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arxiv: 2604.04867 · v1 · submitted 2026-04-06 · 🌌 astro-ph.CO

Recognition: no theorem link

Measurement of the galaxy-velocity power spectrum of DESI tracers with the kinematic Sunyaev-Zeldovich effect using DESI DR2 and ACT DR6

A. Cuceu, A. de la Macorra, A. Font-Ribera, A. Kremin, A. Meisner, B. A. Weaver, B. Dey, C. Howlett, C. Y\`eche, D. Bianchi, D. Brooks, D. Huterer, D. Kirkby, D. Schlegel, D. Sprayberry, Edmond Chaussidon, E. Gazta\~naga, E. Sanchez, F. Prada, G. Gutierrez, G. Rossi, G. Tarl\'e, H. K. Herrera-Alcantar, H. Seo, I. P\'erez-R\`afols, J. Aguilar, J. A. Newman, J. E. Forero-Romero, J. Guy, J. Silber, Kendrick Smith, K. Honscheid, L. Le Guillou, L. Samushia, M. Ishak, M. Landriau, M. Manera, M. Schubnell, N. Palanque-Delabrouille, O. Lahav, P. Doel, R. Joyce, R. Miquel, R. Zhou, S. Ahlen, Selim C. Hotinli, S. Gontcho A Gontcho, Simone Ferraro, S. Nadathur, T. Claybaugh, W. J. Percival, Xinyi Chen

Pith reviewed 2026-05-10 19:35 UTC · model grok-4.3

classification 🌌 astro-ph.CO
keywords kSZ effectDESI surveyACT CMBvelocity reconstructionprimordial non-Gaussianitylarge-scale structuregalaxy clusteringCMB cross-correlations
0
0 comments X

The pith

DESI and ACT data detect galaxy-velocity correlations via the kSZ effect at up to 17 sigma and set the tightest velocity-field limit on local primordial non-Gaussianity.

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

The paper shows how the kinematic Sunyaev-Zeldovich effect in CMB temperature maps can be paired with spectroscopic galaxy catalogs to reconstruct the radial velocity field of matter. Cross-correlating these velocities with positions of luminous red galaxies, emission-line galaxies, and quasars from DESI yields detections at 17.0, 8.3, and 6.8 sigma respectively. The authors also report the first velocity-velocity correlation and the highest cumulative kSZ significance to date at 20.8 sigma. These measurements produce a constraint on local primordial non-Gaussianity of f_NL^loc equal to 15.9 with uncertainties around 34 at 68 percent . The velocity-based observables display lower noise than galaxy auto-correlations on the largest scales, making them useful for future large-scale structure analyses.

Core claim

Joint analysis of ACT DR6 CMB maps and DESI DR2 spectroscopic tracers reconstructs the radial velocity field via the kSZ effect. The velocity-galaxy cross-correlation is detected at 17.0 sigma for LRGs, 8.3 sigma for ELGs, and 6.8 sigma for QSOs, together with a 3.1 sigma velocity-velocity correlation for LRGs. The cumulative kSZ detection reaches 20.8 sigma. The observed signal amplitude lies below the prediction of the fiducial halo model and Battaglia electron profile. Combining the new observables gives f_NL^loc = 15.9 with errors -34.4 and +34.6 at 68 percent .

What carries the argument

The kinematic Sunyaev-Zeldovich effect, which shifts CMB temperature in proportion to the line-of-sight velocity of ionized gas, used to form cross-power spectra between reconstructed velocities and galaxy overdensities.

Load-bearing premise

Foreground contamination is modeled reliably with negligible impact on the measured correlations, and the Battaglia electron profile with the fiducial halo model correctly accounts for the lower observed kSZ amplitude.

What would settle it

A higher-precision measurement showing the kSZ amplitude matching the fiducial model prediction rather than remaining lower, or a value of f_NL^loc lying well outside the current error range around 15.9.

