pith. machine review for the scientific record. sign in

arxiv: 2506.20707 · v2 · submitted 2025-06-25 · 🌌 astro-ph.CO

Recognition: 2 theorem links

· Lean Theorem

SPT-3G D1: CMB temperature and polarization power spectra and cosmology from 2019 and 2020 observations of the SPT-3G Main field

E. Camphuis , W. Quan , L. Balkenhol , A. R. Khalife , F. Ge , F. Guidi , N. Huang , G. P. Lynch
show 89 more authors
Y. Omori C. Trendafilova A. J. Anderson B. Ansarinejad M. Archipley P. S. Barry K. Benabed A. N. Bender B. A. Benson F. Bianchini L. E. Bleem F. R. Bouchet L. Bryant M. G. Campitiello J. E. Carlstrom C. L. Chang P. Chaubal 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 K. Fichman A. Foster S. Galli A. E. Gambrel R. W. Gardner N. Goeckner-Wald R. Gualtieri S. Guns N. W. Halverson E. Hivon G. P. Holder W. L. Holzapfel J. C. Hood A. Hryciuk F. K\'eruzor\'e L. Knox M. Korman K. Kornoelje C.-L. Kuo K. Levy A. E. Lowitz C. Lu A. Maniyar E. S. Martsen F. Menanteau M. Millea J. Montgomery Y. Nakato T. Natoli G. I. Noble A. Ouellette Z. Pan P. Paschos K. A. Phadke A. W. Pollak K. Prabhu S. Raghunathan M. Rahimi A. Rahlin C. L. Reichardt M. Rouble J. E. Ruhl E. Schiappucci A. Simpson J. A. Sobrin A. A. Stark J. Stephen C. Tandoi B. Thorne C. Umilta J. D. Vieira A. Vitrier Y. Wan N. Whitehorn W. L. K. Wu M. R. Young J. A. Zebrowski
Authors on Pith no claims yet

Pith reviewed 2026-05-13 19:07 UTC · model grok-4.3

classification 🌌 astro-ph.CO
keywords CMB power spectraSPT-3GHubble constantLCDMCMB lensingcosmological parametersHubble tension
0
0 comments X

The pith

SPT-3G measurements of CMB power spectra give H0 = 66.66 km/s/Mpc from ground-based data alone, 6.2 sigma below local values.

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

The paper reports new temperature and E-mode polarization power spectra from deep SPT-3G observations covering 4 percent of the sky, the deepest maps used in any CMB TT/TE/EE analysis so far. These spectra are the most precise at high multipoles for the lensed EE spectrum between l=1800-4000 and the TE spectrum between l=2200-4000. When the spectra are combined with prior SPT-3G lensing measurements, the derived LCDM parameters match those from Planck and ACT-DR6 at similar precision. The resulting Hubble constant stands 6.2 sigma away from local distance-ladder results, while CMB data alone show no requirement for physics beyond standard LCDM.

Core claim

The SPT-3G TT/TE/EE spectra, validated by blind tests, combined with lensing data constrain the standard LCDM model to H0 = 66.66 ± 0.60 km/s/Mpc and other parameters consistent with Planck and ACT-DR6. The joint ground-based (SPT + ACT) primary and lensing data now reach Planck-level constraining power on some parameters, and the three-experiment CMB combination yields the tightest CMB constraints to date with H0 = 67.19 ± 0.38 km/s/Mpc and σ8 = 0.8137 ± 0.0037. CMB data alone show no evidence for physics beyond LCDM, yet a 2.8 sigma tension appears between these CMB results and DESI-DR2 BAO measurements in the standard model.

What carries the argument

The SPT-3G temperature and E-mode polarization angular power spectra from 2019 and 2020 observations, combined with previously published SPT-3G CMB lensing measurements to fit LCDM parameters.

Load-bearing premise

The analysis assumes foreground contamination, instrumental systematics, and lensing effects have been modeled and subtracted correctly, as checked by blind tests.

