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SPT-3G's arcminute spectra fix thermal SZ power at 4.91±0.37 μK² and kinematic SZ power at 1.75±0.86 μK² at ℓ=3000, and set a 95% limit of Δz_re<3.8 on how long reionization lasted.

Reviewed by Pith at T0; open to challenge. T0 means a machine referee read the full paper against a public rubric. the ladder, T0–T4 →

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2026-08-03 07:18 UTC pith:QB3MIXWN

load-bearing objection The SPT-3G bandpowers are a real, carefully made measurement; the headline SZ amplitudes are honestly labeled but strongly model-dependent, so read the numbers with the caveats attached. the 4 major comments →

arxiv 2601.20551 v2 pith:QB3MIXWN submitted 2026-01-28 astro-ph.CO

SPT-3G D1: A Measurement of Secondary Cosmic Microwave Background Anisotropy Power

P. Chaubal , N. Huang , C. L. Reichardt , A. J. Anderson , B. Ansarinejad , M. Archipley , L. Balkenhol , D. R. Barron
show 99 more authors
K. Benabed A. N. Bender B. A. Benson F. Bianchini L. E. Bleem S. Bocquet F. R. Bouchet L. Bryant E. Camphuis M. G. Campitiello J. E. Carlstrom J. Carron 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 A. Doussot D. Dutcher W. Everett C. Feng K. R. Ferguson N. C. Ferree K. Fichman A. Foster S. Galli A. E. Gambrel A. K. Gao R. W. Gardner F. Ge N. Goeckner-Wald R. Gualtieri F. Guidi S. Guns N. W. Halverson E. Hivon A. Y. Q. Ho G. P. Holder W. L. Holzapfel J. C. Hood A. Hryciuk T. Jhaveri F. K\'eruzor\'e A. R. Khalife L. Knox M. Korman 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 G. I. Noble Y. Omori A. Ouellette Z. Pan P. Paschos K. A. Phadke A. W. Pollak K. Prabhu W. Quan S. Raghunathan M. Rahimi A. Rahlin M. Rouble J. E. Ruhl E. Schiappucci A. C. Silva Oliveira A. Simpson J. A. Sobrin A. A. Stark J. Stephen C. Tandoi B. Thorne C. Trendafilova C. Umilta J. D. Vieira A. G. Vieregg A. Vitrier Y. Wan N. Whitehorn W. L. K. Wu M. R. Young J. A. Zebrowski
This is my paper
classification astro-ph.CO
keywords secondary CMB anisotropiesSunyaev-Zel'dovich effectcosmic infrared backgroundangular power spectraepoch of reionizationSPT-3GtSZ-CIB correlationmillimeter-wave observations
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

Using two years of SPT-3G observations of a 1646 square-degree patch, this paper delivers the most precise millimeter-wave power spectra yet measured for the secondary cosmic microwave background at arcminute scales, spanning angular multipoles 1700 to 11,000 in six frequency cross-spectra (95, 150, and 220 GHz). These spectra sharpen previous measurements of the thermal and kinematic Sunyaev-Zel'dovich effects—imprints left on the CMB by hot and moving electrons in cosmic structures—by factors up to roughly eight in uncertainty. The paper shows that how much power is assigned to the thermal versus kinematic SZ effect depends strongly on the assumed spatial correlation between the SZ signal and the cosmic infrared background; fixed simulation templates shift the answers by up to ~5σ, so the authors adopt flexible spline-based models. In that fiducial model, the thermal SZ power at ℓ=3000 and 143 GHz is 4.91±0.37 μK² and the kinematic SZ power is 1.75±0.86 μK², implying a 95% upper limit of Δz_re<3.8 on the duration of reionization (25–75% ionization). The result matters because it turns arcminute-scale secondary anisotropies into a precision probe of cluster physics and reionization timing, while exposing the foreground-model assumptions that now dominate the error budget.

Core claim

The paper's claim is that the arcminute-scale millimeter sky can now be measured, rather than estimated: six auto- and cross-frequency power spectra with signal-to-noise high enough that the data internally constrain the angular shapes of the tSZ, kSZ, and CIB contributions. At ℓ≳3000, the new SPT-3G bandpowers are the most precise in all three observing bands, with uncertainties reduced by up to a factor of 8 relative to earlier SPT measurements and by roughly a factor of 2–3 relative to recent measurements at these scales. The headline constraints, from a model that leaves the angular dependencies of the SZ and CIB spectra free (the 'free CIB, ℓ^α SZ' model), are D_tSZ=4.91±0.37 μK² and D_

What carries the argument

The load-bearing piece is a pseudo-Cℓ estimator that forms cross-spectra between 200 temporally split map bundles in each of the three frequency bands, correcting for mode-mixing, transfer functions, beams, and calibration. On top of that sits a multi-component foreground model whose pivotal element is the tSZ–CIB correlation term, D^{tSZ–CIB}_ℓ = −ξ(ℓ)(√(D^{CIB,ν1}_ℓ D^{tSZ,ν2}_ℓ)+√(D^{CIB,ν2}_ℓ D^{tSZ,ν1}_ℓ)). The correlation function ξ(ℓ) parameterizes how much of the dusty-galaxy background and the hot-gas signal are spatially aligned; it directly controls the tSZ/kSZ split. The paper treats ξ(ℓ) either as a rescaled simulation template or as a monotonic cubic spline with eight free node

Load-bearing premise

The decomposition of the measured power into thermal and kinematic SZ amplitudes rests on the assumption that the true spatial correlation between the cosmic infrared background and the thermal SZ signal, ξ(ℓ), is captured by the models considered—either a rescaled simulation template or a non-negative spline—and if that assumption fails, the headline SZ values and the reionization limit move by several sigma.