Figures

Figures reproduced from arXiv: 2604.04867 by A. Cuceu, A. de la Macorra, A. Font-Ribera, A. Kremin, A. Meisner, B. A. Weaver, B. Dey, C. Howlett, C. Y\`eche, D. Bianchi, D. Brooks, D. Huterer, D. Kirkby, D. Schlegel, D. Sprayberry, Edmond Chaussidon, E. Gazta\~naga, E. Sanchez, F. Prada, G. Gutierrez, G. Rossi, G. Tarl\'e, H. K. Herrera-Alcantar, H. Seo, I. P\'erez-R\`afols, J. Aguilar, J. A. Newman, J. E. Forero-Romero, J. Guy, J. Silber, Kendrick Smith, K. Honscheid, L. Le Guillou, L. Samushia, M. Ishak, M. Landriau, M. Manera, M. Schubnell, N. Palanque-Delabrouille, O. Lahav, P. Doel, R. Joyce, R. Miquel, R. Zhou, S. Ahlen, Selim C. Hotinli, S. Gontcho A Gontcho, Simone Ferraro, S. Nadathur, T. Claybaugh, W. J. Percival, Xinyi Chen.

Figure 2
Figure 2. Figure 2: FIG. 1. Angular density distribution of DESI DR2 LRGs before correction for observational completeness. The bluer region corresponds to area that are not fully complete. We show only the area common to DESI and ACT DR6. The nominal DESI survey (including its extension) will cover the entire blue shaded area, while the gray shaded region indicates the ACT DR6 mask used in the analysis as described in the te… view at source ↗
Figure 1
Figure 1. Figure 1: FIG. 1. Angular density distribution of DESI DR2 LRGs [PITH_FULL_IMAGE:figures/full_fig_p010_1.png] view at source ↗
Figure 3
Figure 3. Figure 3: FIG. 3. Monopole of the LRG galaxy-velocity power spectrum ( [PITH_FULL_IMAGE:figures/full_fig_p012_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: FIG. 4. Residuals between the galaxy-velocity dipoles with [PITH_FULL_IMAGE:figures/full_fig_p013_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: FIG. 5. Blue points are the data and red dashed lines are the best fit that is given in [PITH_FULL_IMAGE:figures/full_fig_p014_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: FIG. 6. Posteriors obtained with LRG [PITH_FULL_IMAGE:figures/full_fig_p015_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: FIG. 7. Comparison of the posteriors obtained with [PITH_FULL_IMAGE:figures/full_fig_p015_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: FIG. 8. Evolution of the signal-to-noise ratio as a function of [PITH_FULL_IMAGE:figures/full_fig_p016_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: FIG. 9. Similar than [PITH_FULL_IMAGE:figures/full_fig_p017_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: FIG. 10. Posteriors obtained from the dipole of the ELG (left) and QSO (right) galaxy-velocity power spectrum. The two [PITH_FULL_IMAGE:figures/full_fig_p018_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: FIG. 11 [PITH_FULL_IMAGE:figures/full_fig_p018_11.png] view at source ↗
Figure 12
Figure 12. Figure 12: FIG. 12. Linear matter power spectrum at [PITH_FULL_IMAGE:figures/full_fig_p020_12.png] view at source ↗
Figure 13
Figure 13. Figure 13: FIG. 13. Comparison between the NGC (blue) and SGC (orange) dipole of galaxy-velocity power spectrum for the LRG, ELG [PITH_FULL_IMAGE:figures/full_fig_p027_13.png] view at source ↗
Figure 14
Figure 14. Figure 14: FIG. 14. Posterior comparison for the LRG sample between [PITH_FULL_IMAGE:figures/full_fig_p028_14.png] view at source ↗
Figure 16
Figure 16. Figure 16: FIG. 16. Comparison between the posteriors from the dipole [PITH_FULL_IMAGE:figures/full_fig_p028_16.png] view at source ↗
Figure 17
Figure 17. Figure 17: FIG. 17. Similar to [PITH_FULL_IMAGE:figures/full_fig_p029_17.png] view at source ↗
Figure 18
Figure 18. Figure 18: FIG. 18. Correlation matrix for the LRG joint analysis. The observables are stacking in the following order: [PITH_FULL_IMAGE:figures/full_fig_p031_18.png] view at source ↗
Figure 19
Figure 19. Figure 19: FIG. 19. Full posteriors for the combined fit of the LRG, ELG, and QSO. The gray dashed lines correspond to the fiducial [PITH_FULL_IMAGE:figures/full_fig_p032_19.png] view at source ↗
read the original abstract

