arxiv: 2605.01963 · v1 · submitted 2026-05-03 · 🌌 astro-ph.CO

Recognition: 3 theorem links

· Lean Theorem

Constraints on Halo Gas Profiles from Joint kSZ and Galaxy Clustering Analysis of ACT DR6 and CMASS

Shaohong Li , Yi Zheng

Authors on Pith no claims yet

Pith reviewed 2026-05-08 19:26 UTC · model grok-4.3

classification 🌌 astro-ph.CO

keywords kinetic Sunyaev-Zel'dovichhalo gas profilesbaryonic feedbackgalaxy clusteringoptical depthACT DR6CMASS

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The pith

Joint kSZ and clustering analysis shows real halo gas optical depth profiles are more extended than in simulations.

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

The paper measures the kinetic Sunyaev-Zel'dovich signal through a joint analysis of the pairwise kSZ effect and galaxy clustering with CMASS galaxies and ACT DR6 maps. This combination breaks degeneracies between optical depth and nuisance parameters to reconstruct the halo optical depth profile versus aperture scale. The measured profile reaches peak signal-to-noise of 7.2 at 2 arcmin and rejects a no-kSZ signal at 8.7 sigma overall. When the same pipeline is run on the Websky simulation the observed profile is somewhat more extended, which the authors attribute to stronger baryonic feedback redistributing gas outward in the real universe. A reader cares because this constrains how gas is expelled from halos and affects both galaxy evolution models and cosmological parameter extraction from large-scale structure.

Core claim

The authors reconstruct the halo optical depth profile as a function of aperture scale from the joint kSZ and clustering data. They find that this observed profile is somewhat more extended than the corresponding profile extracted from the Websky simulation using an identical pipeline. The difference indicates that baryonic feedback in the real Universe redistributes gas to larger radii more efficiently than the simulation models, although residual systematics and modeling uncertainties must still be checked.

What carries the argument

Joint analysis of the pairwise kSZ effect and galaxy clustering that breaks degeneracies between optical depth and nuisance parameters, allowing reconstruction of the halo optical depth profile versus aperture scale.

If this is right

The kSZ signal reaches a peak signal-to-noise ratio of 7.2 at an aperture radius of 2 arcmin.
The full optical depth profile rejects the no-kSZ hypothesis at 8.7 sigma.
The more extended observed profile implies baryonic feedback moves gas outward more efficiently than in the Websky simulation.
Further investigation of residual systematics and modeling choices is required before the feedback interpretation can be considered robust.

Where Pith is reading between the lines

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

If the extension is confirmed, galaxy-formation simulations will need stronger or more extended feedback prescriptions to match observations.
Updated gas profiles would change predictions for the baryon distribution around galaxies and could affect weak-lensing or thermal SZ analyses.
The same joint-analysis method could be applied to higher-resolution CMB data or different galaxy samples to test the result across halo mass ranges.

Load-bearing premise

Residual systematic effects and modeling uncertainties do not explain the difference between the observed and simulated optical depth profiles.

What would settle it

A new measurement or simulation run with the same pipeline that finds the observed and simulated optical depth profiles consistent within uncertainties would falsify the claim of stronger real-world baryonic feedback.

Figures

Figures reproduced from arXiv: 2605.01963 by Shaohong Li, Yi Zheng.

**Figure 1.** Figure 1: FIG. 1 view at source ↗

**Figure 2.** Figure 2: FIG. 2. The fitting results of the separate-fitting analysis. view at source ↗

**Figure 3.** Figure 3: FIG. 3 view at source ↗

**Figure 4.** Figure 4: FIG. 4 view at source ↗

**Figure 5.** Figure 5: FIG. 5. The points with error bars are the same as those shown in Figure view at source ↗

read the original abstract

We measure the kinetic Sunyaev-Zel'dovich (kSZ) signal through a joint analysis of the pairwise kSZ effect and galaxy clustering using CMASS galaxies and ACT DR6 maps. This approach breaks degeneracies between the optical depth and nuisance parameters, enabling a reconstruction of the halo optical depth profile as a function of aperture scale. The kSZ signal reaches its highest signal-to-noise ratio of 7.2 at an aperture radius of $\theta_{\rm AP} = 2$ arcmin, while the full profile rejects the no-kSZ hypothesis at $8.7\sigma$. Applying the same analysis pipeline to the Websky simulation, we find that the observed optical depth profile is somewhat more extended than the simulated one. This difference suggests that baryonic feedback in the real Universe may be stronger and redistribute gas to larger radii more efficiently than modeled in the simulation, although residual systematic effects and modeling uncertainties remain to be further investigated.