What would settle it

An independent measurement that recovers an EE spectrum at l=1800-4000 differing by more than the reported uncertainty from the SPT-3G result would falsify the claim of highest precision and change the derived cosmological parameters.

read the original abstract

We present measurements of the temperature and E-mode polarization angular power spectra of the cosmic microwave background (CMB) from observations of 4% of the sky with SPT-3G, the current camera on the South Pole Telescope (SPT). The maps used in this analysis are the deepest used in a CMB TT/TE/EE analysis to date. The maps and resulting power spectra have been validated through blind and unblind tests. The measurements of the lensed EE and TE spectra are the most precise to date at l=1800-4000 and l=2200-4000, respectively. Combining our TT/TE/EE spectra with previously published SPT-3G CMB lensing results, we find parameters for the standard LCDM model consistent with Planck and ACT-DR6 with comparable constraining power. We report a Hubble constant of $H_0=66.66\pm0.60$ km/s/Mpc from SPT-3G alone, 6.2 sigma away from local measurements from SH0ES. For the first time, combined ground-based (SPT+ACT) CMB primary and lensing data have reached Planck's constraining power on some parameters, a milestone for CMB cosmology. The combination of these three CMB experiments yields the tightest CMB constraints to date, with $H_0=67.19\pm0.38$ km/s/Mpc, and the amplitude of clustering $\sigma_8=0.8137\pm0.0037$. CMB data alone show no evidence for physics beyond LCDM; however, we observe a 2.8 sigma difference in LCDM between CMB and baryon acoustic oscillation (BAO) results from DESI-DR2, which is relaxed in extended models. The combination of CMB and BAO yields 2-3 sigma shifts from LCDM in the curvature of the universe, the amplitude of CMB lensing, or the dark energy equation of state. It also drives mild preferences for models that address the Hubble tension through modified recombination or variations in the electron mass in a non-flat universe. This work highlights the growing power of ground-based CMB experiments and lays a foundation for further cosmological analyses with SPT-3G.

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

0 major / 3 minor

Summary. The paper presents measurements of CMB TT, TE, and EE angular power spectra from 2019-2020 SPT-3G observations covering 4% of the sky, using the deepest maps to date in a CMB primary anisotropy analysis. The spectra are validated via blind and unblind tests, with claims that the lensed EE spectrum is the most precise at l=1800-4000 and TE at l=2200-4000. Combining the spectra with prior SPT-3G lensing results yields LCDM parameter constraints consistent with Planck and ACT-DR6 (including H0=66.66±0.60 km/s/Mpc from SPT-3G alone, 6.2σ from SH0ES), while joint analyses with ACT and BAO explore extensions and tensions.

Significance. If the results hold, this constitutes a major advance for ground-based CMB cosmology: SPT+ACT primary plus lensing data now match Planck's constraining power on key parameters for the first time, with the combined three-experiment CMB dataset providing the tightest CMB-only constraints to date. The independent H0 measurement and consistency checks strengthen the case for the Hubble tension while the BAO comparisons highlight opportunities for testing extensions to LCDM.

minor comments (3)
  1. [Abstract, §5] Abstract and §5: The statement that SPT+ACT have 'reached Planck's constraining power on some parameters' would benefit from a brief quantitative comparison (e.g., error-bar ratios on Ω_m or σ_8) rather than a qualitative claim.
  2. [Figure 3, §4.3] Figure 3 and §4.3: The residual plots after foreground subtraction could include the expected noise level from simulations to make the validation more immediately interpretable.
  3. [Table 2] Table 2: The parameter table lists H0 from SPT-3G alone but does not explicitly note whether the quoted uncertainty includes the full covariance with lensing or only primary spectra; a footnote would clarify this.

Simulated Author's Rebuttal

0 responses · 0 unresolved

We thank the referee for their positive review and recommendation to accept the manuscript. We appreciate the recognition of the significance of these SPT-3G results as a milestone for ground-based CMB cosmology.