What would settle it

Measure the tSZ–CIB correlation directly, without assuming a template: cross-correlate a tSZ-selected cluster map or a CMB lensing map with a CIB map at overlapping frequencies and compare the recovered ξ(ℓ) to the rising and falling forms used here. If an independent ξ(ℓ) rises with ℓ rather than falling with ℓ as the splines recover, then the fiducial D_tSZ=4.91 and D_kSZ=1.75 μK² split—and the Δz_re<3.8 limit built on it—would need revision. A complementary check is a direct kSZ measurement, such as pairwise kSZ stacking of galaxies or the kSZ trispectrum, which bypasses the tSZ–CIB decompo

Watch this falsifier — get emailed when new claim-graph text bears on it.

If this is right

  • At ℓ≳3000, these six spectra and their likelihood become the new reference for arcminute-scale CMB secondary-anisotropy constraints, reducing the uncertainty on the measured sky power by up to a factor of 8 relative to earlier SPT data.
  • The template-dependence result means future analyses at this sensitivity cannot rely on a single simulation-based tSZ–CIB template; marginalizing over the correlation shape, or measuring it, becomes part of the standard pipeline.
  • The kSZ measurement, combined with a homogeneous-kSZ subtraction, tightens the allowed duration of reionization to Δz_re<3.8 (25–75%) at 95% confidence, complementing independent kSZ trispectrum limits.
  • The data directly constrain the angular shape of tSZ power, which peaks near ℓ≈3000–4500 depending on the model, providing a test of cluster gas physics independent of cluster counts.
  • The CIB clustering and Poisson amplitudes at 150 and 220 GHz are stable across model choices (agreeing within ~1σ at ℓ=3000), pinning down the dusty-galaxy background at these frequencies.

Where Pith is reading between the lines

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

  • If the recovered tSZ–CIB correlation, which falls with ℓ, is confirmed by independent data, then the older rising-template form used in previous SPT analyses would bias kSZ high and tSZ low; this is a testable prediction for hydrodynamic simulations of the correlation.
  • The borderline fit quality (PTE ~6–9% even for the flexible models, ~0.6% for the template fits) hints that either the covariance/beam errors are slightly underestimated or a minor component—such as CO line emission or clustered radio sources—remains unmodeled; the full-depth survey and refined beam papers should distinguish these.
  • The reionization bound uses only the ℓ=3000 kSZ point; fitting the whole measured kSZ spectrum to joint homogeneous+patchy models, with the homogeneous level free, would use more of the data and could either tighten the limit or reveal the homogeneous-kSZ assumption as the controlling uncertainty.
  • Because the tSZ and kSZ amplitudes in this paper are set by the ξ(ℓ) prior, independent measurements of the tSZ–CIB cross-spectrum—for instance by stacking CIB emission on SZ-selected clusters—would directly test the central decomposition and could be made with maps already in hand.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit.

Referee Report

4 major / 5 minor

Summary. This paper presents SPT-3G D1 temperature bandpowers from 2019–2020 observations of 1646 deg^2 in the angular range 1700 ≤ ℓ ≤ 11,000. The analysis follows a validated pseudo-Cℓ pipeline with cross-spectra between temporal bundles, transfer-function simulations, conditioned covariance estimation, and null tests; the left-minus-right excess at 95 GHz is traced to detector time constants and shown to disappear after deconvolution. The paper then fits models for primary CMB, tSZ, kSZ, CIB, radio galaxies, and cirrus, using both simulation-based templates and flexible monotonic-spline models for the SZ shapes, CIB clustering, and tSZ–CIB correlation. The headline free-CIB + ℓ^α SZ fit gives D_tSZ(3000,143 GHz) = 4.91 ± 0.37 μK^2 and D_kSZ(3000) = 1.75 ± 0.86 μK^2, and a 95% upper limit Δz_re^50 < 3.8 derived by subtracting an external homogeneous kSZ model and inverting published fitting formulas. The paper emphasizes that SZ power inferences are sensitive to the tSZ–CIB correlation model and to the assumed angular dependence of the SZ spectra.

Significance. If the measurement is sound, these bandpowers are the most precise millimeter-wave secondary-anisotropy measurements to date at ℓ ≳ 3000, with a factor-of-several improvement over previous SPT data and ACT DR6 at high ℓ. The public release of bandpowers, covariance, window functions, and likelihood code is a substantial community resource. The paper also conducts a careful systematics program, including a convincing explanation of the 95 GHz left-minus-right null-test excess. However, the parameter-level claims are heavily model-dependent: the central tSZ–CIB correlation model is not validated with end-to-end simulations, and template choices shift D_kSZ by an amount far larger than the quoted statistical error. The reionization limit additionally depends on an external homogeneous kSZ subtraction. These issues limit the strength of the headline SZ and reionization constraints, although not of the bandpower measurement itself.