Joint analyses of high-resolution CMB temperature maps with galaxy surveys provide a unique way to reconstruct the radial velocity field of the underlying matter distribution via the kinematic Sunyaev-Zeldovich (kSZ) effect. Using data from the Atacama Cosmology Telescope (ACT) DR6 and the Dark Energy Spectroscopic Instrument (DESI) DR2, we present radial velocity reconstructions for luminous red galaxies (LRGs), emission-line galaxies (ELGs), and quasars (QSOs). Leveraging the spectroscopic data, we are able to reliably model the foreground contamination and report a negligible impact on our main observables. We detect the velocity-galaxy cross-correlation at $17.0\sigma$ for LRGs, and for the first time, at $8.3\sigma$ for ELGs and $6.8\sigma$ for QSOs. We further report the first detection of the velocity-velocity correlation using LRGs at $3.1\sigma$, as well as the highest cumulative detection of the kSZ effect to date at $20.8 \sigma$. Similarly to previous results, we find a lower amplitude of the kSZ signal compared to our fiducial halo model prediction and electron profile assuming a Battaglia profile. Combining these new observables, we obtain constraints on local-type primordial non-Gaussianity (PNG): $f_{\rm NL}^{\rm loc} = 15.9_{-34.4}^{+34.6}$ at 68\% confidence, which represents the tightest constraint to date derived from the velocity field. The measurements presented here already exhibit lower noise on a per-mode basis than the galaxy auto-correlation on the largest scales, $k<0.004~\rm{Mpc^{-1}}$, highlighting the key role these observables will play in the context of future CMB experiments such as the Simons Observatory.

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

1 major / 0 minor

Summary. The manuscript reports measurements of the galaxy-velocity cross-power spectrum via the kinematic Sunyaev-Zeldovich effect using ACT DR6 CMB maps and DESI DR2 spectroscopic tracers (LRGs, ELGs, QSOs). It claims detections at 17.0σ (LRG velocity-galaxy), 8.3σ (ELG), and 6.8σ (QSO), a 3.1σ velocity-velocity correlation with LRGs, and a cumulative 20.8σ kSZ detection—the highest to date. Foreground contamination is modeled as having negligible impact, a lower kSZ amplitude than the fiducial Battaglia electron profile plus halo model is noted (consistent with prior work), and these observables are combined to constrain local primordial non-Gaussianity at f_NL^loc = 15.9_{-34.4}^{+34.6} (68% CL), the tightest from the velocity field, while highlighting lower per-mode noise than galaxy auto-correlations at k < 0.004 Mpc^{-1}.

Significance. If the modeling holds, the result delivers the first ELG and QSO kSZ detections, the highest cumulative kSZ significance, and the tightest velocity-field f_NL^loc constraint to date. The explicit foreground assessment and high reported significances bolster the detections, while the per-mode noise comparison underscores the observables' future value for experiments such as Simons Observatory. Machine-checked elements are absent, but the multi-tracer approach and explicit negligible-foreground statement are strengths.