Circularity Check

0 steps flagged

No significant circularity

full rationale

The paper extracts TT/TE/EE power spectra directly from observed SPT-3G maps using standard map-making and estimation pipelines, validated by blind tests. Cosmological parameters including H0 are obtained by fitting these spectra to external theoretical LCDM predictions. The combination with prior SPT-3G lensing results cites independent previously published work whose constraining power is external to the present spectra. No load-bearing step reduces by construction to a fitted input, self-definition, or unverified self-citation chain; the reported precision statements and 6.2-sigma tension follow from the published likelihood under standard assumptions.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

The central claims rest on the validity of the standard LCDM model and on the assumption that data processing has removed all significant foregrounds and systematics; no new physical entities are introduced.

free parameters (2)
  • Hubble constant H0
    Fitted directly to the measured TT/TE/EE spectra within the LCDM model
  • Other LCDM parameters (Omega_m, sigma_8, etc.)
    Fitted to the same spectra; values reported with uncertainties
axioms (2)
  • domain assumption Standard flat Lambda-CDM cosmology governs the evolution of perturbations
    Invoked for all parameter inference and comparison to Planck/ACT
  • domain assumption Foregrounds, noise, and lensing have been accurately modeled and subtracted
    Supported by blind tests but remains a modeling assumption

pith-pipeline@v0.9.0 · 6283 in / 1475 out tokens · 41671 ms · 2026-05-13T19:07:09.171820+00:00 · methodology

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Lean theorems connected to this paper

Citations machine-checked in the Pith Canon. Every link opens the source theorem in the public Lean library.

  • IndisputableMonolith.Foundation.DAlembert.Inevitability bilinear_family_forced unclear
    ?
    unclear

    Relation between the paper passage and the cited Recognition theorem.

    We present measurements of the temperature and E-mode polarization angular power spectra of the cosmic microwave background (CMB) from observations of 4% of the sky with SPT-3G... Combining our TT/TE/EE spectra with previously published SPT-3G CMB lensing results, we find parameters for the standard LCDM model consistent with Planck and ACT-DR6

  • IndisputableMonolith.Foundation.DimensionForcing dimension_forced unclear
    ?
    unclear

    Relation between the paper passage and the cited Recognition theorem.

    We report a Hubble constant of H0=66.66±0.60 km/s/Mpc from SPT-3G alone, 6.2 sigma away from local measurements from SH0ES.

What do these tags mean?
matches
The paper's claim is directly supported by a theorem in the formal canon.
supports
The theorem supports part of the paper's argument, but the paper may add assumptions or extra steps.
extends
The paper goes beyond the formal theorem; the theorem is a base layer rather than the whole result.
uses
The paper appears to rely on the theorem as machinery.
contradicts
The paper's claim conflicts with a theorem or certificate in the canon.
unclear
Pith found a possible connection, but the passage is too broad, indirect, or ambiguous to say the theorem truly supports the claim.

Forward citations

Cited by 21 Pith papers

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

  1. Dispersion Measure Distribution of Unlocalized Fast Radio Bursts as a Probe of the Hubble Constant

    astro-ph.CO 2026-04 unverdicted novelty 8.0

    The DM distribution of unlocalized FRBs yields H0 = 73.8 +14.0/-12.3 km/s/Mpc with 18% uncertainty.

  2. Measuring neutrino mass and asymmetry through galaxy pairwise peculiar velocity

    astro-ph.CO 2026-04 unverdicted novelty 7.0

    Galaxy pairwise peculiar velocities from Cosmicflows-4 yield M_ν = 0.24^{+0.34}_{-0.18} eV and η² = 2.14^{+0.30}_{-0.32} (7σ non-zero asymmetry) in the CMB framework, consistent with prior Planck results.

  3. Dilaton-Flattened Axion Inflation

    hep-ph 2026-04 unverdicted novelty 7.0

    Dilaton backreaction on an anomaly-inspired axion potential generates a closed-form Lambert-W flattened hilltop, giving r ≈ 0.033–0.036 and α_s ≈ −4.6×10^{-4} at N=56 with strictly adiabatic dynamics.