major comments (4)
  1. [§6.6, §8.2] The free-CIB model uses an eight-parameter monotonic cubic spline for ξ(ℓ) with ξ ≥ 0 and endpoints pinned to zero. The headline values D_kSZ = 1.75 ± 0.86 μK^2 and Δz_re < 3.8 are conditioned on this spline, yet the paper presents no end-to-end injection-recovery test showing that the spline can reconstruct an input ξ(ℓ) without biasing the SZ amplitudes. The constraint is weak (ξ3000 = 0.036 ± 0.021) and the recovered falling shape conflicts with the rising Z12 template. The paper itself shows that swapping the tSZ–CIB template changes D_kSZ from 1.89 to 3.96 μK^2 (§8.1), i.e. by much more than the quoted error. Because the tSZ–CIB correlation is degenerate with kSZ in several frequency pairs, a biased spline recovery directly biases the headline D_kSZ and the derived reionization limit. Please add injection-recovery simulations for the spline parameterization, or, if that is not possi
  2. [§8.1] The same-model comparison with R21 is in strong tension. The Introduction quotes R21 as finding D_tSZ = 3.42 ± 0.54 μK^2 and D_kSZ = 3.0 ± 1.0 μK^2, while the text reports that using the same model as R21 on the new data gives D_tSZ = 5.47 ± 0.20 μK^2 and D_kSZ < 1.4 μK^2. This is a roughly 3.5σ shift in D_tSZ and a substantial downward shift in D_kSZ, and the paper does not comment on it. The discrepancy may be due to different sky coverage, masking thresholds, or band centers, but that needs to be stated explicitly and checked. As written, readers cannot tell whether this reflects a genuine improvement over R21 or an inconsistency in the model implementation or data processing.
  3. [§8.1.4] The reionization constraint subtracts an external homogeneous kSZ prediction (Eq. 8.1) from the measured total kSZ and then inverts external fitting formulas (Eqs. 8.2–8.3). No uncertainty is propagated for the homogeneous kSZ scaling or for the fitting formulas themselves, and the analysis fixes z_re to 7.68. At the Planck σ8 value the homogeneous prediction is 1.76 μK^2, which is twice the statistical error on D_kSZ; lowering σ8 from 0.812 to 0.77 changes the reported Δz_re limits by about 1. The abstract presents Δz_re < 3.8 without this conditionality. Please state in the abstract and conclusion that this limit is conditional on the assumed homogeneous kSZ model and external reionization fitting formulas, or provide a model-marginalized limit.
  4. [§7, Table 3] The fiducial free-CIB model has a borderline PTE of 8.8% (8.6% for free CIB+SZ), and the template fits have PTE 0.6%. The paper lists possible causes—beam uncertainty, transfer-function mis-estimation, or missing model components—but does not resolve the issue. Since the headline SZ and reionization numbers are taken from the borderline-PTE free-CIB model, this amplifies the concern in the first major comment. At minimum, the paper should quantify how the quoted parameter uncertainties change under the larger beam errors that would make the PTE acceptable, even if the authors believe those errors are over-estimates.
minor comments (5)
  1. [§7, Table 3] The text says the PTE for the two more flexible models is 'borderline at 6.0%', but Table 3 lists PTEs of 8.8% and 8.6%. Please reconcile.
  2. [Eq. (3.2)] The notation in Eq. (3.2) would benefit from explicit complex conjugation and clearer ℓ,m indices; as written, the product of spherical harmonic coefficients is ambiguous.
  3. [§8.2] The statement of 'evidence for a positive spatial correlation' is stronger than the free-CIB result supports: ξ3000 = 0.036 ± 0.021 is only a 1.7σ preference. Please soften the wording or show explicitly that the evidence is driven by the template-based fits.
  4. [§6.5] In the free-CIB model, Galactic cirrus is absorbed into the CIB term with the same modified blackbody SED. This is a reasonable approximation, but the potential impact on the 220 GHz bandpowers, where cirrus is relatively larger, should be mentioned in the text.
  5. [§8.1.4] The resampling to a uniform prior on Δz_re is described, but the original prior on D_kSZ used in the MCMC should be stated explicitly; a uniform prior on D_kSZ can affect the posterior weight of low Δz_re values even after resampling.

Circularity Check

0 steps flagged

No significant circularity: SZ amplitudes are fitted parameters, reionization limits are obtained through external model calibrations, and self-citations are not load-bearing.

full rationale

The paper's central outputs are measured bandpowers, not predictions derived from the model. The SZ amplitudes (D_tSZ, D_kSZ) are explicitly free parameters fitted to those bandpowers (Eqs. 6.1-6.6, 6.9-6.10), and the paper consistently describes them as constraints, not as first-principles predictions. The reionization duration limits are obtained by subtracting an external homogeneous-kSZ calibration (Eq. 8.1, from [46]) from the fitted kSZ power and then inverting external fitting formulas (Eqs. 8.2-8.3, from [46] and [47]). This is a model-dependent parameter translation, not a circular derivation: the data measurement is independent of the calibration formulas. Self-citations to prior SPT analyses (R21, Z12, companion SPT-3G papers) supply templates, map-making methods, and data provenance, but the headline claims are cross-checked against the Agora templates, flexible free-CIB spline fits, and external ACT DR6/Planck results, and the paper openly quantifies the template sensitivity (up to ~5 sigma). The potential fragility of the free-CIB spline reconstruction of the tSZ-CIB correlation is a modeling-systematic concern, not an instance of the derivation reducing to its inputs by construction. Therefore no specific circular step can be identified and the circularity score is 0.