major comments (1)
  1. [Abstract and results discussion of amplitude] Abstract and results discussion of amplitude: the lower kSZ amplitude relative to the Battaglia profile plus fiducial halo model is noted without detailed resolution or quantitative propagation into the f_NL^loc posterior. Because the PNG constraint combines the cross-spectra (whose normalization enters the model), this mismatch risks mis-calibrating the scale-dependent signature; the manuscript should demonstrate robustness, e.g., by showing the f_NL posterior with and without amplitude rescaling or by marginalizing over profile parameters.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their careful reading of the manuscript and for the positive assessment of the reported detections and their potential for future experiments. We address the single major comment below and will incorporate the requested robustness test in the revised version.

read point-by-point responses

  1. Referee: Abstract and results discussion of amplitude: the lower kSZ amplitude relative to the Battaglia profile plus fiducial halo model is noted without detailed resolution or quantitative propagation into the f_NL^loc posterior. Because the PNG constraint combines the cross-spectra (whose normalization enters the model), this mismatch risks mis-calibrating the scale-dependent signature; the manuscript should demonstrate robustness, e.g., by showing the f_NL posterior with and without amplitude rescaling or by marginalizing over profile parameters.

    Authors: We agree that explicitly demonstrating robustness of the f_NL^loc posterior to the overall kSZ amplitude is valuable. The lower amplitude relative to the fiducial Battaglia profile plus halo model is already noted in the manuscript and is consistent with previous kSZ measurements. In the model for the galaxy-velocity cross-spectra, an overall amplitude parameter is included that absorbs the normalization of the kSZ signal (including any profile mismatch). The f_NL^loc constraint is driven by the scale-dependent shape at the largest scales rather than the overall normalization. To directly address the concern, we have performed an additional test in which the model amplitude is rescaled to match the observed kSZ signal before refitting for f_NL^loc; the resulting posterior is statistically consistent with the fiducial result. We will add a description of this test, together with a comparison of the two posteriors, to the revised manuscript. revision: yes

Circularity Check

0 steps flagged

No circularity: measurements and f_NL constraint are independent of model inputs

full rationale

The paper reports direct detections of velocity-galaxy cross-spectra (17.0σ LRG, 8.3σ ELG, 6.8σ QSO) and velocity-velocity (3.1σ) from ACT+DESI data, then combines them to constrain f_NL^loc. No quoted step defines a prediction via a fit to the same data, renames a known result, or relies on a self-citation chain for the central claim. The noted lower amplitude vs. Battaglia+fiducial model is an external comparison, not a self-definitional input to the f_NL posterior. The derivation remains self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

1 free parameters · 2 axioms · 0 invented entities

The central results rest on the assumption that the kSZ velocity reconstruction is unbiased after foreground modeling and that the Battaglia profile plus fiducial halo model provide a fair comparison point. No new particles or forces are introduced.

free parameters (1)
  • f_NL^loc
    Fitted parameter whose posterior is reported from the combined velocity observables.
axioms (2)
  • domain assumption Foreground contamination can be reliably modeled from spectroscopic data with negligible residual impact on the kSZ observables.
    Stated explicitly in the abstract as enabling the reported detections.
  • domain assumption The Battaglia electron pressure profile and fiducial halo model are appropriate benchmarks for the observed kSZ amplitude.
    Used to note that the measured amplitude is lower than predicted.

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discussion (0)

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Forward citations

Cited by 2 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score.

  1. Backlighting the Cosmic Web with Fast Radio Bursts: An Anthology of Dispersion Measure Cross-Correlations with Large-Scale Structure and Baryon Tracers

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    FRB DMs correlate at 2.6-5 sigma with galaxies, weak lensing, CIB, CMB lensing, tSZ, X-ray clusters, SXRB and radio continuum, consistent with moderate feedback models while ruling out weak feedback at 3.5 sigma via SXRB-DM.

  2. New constraints on primordial non-Gaussianity from large-scale cross-correlations of CMB lensing and the cosmic infrared background

    astro-ph.CO 2026-05 unverdicted novelty 4.0

    Dust-cleaned CIB and CMB lensing cross-correlations yield f_NL^local = 43 ± 23, tightening constraints on local primordial non-Gaussianity.

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