at each halo location: y(l) = X i∈halos yl(Mi)e −il·θi (C1) wherey l(M) is...

    work page

  50. [50]

    Therefore, our toy CIB model will use the matter snapshot of the Quijote simulations, not the halo catalog

    Toy CIB model Most of the CIB signal comes from halos that are not resolved by Quijote (in contrast to the preceding tSZ case). Therefore, our toy CIB model will use the matter snapshot of the Quijote simulations, not the halo catalog. We simply assume that CIB emission is proportional to the total matter field, via anl-dependent factor, which is chosen t...

    work page

  51. [51]

    moving lens signal

    Simplified moving-lens pipeline For each Quijote simulation, we run a simplified moving-lens pipeline which follows the steps from our main pipeline (§III), adapted to the snapshot geometry. Since the input to our pipeline is a galaxy field, we use the Quijote halo catalog (i.e. we assume one central galaxy per halo). The number densityn g = 5.9×10 −5 Mpc...

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