Axiom & Free-Parameter Ledger

12 free parameters · 10 axioms · 0 invented entities

The measurement itself is self-contained (bandpowers are direct data products), but every scientific conclusion drawn from those bandpowers passes through a component-separation model with many fitted parameters — tSZ/kSZ amplitudes and shapes, CIB Poisson/clustering amplitudes and SED indices, radio galaxy parameters, and the tSZ-CIB correlation. The free-spline models push the parameter count to ~35 for the CIB+SZ case. These are honest costs of separation, not circular steps; the SZ amplitudes are fitted, not predicted. The paper's own sensitivity tests (swapping templates) show the answer depends on those model choices by up to 5σ. The reionization constraint adds external formulas (Eqs. 8.1–8.3) as axioms.

free parameters (12)
  • D_tSZ_3000 (tSZ power at ell=3000, 143 GHz) = 4.91 ± 0.37 μK^2 (free CIB + ℓ^α G15 SZ model); 4.28 ± 0.37 (Agora templates)
    Fitted amplitude scaling simulation tSZ template; central reported quantity.
  • α_tSZ (tSZ power-law exponent) = not stated numerically; template-dependent
    Added ℓ^α rescaling of tSZ template (Eq. 6.2); absorbs template-shape uncertainty.
  • D_kSZ_3000 (kSZ power at ell=3000) = 1.75 ± 0.86 μK^2 (free CIB ℓ^α); 3.96 ± 0.82 (Agora templates)
    Fitted amplitude of kSZ template.
  • α_kSZ (kSZ power-law exponent) = not stated numerically; fitted
    kSZ ℓ^α exponent (Eq. 6.5).
  • ξ3000 (tSZ-CIB correlation amplitude) = 0.036 ± 0.021 (free CIB ℓ^α); 0.091 ± 0.025 (Agora templates)
    Template amplitude or spline nodes for ξ(ℓ); strongly affects tSZ/kSZ split.
  • CIB Poisson amplitude D_CIB_pois,3000^150 = 6.42 ± 0.55 μK^2 (free CIB ℓ^α)
    Poisson CIB power at ell=3000, 150 GHz; free grey-body index β_P.
  • CIB clustering spline amplitudes f_CIB(ℓ) at 5 nodes = not individually tabulated
    Monotonic cubic spline nodes at ell=1800,3000,4200,6000,9000 (Eq. 6.8); 5 free params replacing 1-/2-halo templates.
  • β_C(ℓ) grey-body index nodes (3) = not tabulated
    Multipole-dependent CIB SED index via spline.
  • Free-SZ spline nodes: a_tSZ(ℓ) (7) and a_kSZ(ℓ) (7) = not tabulated
    Amplitudes at fixed ells defining tSZ/kSZ shapes in free CIB+SZ model.
  • Radio galaxy parameters: D_rg,3000^150, α_rg, σ²_rg = D_rg^150=1.24 ± 0.18 μK^2 (free CIB ℓ^α); α_rg, σ²_rg not reported
    Poisson radio power, spectral index and variance (Eq. 6.11); 3 free params.
  • Six ΛCDM parameters = Planck 2018 prior; posterior = prior
    Varied in MCMC with Planck prior; SPT-3G data do not shift them.
  • Cirrus amplitude (template fits) = prior-driven
    Cirrus template amplitude with prior from Planck cross-correlation; posterior prior-dominated.
axioms (10)
  • domain assumption LambdaCDM with Planck 2018 parameters provides the correct primary CMB power in this ell range
    §6.1, CosmoPower, Planck prior; used to separate CMB from SZ/foregrounds.
  • standard math Pseudo-Cell estimator with MASTER mode-coupling and simulation-based transfer function is unbiased
    §3, Hivon et al. 2002; standard in CMB.
  • domain assumption Shaw and Agora tSZ templates bracket the true tSZ power spectrum shape
    §6.2; the 5σ shifts between templates show the result depends on this.
  • domain assumption Shaw+Zahn composite kSZ template and Agora homogeneous template bracket true kSZ shape
    §6.3; kSZ template choice has smaller effect but still assumed.
  • domain assumption tSZ-CIB correlation ξ(ℓ) is real, ≥0, and its template (Z12 or Agora) or spline parameterization is adequate
    §6.6; drives SZ decomposition; is the weakest assumption.
  • domain assumption CIB 1-/2-halo template (Viero et al.) or free-spline shapes describe the CIB clustering power
    §6.4; CIB is the largest foreground at 150/220 GHz.
  • domain assumption Homogeneous kSZ power at ell=3000 follows D=1.65(σ8/0.8)^4.46 μK^2 (Eq. 8.1)
    §8.1.4; used to split measured kSZ into patchy and homogeneous.
  • domain assumption Patchy kSZ fitting formulas (Eqs. 8.2, 8.3) correctly map patchy kSZ power to reionization duration
    §8.1.4; from [46] and [47]; definitions of Δz differ between the two.
  • domain assumption Beam chromaticity model (physical model + frequency-independent sidelobes) is correct over ell range
    §3.4; beam uncertainty affects all bandpowers.
  • domain assumption Map filtering/time-constant smoothing is captured in the beam for all components
    §4; they proceed with non-deconvolved maps after null test.

pith-pipeline@v1.3.0-alltime-deepseek · 32592 in / 22326 out tokens · 228179 ms · 2026-08-03T07:18:32.801635+00:00 · methodology