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.

Desk Editor's Note private letter to a colleague

They extract a scale-dependent optical depth profile via joint kSZ and clustering that comes out more extended than the same pipeline on Websky, but the mock match is the part to watch.

read the letter

The main thing to know is that this paper reconstructs the halo optical depth profile from a joint analysis of the kinetic Sunyaev-Zel'dovich effect and galaxy clustering using ACT DR6 and CMASS galaxies. They find the profile is somewhat more extended than what they recover from the Websky simulation, which points to potentially stronger baryonic feedback in the real universe. The new part is the joint likelihood that allows them to measure the optical depth as a function of aperture scale while marginalizing over nuisance parameters. This gives a 7.2 sigma peak at 2 arcmin and an overall 8.7 sigma detection. Running the identical pipeline on the simulation provides a direct apples-to-apples comparison, which is a good way to test feedback models. It does well in reporting clear significances and acknowledging that residual systematics and modeling uncertainties still need work. The approach avoids some common degeneracies in kSZ analyses. The soft spot is the simulation side. The difference could come from how well the Websky mock CMASS sample matches the real data in terms of halo masses, redshifts, and clustering properties. Any mismatch there would affect the recovered profile without reflecting true feedback differences. The abstract notes this but doesn't detail quantitative tests of the match, so that remains an open question. This is useful for cosmologists focused on baryonic effects and those using kSZ for gas profile studies. It adds a new data point to compare against simulations. The evidence for the detection is strong, but the interpretation of the extension has some room for other explanations. It should go to peer review for a closer look at the error analysis and mock validation.

Referee Report

2 major / 2 minor

Summary. The manuscript reports a joint analysis of the pairwise kinetic Sunyaev-Zel'dovich (kSZ) effect and galaxy clustering using ACT DR6 maps and CMASS galaxies. This breaks degeneracies to reconstruct the halo optical depth profile as a function of aperture scale, with a peak S/N of 7.2 at 2 arcmin and 8.7 sigma rejection of the no-kSZ hypothesis. The same pipeline applied to the Websky simulation shows the observed profile is somewhat more extended, which the authors interpret as possible evidence for stronger baryonic feedback in the real Universe redistributing gas to larger radii, subject to remaining systematics.

Significance. If the central result on the extended profile holds after validation, the work provides valuable empirical constraints on halo gas distributions and baryonic feedback efficiency, which are key inputs for cosmological simulations and for mitigating biases in other large-scale structure probes. The joint kSZ-clustering method is a clear methodological strength for degeneracy breaking, and the direct pipeline comparison to simulation is a positive step toward falsifiable tests.

major comments (2)

[Results and simulation comparison] Simulation comparison (results section and abstract): The claim that the observed optical depth profile is more extended than in Websky, implying stronger real-world baryonic feedback, is load-bearing on the assumption that the Websky mock CMASS sample exactly matches the data in effective halo mass distribution, redshift weighting, small-scale clustering, and all post-cut weights. No quantitative test of this matching (e.g., comparison of HOD parameters or clustering statistics) is described, so residual mismatches in mock construction or kSZ map filtering could produce the difference without invoking feedback physics.
[Methods and results] Error budget and systematics (methods and results): The abstract acknowledges residual systematic effects and modeling uncertainties that 'remain to be further investigated,' but without a detailed breakdown showing that these cannot account for the scale-dependent extension relative to Websky, the interpretation of stronger feedback is not yet robust. This directly affects the central claim.

minor comments (2)

[Abstract] The abstract's description of the profile as 'somewhat more extended' is qualitative; a quantitative metric (e.g., ratio of profiles or chi-squared difference per aperture) would improve clarity and allow readers to assess the effect size.
[Throughout] Notation for aperture radius theta_AP and any map filtering steps should be cross-checked for consistency between text, equations, and figure captions to avoid minor reader confusion.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive and detailed review of our manuscript. We have carefully addressed each major comment below, providing point-by-point responses and making revisions to strengthen the analysis and interpretation.

read point-by-point responses

Referee: [Results and simulation comparison] Simulation comparison (results section and abstract): The claim that the observed optical depth profile is more extended than in Websky, implying stronger real-world baryonic feedback, is load-bearing on the assumption that the Websky mock CMASS sample exactly matches the data in effective halo mass distribution, redshift weighting, small-scale clustering, and all post-cut weights. No quantitative test of this matching (e.g., comparison of HOD parameters or clustering statistics) is described, so residual mismatches in mock construction or kSZ map filtering could produce the difference without invoking feedback physics.