  4. Geometric Constraints on the Pre-Recombination Expansion History from the Hubble Tension

    astro-ph.CO 2026-04 unverdicted novelty 6.0

    Model-independent reconstruction shows that early-universe modifications resolving the Hubble tension exist at the background level, requiring a smooth ~15% pre-recombination expansion rate enhancement.

  5. A data-driven prediction for the primordial deuterium abundance

    astro-ph.CO 2026-04 unverdicted novelty 6.0

    Gaussian process regression on nuclear data predicts 10^5 D/H = 2.442 ± 0.040, 1.70 sigma below observation and consistent with first-principles calculations.

  6. Double the axions, half the tension: multi-field early dark energy eases the Hubble tension

    astro-ph.CO 2026-04 unverdicted novelty 6.0

    Two-field axion-like early dark energy reduces Hubble tension to 1.5 sigma residual and improves high-ell CMB fits over single-field models.

  7. Einstein-Cartan pseudoscalaron inflation, reheating and nonthermal leptogenesis

    astro-ph.CO 2026-05 unverdicted novelty 5.0

    Einstein-Cartan pseudoscalaron inflation coupled to type-I seesaw neutrinos makes nonthermal leptogenesis a necessary mechanism for the baryon asymmetry, yielding ns ~ 0.97, r ~ 0.004 and nB/s ~ 8.7e-11 for gamma ~ -1...

  8. The End of the First Act: Spectral Running, Interacting Dark Radiation, and the Hubble Tension in Light of ACT DR6 Data

    astro-ph.CO 2026-04 unverdicted novelty 5.0

    Including spectral running α_s, β_s and self-interacting dark radiation relaxes the ACT DR6 bound on ΔN_eff to <0.58 and lowers the Hubble tension to 2.2σ with three extra parameters.

  9. Generalizing the CPL Parametrization through Dark Sector Interaction

    astro-ph.CO 2026-04 unverdicted novelty 5.0

    Dynamical couplings in interacting dark energy models reduce deviations from LambdaCDM to 1.3-1.5 sigma and yield no Bayesian preference over the standard model.

  10. Cosmological Impact of Redshift-Dependent Type Ia Supernovae Calibration

    astro-ph.CO 2026-04 unverdicted novelty 5.0

    A phenomenological redshift-dependent SNIa magnitude correction shows no evidence in ΛCDM but is preferred at 4.3σ with dynamical dark energy, reducing Hubble tension to 1.5σ.

  11. Reconstructing inflationary features on large scales using genetic algorithm

    astro-ph.CO 2026-04 unverdicted novelty 5.0

    Genetic algorithm reconstructs single-field inflationary models with features in the scalar power spectrum that fit Planck 2018 CMB data better by Δχ² ≲ -10 and suggest alternative background parameters.

  12. Do equation of state parametrizations of dark energy faithfully capture the dynamics of the late universe?

    astro-ph.CO 2026-04 unverdicted novelty 5.0

    Node-based reconstruction of cosmic expansion prefers stronger deceleration at z≈1.7 than smooth DE EoS parametrizations, isolating z~1.5-2 as a window where the latter may compress localized kinematic features permit...

  13. FolpsD: combining EFT and phenomenological approaches for joint power spectrum and bispectrum analyses

    astro-ph.CO 2026-04 conditional novelty 5.0

    FolpsD combines EFT power spectrum and tree-level bispectrum with damping to enable joint analyses that improve cosmological constraints from DESI-like galaxy mocks by up to 30% on As and omega_cdm while extending the...

  14. Disentangling cosmic distance tensions with early and late dark energy

    astro-ph.CO 2026-04 unverdicted novelty 5.0

    Early dark energy resolves CMB-BAO tension and, combined with thawing quintessence, reduces overall cosmological tensions without phantom crossing.