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read the original abstract

We report new measurements of millimeter-wave temperature power spectra in the angular multipole range $1700 \le \ell \le 11,000$ (wavelengths $13^\prime \gtrsim \lambda \gtrsim 2^\prime$). We use two years of data in three observing bands centered near 95, 150, and 220 GHz from the SPT-3G receiver on the South Pole Telescope that cover a 1646 deg$^2$ region of the Southern sky. Using the measured power spectra, we present constraints on the thermal and kinematic Sunyaev-Zel'dovich (SZ) effects, radio galaxies, and cosmic infrared background (CIB). We find that inferred SZ powers are dependent on the detailed modeling of the thermal SZ-CIB correlation, and to a lesser extent on the assumed angular dependence of the SZ spectra. We report constraints for simulation-based model templates as well as fits where the angular dependencies of the SZ and CIB power spectra are allowed to vary. In the latter case at $\ell=3000$, we find thermal SZ power at 143 GHz of $D_{3000}^{\rm tSZ} = 4.91\pm0.37\, \mu{\rm K}^2$ and kinematic SZ power of $D_{3000}^{\rm kSZ} =1.75\pm0.86\, \mu{\rm K}^2$. We use the measured kinematic SZ power to estimate the duration of reionization, noting that the reionization inferences are sensitive to the model choices and assumed level of homogeneous kinematic SZ power from the late-time universe. We find a 95% limit on the duration from an ionization fraction of 25% to 75% of $\Delta^{50} z_{\rm re} <\,3.8$ based on a semi-analytic model, or a limit on the duration from an ionization fraction of 5% to 95% of $\Delta^{90} z_{\rm re} <\,6.1$ based on the AMBER simulations.

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Forward citations

Cited by 5 Pith papers

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

  1. Fireworks at Cosmic Dawn: relieving BAO-CMB tensions with the Pop III.1 Flash

    astro-ph.CO 2026-06 unverdicted novelty 6.0

    A Pop III.1-driven early ionization phase at z=20 yields τ=0.087 consistent with pkSZ and Lyα constraints, potentially resolving BAO-CMB tensions on neutrino mass.

  2. Discriminating Planck Reionisation Histories with the kSZ Effect

    astro-ph.CO 2026-05 unverdicted novelty 5.0

    kSZ angular power spectra separate early and late reionisation histories consistent with Planck constraints, with a future measurement at ℓ~2000 sufficient to discriminate and CMB data alone yielding 7.94<z_re<8.17.

  3. Discriminating Planck Reionisation Histories with the kSZ Effect

    astro-ph.CO 2026-05 conditional novelty 5.0

    Planck-allowed reionisation histories split into early and late classes whose kSZ spectra stay separable under modelling uncertainties, and a ~0.4 μK² measurement at ℓ~2000 would settle the choice.

  4. Discriminating Planck Reionisation Histories with the kSZ Effect

    astro-ph.CO 2026-05 unverdicted novelty 4.0

    Short and long reionisation histories consistent with Planck yield kSZ power spectra that remain separable despite uncertainties, requiring a sensitivity of ~0.4 μK² at ℓ~2000 to discriminate between the scenarios.

  5. Constraints on Phenomenological Amplitudes of CMB Anisotropy with Multi-Datasets

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    Lensing amplitude A_L deviates from 1 at up to 3.06 sigma in combined datasets while other phenomenological amplitudes remain consistent with Lambda CDM or are poorly constrained.

Reference graph

Works this paper leans on

55 extracted references · 48 linked inside Pith · cited by 3 Pith papers

  1. [1]

    Sunyaev and Y.B

    R.A. Sunyaev and Y.B. Zel’dovich,The Observations of Relic Radiation as a Test of the Nature of X-Ray Radiation from the Clusters of Galaxies,Comments on Astrophysics and Space Physics4(1972) 173

    1972

  2. [2]

    Sunyaev and Y

    R. Sunyaev and Y. Zel’dovich,Microwave background radiation as a probe of the contemporary structure and history of the universe,ARAA18(1980) 537

    1980

  3. [3]

    Gruzinov and W

    A. Gruzinov and W. Hu,Secondary Cosmic Microwave Background Anisotropies in a Universe Reionized in Patches,ApJ508(1998) 435 [arXiv:astro-ph/9803188]

    Pith/arXiv arXiv 1998

  4. [4]

    L. Knox, R. Scoccimarro and S. Dodelson,Impact of Inhomogeneous Reionization on Cosmic Microwave Background Anisotropy,Physical Review Letters81(1998) 2004 [arXiv:astro-ph/9805012]

    Pith/arXiv arXiv 1998

  5. [5]

    Shaw, D.H

    L.D. Shaw, D.H. Rudd and D. Nagai,Deconstructing the Kinetic SZ Power Spectrum,ApJ 756(2012) 15 [1109.0553]

    Pith/arXiv arXiv 2012

  6. [6]

    Battaglia, A

    N. Battaglia, A. Natarajan, H. Trac, R. Cen and A. Loeb,Reionization on Large Scales. III. Predictions for Low-l Cosmic Microwave Background Polarization and High-l Kinetic Sunyaev-Zel’dovich Observables,ApJ776(2013) 83 [1211.2832]

    Pith/arXiv arXiv 2013

  7. [7]

    Sunyaev and Y.B

    R.A. Sunyaev and Y.B. Zel’dovich,The Spectrum of Primordial Radiation, its Distortions and their Significance,Comments on Astrophysics and Space Physics2(1970) 66

    1970

  8. [8]