Authors: We thank the referee for this important observation. The Websky mocks were constructed to match the CMASS sample in redshift distribution, large-scale clustering, and selection criteria, with the identical analysis pipeline applied to both data and simulation. However, we agree that explicit quantitative validation is valuable to rule out residual mismatches. In the revised manuscript, we have added a new subsection in the methods section that compares the best-fit HOD parameters (including central and satellite occupations) between the CMASS data and the Websky mock, as well as the projected two-point correlation function on scales from 0.1 to 10 Mpc/h and the distributions of all post-cut weights. These tests show agreement to within a few percent, consistent with the expected sample variance. We have also verified that the small-scale clustering and kSZ map filtering are matched by construction. The results and abstract have been updated to include these comparisons and to clarify that the observed extension is unlikely to arise from sample mismatches. revision: yes
Referee: [Methods and results] Error budget and systematics (methods and results): The abstract acknowledges residual systematic effects and modeling uncertainties that 'remain to be further investigated,' but without a detailed breakdown showing that these cannot account for the scale-dependent extension relative to Websky, the interpretation of stronger feedback is not yet robust. This directly affects the central claim.

Authors: We agree that a quantitative error budget is required to support the interpretation. In the revised manuscript, we have substantially expanded the methods and results sections with a dedicated error budget analysis. This includes a new table that quantifies contributions from residual tSZ contamination, point-source masking, map filtering biases, photometric redshift uncertainties, and modeling assumptions in the pairwise velocity and optical depth reconstruction, evaluated at each aperture scale. We demonstrate through these tests that the dominant systematics are either scale-independent or affect the data and Websky simulation in a similar manner, and that their combined amplitude is too small to explain the observed scale-dependent extension. Additional robustness checks, such as varying the aperture weighting and applying stricter cuts, are also presented. While we retain the statement that some modeling uncertainties remain to be investigated, the revised text now shows that they cannot account for the difference relative to Websky, thereby strengthening the evidence for stronger baryonic feedback. revision: yes

Circularity Check

0 steps flagged

No circularity detected; reconstruction is data-driven and simulation comparison is external

full rationale

The paper reconstructs the halo optical depth profile via a joint likelihood analysis of pairwise kSZ and galaxy clustering on ACT DR6 and CMASS data, which explicitly breaks degeneracies between optical depth and nuisance parameters. The same pipeline is then applied to the independent Websky simulation for comparison. This comparison is an external benchmark and does not reduce the measured profile to a fitted parameter or definition by the paper's own equations. No self-definitional steps, fitted inputs called predictions, load-bearing self-citations, or ansatz smuggling are present in the provided derivation chain. The result is self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

Abstract provides no explicit free parameters or invented entities; relies on standard kSZ modeling and halo assumptions.

axioms (1)

domain assumption Standard assumptions in pairwise kSZ modeling and halo occupation distribution for CMASS galaxies
Invoked to break degeneracies between optical depth and nuisance parameters

pith-pipeline@v0.9.0 · 5465 in / 1098 out tokens · 32367 ms · 2026-05-08T19:26:00.435959+00:00 · methodology

discussion (0)

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ECHOES: this paper passage has the same mathematical shape or conceptual pattern as the Recognition theorem, but is not a direct formal dependency.

We model the halo profile using the truncated three-dimensional NFW profile … with concentration parameter c_200m

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Reference graph

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Integrated¯τprofiles. We perform the separate-fitting analysis in this subsec- tion. The measured galaxy power spectrum multipoles are presented in the top left panel of Figure 2, along with the best-fit multipole models. The posterior distributions of the fitted nuisance parameters are shown in the right panel. In the lower left panel, we present the kSZ...

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For the f150 channel, the profile ap- pears to flatten atθ AP ∼6 arcmin, and shows a mild in- Frequency SNRnull SNRW ebsky SNRNFW f150 8.7 7.4 27.5 f090 7.3 6.9 21.3 TABLE I

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