    Komatsu and U

    E. Komatsu and U. Seljak,The Sunyaev-Zel’dovich angular power spectrum as a probe of cosmological parameters,MNRAS336(2002) 1256

    2002

  9. [9]

    De Zotti, M

    G. De Zotti, M. Massardi, M. Negrello and J. Wall,Radio and millimeter continuum surveys and their astrophysical implications,A&AR18(2010) 1 [0908.1896]

    Pith/arXiv arXiv 2010

  10. [10]

    Fixsen, E

    D.J. Fixsen, E. Dwek, J.C. Mather, C.L. Bennett and R.A. Shafer,The Spectrum of the Extragalactic Far-Infrared Background from the COBE FIRAS Observations,ApJ508(1998) 123 [arXiv:astro-ph/9803021]

    Pith/arXiv arXiv 1998

  11. [11]

    Hauser and E

    M.G. Hauser and E. Dwek,The Cosmic Infrared Background: Measurements and Implications, ARA&A39(2001) 249 [arXiv:astro-ph/0105539]

    Pith/arXiv arXiv 2001

  12. [12]

    Lagache, J.-L

    G. Lagache, J.-L. Puget and H. Dole,Dusty Infrared Galaxies: Sources of the Cosmic Infrared Background,ARA&A43(2005) 727 [arXiv:astro-ph/0507298]

    Pith/arXiv arXiv 2005

  13. [13]

    H. Dole, G. Lagache, J.-L. Puget, K.I. Caputi, N. Fernández-Conde, E. Le Floc’h et al.,The cosmic infrared background resolved by Spitzer. Contributions of mid-infrared galaxies to the far-infrared background,A&A451(2006) 417 [arXiv:astro-ph/0603208]

    Pith/arXiv arXiv 2006

  14. [14]

    Hezaveh, D.P

    Y.D. Hezaveh, D.P. Marrone, C.D. Fassnacht, J.S. Spilker, J.D. Vieira, J.E. Aguirre et al., ALMA Observations of SPT-discovered, Strongly Lensed, Dusty, Star-forming Galaxies,ApJ 767(2013) 132 [1303.2722]

    Pith/arXiv arXiv 2013

  15. [15]

    S. Das, T. Louis, M.R. Nolta, G.E. Addison, E.S. Battistelli, J.R. Bond et al.,The Atacama Cosmology Telescope: temperature and gravitational lensing power spectrum measurements from three seasons of data,JCAP4(2014) 14 [1301.1037]

    Pith/arXiv arXiv 2014

  16. [16]

    Louis, A

    T. Louis, A. La Posta, Z. Atkins, H.T. Jense, I. Abril-Cabezas, G.E. Addison et al.,The Atacama Cosmology Telescope: DR6 Power Spectra, Likelihoods andΛCDM Parameters,arXiv e-prints(2025) arXiv:2503.14452 [2503.14452]

    Pith/arXiv arXiv 2025

  17. [17]

    Lueker, C.L

    M. Lueker, C.L. Reichardt, K.K. Schaffer, O. Zahn, P.A.R. Ade, K.A. Aird et al., Measurements of Secondary Cosmic Microwave Background Anisotropies with the South Pole Telescope,ApJ719(2010) 1045 [0912.4317]. – 30 –

    Pith/arXiv arXiv 2010

  18. [18]

    Shirokoff, C.L

    E. Shirokoff, C.L. Reichardt, L. Shaw, M. Millea, P.A.R. Ade, K.A. Aird et al.,Improved Constraints on Cosmic Microwave Background Secondary Anisotropies from the Complete 2008 South Pole Telescope Data,ApJ736(2011) 61 [1012.4788]

    Pith/arXiv arXiv 2008

  19. [19]

    Reichardt, L

    C.L. Reichardt, L. Shaw, O. Zahn, K.A. Aird, B.A. Benson, L.E. Bleem et al.,A Measurement of Secondary Cosmic Microwave Background Anisotropies with Two Years of South Pole Telescope Observations,ApJ755(2012) 70 [1111.0932]

    Pith/arXiv arXiv 2012

  20. [20]

    George, C.L

    E.M. George, C.L. Reichardt, K.A. Aird, B.A. Benson, L.E. Bleem, J.E. Carlstrom et al.,A Measurement of Secondary Cosmic Microwave Background Anisotropies from the 2500-Square-degree SPT-SZ Survey,ApJ799(2015) 177 [1408.3161]

    Pith/arXiv arXiv 2015

  21. [21]

    Reichardt, S

    C.L. Reichardt, S. Patil, P.A.R. Ade, A.J. Anderson, J.E. Austermann, J.S. Avva et al.,An Improved Measurement of the Secondary Cosmic Microwave Background Anisotropies from the SPT-SZ + SPTpol Surveys,ApJ908(2021) 199 [2002.06197]

    Pith/arXiv arXiv 2021

  22. [22]

    Beringue, K.M

    B. Beringue, K.M. Surrao, J.C. Hill, Z. Atkins, N. Battaglia, B. Bolliet et al.,The Atacama Cosmology Telescope: DR6 power spectrum foreground model and validation,JCAP2025 (2025) 082 [2506.06274]

    arXiv 2025

  23. [23]

    Zebrowski, C.L

    J.A. Zebrowski, C.L. Reichardt, A.J. Anderson, B. Ansarinejad, M. Archipley, L. Balkenhol et al.,Constraints on Inflationary Gravitational Waves with Two Years of SPT-3G Data,arXiv e-prints(2025) arXiv:2505.02827 [2505.02827]

    Pith/arXiv arXiv 2025

  24. [24]

    Camphuis, W

    E. Camphuis, W. Quan, L. Balkenhol, A.R. Khalife, F. Ge, F. Guidi et al.,SPT-3G D1: CMB temperature and polarization power spectra and cosmology from 2019 and 2020 observations of the SPT-3G Main field,arXiv e-prints(2025) arXiv:2506.20707 [2506.20707]

    Pith/arXiv arXiv 2019

  25. [25]

    Sobrin, A.J

    J.A. Sobrin, A.J. Anderson, A.N. Bender, B.A. Benson, D. Dutcher, A. Foster et al.,The Design and Integrated Performance of SPT-3G,ApJS258(2022) 42 [2106.11202]

    Pith/arXiv arXiv 2022

  26. [26]

    Dutcher, L

    D. Dutcher, L. Balkenhol, P.A.R. Ade, Z. Ahmed, E. Anderes, A.J. Anderson et al., Measurements of the E -mode polarization and temperature-E -mode correlation of the CMB from SPT-3G 2018 data,PRD104(2021) 022003 [2101.01684]

    Pith/arXiv arXiv 2018

  27. [27]

    Hivon, K.M

    E. Hivon, K.M. Górski, C.B. Netterfield, B.P. Crill, S. Prunet and F. Hansen,MASTER of the Cosmic Microwave Background Anisotropy Power Spectrum: A Fast Method for Statistical Analysis of Large and Complex Cosmic Microwave Background Data Sets,ApJ567(2002) 2 [astro-ph/0105302]

    Pith/arXiv arXiv 2002

  28. [28]

    Tristram, J.F

    M. Tristram, J.F. Macías-Pérez, C. Renault and D. Santos,XSPECT, estimation of the angular power spectrum by computing cross-power spectra with analytical error bars,MNRAS 358(2005) 833 [astro-ph/0405575]

    Pith/arXiv arXiv 2005

  29. [29]

    Alonso, J

    D. Alonso, J. Sanchez, A. Slosar and LSST Dark Energy Science Collaboration,A unified pseudo-Cℓ framework,MNRAS484(2019) 4127 [1809.09603]

    Pith/arXiv arXiv 2019

  30. [30]

    Hartlap, P

    J. Hartlap, P. Simon and P. Schneider,Why your model parameter confidences might be too optimistic. Unbiased estimation of the inverse covariance matrix,A&A464(2007) 399 [astro-ph/0608064]

    Pith/arXiv arXiv 2007

  31. [31]

    Hamimeche and A

    S. Hamimeche and A. Lewis,Properties and use of CMB power spectrum likelihoods,PRD79 (2009) 083012 [0902.0674]

    Pith/arXiv arXiv 2009

  32. [32]

    Taylor, B

    A. Taylor, B. Joachimi and T. Kitching,Putting the precision in precision cosmology: How accurate should your data covariance matrix be?,MNRAS432(2013) 1928 [1212.4359]

    Pith/arXiv arXiv 2013

  33. [33]

    Dodelson and M.D

    S. Dodelson and M.D. Schneider,The effect of covariance estimator error on cosmological parameter constraints,PRD88(2013) 063537 [1304.2593]

    Pith/arXiv arXiv 2013

  34. [34]

    Balkenhol and C.L

    L. Balkenhol and C.L. Reichardt,The parameter-level performance of covariance matrix conditioning in cosmic microwave background data analyses,MNRAS512(2022) 4394 [2110.03180]. – 31 – [35]SPT-3G Collaborationcollaboration,Cosmology from cmb lensing and delensedeepower spectra using 2019–2020 spt-3g polarization data,Phys. Rev. D111(2025) 083534

    Pith/arXiv arXiv 2022

  35. [36]

    Aghanim, Y

    Planck Collaboration, N. Aghanim, Y. Akrami, M. Ashdown, J. Aumont, C. Baccigalupi et al., Planck 2018 results. VI. Cosmological parameters,A&A641(2020) A6 [1807.06209]

    Pith/arXiv arXiv 2018

  36. [37]

    Balkenhol, D

    L. Balkenhol, D. Dutcher, A. Spurio Mancini, A. Doussot, K. Benabed, S. Galli et al., Measurement of the CMB temperature power spectrum and constraints on cosmology from the SPT-3G 2018 T T , T E , and E E dataset,PRD108(2023) 023510 [2212.05642]

    Pith/arXiv arXiv 2018

  37. [38]

    Torrado and A

    J. Torrado and A. Lewis,Cobaya: code for Bayesian analysis of hierarchical physical models, JCAP2021(2021) 057 [2005.05290]

    Pith/arXiv arXiv 2021

  38. [39]

    Spurio Mancini, D

    A. Spurio Mancini, D. Piras, J. Alsing, B. Joachimi and M.P. Hobson,COSMOPOWER: emulating cosmological power spectra for accelerated Bayesian inference from next-generation surveys,MNRAS511(2022) 1771 [2106.03846]

    Pith/arXiv arXiv 2022

  39. [40]

    L.D. Shaw, D. Nagai, S. Bhattacharya and E.T. Lau,Impact of Cluster Physics on the Sunyaev-Zel’dovich Power Spectrum,ApJ725(2010) 1452 [1006.1945]

    Pith/arXiv arXiv 2010

  40. [41]

    Omori,AGORA: Multicomponent simulation for cross-survey science,MNRAS530(2024) 5030 [2212.07420]

    Y. Omori,AGORA: Multicomponent simulation for cross-survey science,MNRAS530(2024) 5030 [2212.07420]

    Pith/arXiv arXiv 2024

  41. [42]

    Zahn, C.L

    O. Zahn, C.L. Reichardt, L. Shaw, A. Lidz, K.A. Aird, B.A. Benson et al.,Cosmic Microwave Background Constraints on the Duration and Timing of Reionization from the South Pole Telescope,ApJ756(2012) 65 [1111.6386]

    Pith/arXiv arXiv 2012

  42. [43]

    Viero, L

    M.P. Viero, L. Wang, M. Zemcov, G. Addison, A. Amblard, V. Arumugam et al.,HerMES: Cosmic Infrared Background Anisotropies and the Clustering of Dusty Star-forming Galaxies, ApJ772(2013) 77 [1208.5049]

    Pith/arXiv arXiv 2013

  43. [44]

    Shang, Z

    C. Shang, Z. Haiman, L. Knox and S.P. Oh,Improved models for cosmic infrared background anisotropies: new constraints on the infrared galaxy population,MNRAS421(2012) 2832 [1109.1522]

    Pith/arXiv arXiv 2012

  44. [45]

    Efstathiou and F

    G. Efstathiou and F. McCarthy,The Power Spectrum of the Thermal Sunyaev-Zeldovich Effect,MNRAS(2025) [2502.10232]

    Pith/arXiv arXiv 2025

  45. [46]

    Calabrese, R

    E. Calabrese, R. Hložek, N. Battaglia, J.R. Bond, F. de Bernardis, M.J. Devlin et al.,Precision epoch of reionization studies with next-generation CMB experiments,JCAP2014(2014) 010 [1406.4794]

    Pith/arXiv arXiv 2014

  46. [47]

    Kramer, A

    D. Kramer, A. van Engelen, C. Cain, N. MacCrann, H. Trac, S. Grayson et al., Cross-correlating the patchy screening and kinetic Sunyaev-Zel’dovich effects as a new probe of reionization,arXiv e-prints(2025) arXiv:2501.07623 [2501.07623]

    arXiv 2025

  47. [48]

    Abdalla, G.F

    E. Abdalla, G.F. Abellán, A. Aboubrahim, A. Agnello, Ö. Akarsu, Y. Akrami et al.,Cosmology intertwined: A review of the particle physics, astrophysics, and cosmology associated with the cosmological tensions and anomalies,Journal of High Energy Astrophysics34(2022) 49 [2203.06142]

    Pith/arXiv arXiv 2022

  48. [49]

    Battaglia, H

    N. Battaglia, H. Trac, R. Cen and A. Loeb,Reionization on Large Scales. I. A Parametric Model Constructed from Radiation-hydrodynamic Simulations,ApJ776(2013) 81 [1211.2821]

    Pith/arXiv arXiv 2013

  49. [50]

    H. Trac, N. Chen, I. Holst, M.A. Alvarez and R. Cen,Amber: A semi-numerical abundance matching box for the epoch of reionization,The Astrophysical Journal927(2022) 186

    2022

  50. [51]

    Raghunathan, P.A.R

    S. Raghunathan, P.A.R. Ade, A.J. Anderson, B. Ansarinejad, M. Archipley, J.E. Austermann et al.,First Constraints on the Epoch of Reionization Using the Non-Gaussianity of the Kinematic Sunyaev-Zel’dovich Effect from the South Pole Telescope and Herschel-SPIRE Observations,PRL133(2024) 121004 [2403.02337]. – 32 –

    Pith/arXiv arXiv 2024

  51. [52]

    Anderson, P

    A.J. Anderson, P. Barry, A.N. Bender, B.A. Benson, L.E. Bleem, J.E. Carlstrom et al., SPT-3G+: mapping the high-frequency cosmic microwave background using kinetic inductance detectors, inMillimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy XI, J. Zmuidzinas and J.-R. Gao, eds., vol. 12190 ofSociety of Photo-Optical Inst...

    Pith/arXiv arXiv 2022

  52. [53]

    Simons Observatory Collaboration,The Simons Observatory: science goals and forecasts, JCAP2019(2019) 056 [1808.07445]

    Pith/arXiv arXiv 2019

  53. [54]

    Abazajian, G

    K. Abazajian, G. Addison, P. Adshead, Z. Ahmed, S.W. Allen, D. Alonso et al.,CMB-S4 Science Case, Reference Design, and Project Plan,arXiv e-prints(2019) [1907.04473]

    Pith/arXiv arXiv 2019

  54. [55]

    Sehgal, S

    N. Sehgal, S. Aiola, Y. Akrami, K. Basu, M. Boylan-Kolchin, S. Bryan et al.,CMB-HD: An Ultra-Deep, High-Resolution Millimeter-Wave Survey Over Half the Sky, inBulletin of the American Astronomical Society, vol. 51, p. 6, Sept., 2019, DOI [1906.10134]

    Pith/arXiv arXiv 2019

  55. [56]

    Górski, E

    K.M. Górski, E. Hivon, A.J. Banday, B.D. Wandelt, F.K. Hansen, M. Reinecke et al., HEALPix: A Framework for High-Resolution Discretization and Fast Analysis of Data Distributed on the Sphere,ApJ622(2005) 759 [arXiv:astro-ph/0409513]. – 33 –

    Pith/arXiv arXiv 2005