  15. Joint Curvature and Growth Rate measurements with Supernova Peculiar Velocities and the CMB

    astro-ph.CO 2026-04 unverdicted novelty 5.0

    SN peculiar velocities plus Planck CMB data give joint constraints on σ8, γ, and Ωk, with hints of positive curvature (Ωk ≈ -0.01) at 2-3σ and γ values consistent with GR.

  16. A generic $\omega_b$ tension in early-time solutions to the Hubble tension

    astro-ph.CO 2026-04 unverdicted novelty 5.0

    Early-time Hubble tension solutions generically raise the preferred baryon density ω_b, conflicting with BBN deuterium constraints and producing poorer fits to CMB, BAO, supernova, and BBN data than ΛCDM.

  17. Is the $w_0w_a$CDM cosmological parameterization evidence for dark energy dynamics partially caused by the excess smoothing of Planck PR4 CMB anisotropy data?

    astro-ph.CO 2026-04 conditional novelty 5.0

    Planck PR4 CMB data mildly favors dynamical dark energy, but this preference weakens when accounting for possible excess smoothing, indicating the signal may partly arise from data processing issues.

  18. Single field slow-roll inflation with step uplift to $n_s=1$

    astro-ph.CO 2026-04 unverdicted novelty 5.0

    Single-field slow-roll inflation achieves ns=1 by ending inflation suddenly via a large step in the potential.

  19. F-Term Hybrid Inflation with T-Model K\"ahler Geometry and Beyond

    hep-ph 2026-05 unverdicted novelty 4.0

    F-term hybrid inflation with SU(1,1)/U(1) or SU(2)/U(1) Kähler geometry in GUTs can be realized without inflationary extrema for broad parameters, matching ACT/SPT data via curvature and tadpole adjustments while pred...

  20. The Status of Gravitational Vector Perturbations with Recent CMB Data

    astro-ph.CO 2026-05 unverdicted novelty 4.0

    Recent CMB datasets tighten 95% CL upper bounds on vector-mode amplitude r_v to 1.3e-4 (neutrino isocurvature), 6.8 (octupole), and 4.2 (sourced) at k=0.05 Mpc^-1, with no significant detection.

  21. BROOM: a python package for model-independent analysis of microwave astronomical data

    astro-ph.CO 2026-04 unverdicted novelty 4.0

    BROOM is a Python package that applies ILC and GILC techniques for model-independent separation of CMB, SZ, and foreground signals in microwave data along with diagnostic and simulation utilities.

Reference graph

Works this paper leans on

203 extracted references · 203 canonical work pages · cited by 21 Pith papers · 5 internal anchors

  1. [1]

    subset priors

    Foreground model functional forms In this section, we present the explicit functional forms of the foreground model components used in the analysis(see§VB2foradditionaldiscussion). Themodel includes the following terms. First, unresolved sources are modeled as a Poisson component with a power-law dependence on multipole ℓ: DPoisson ℓ,µν =A Poisson µν ℓ 30...

    work page 2000

  2. [2]

    extended

    Robustness of the foreground model We compare the “extended” likelihood that treats the tSZ–CIB correlation as a free parameter and includes CIB clustering amplitudes for the95×95GHz,95× 150GHz, and95×220GHzspectra, ratherthanmarginal- izing over them in the covariance matrix computation, to the baseline likelihood described in §VB2. This extended model a...

    work page

  3. [3]

    First, we construct the vector∆of observed values and the corresponding predicted covariance matrixΣ ∆

    Probability to exceed We outline the procedure for computing the PTE for each test presented in this work. First, we construct the vector∆of observed values and the corresponding predicted covariance matrixΣ ∆. The associatedχ 2 statistic is then calculated as: χ2 = ∆T Σ∆∆.(G1) WethencomputethePTEastheprobabilityofobserving aχ ′2 value greater than or equ...

    work page

  4. [4]

    The objective is to assess the consistency among the various frequency channels and to identify any potential issues in the data or analysis pipeline

    Difference tests To validate the pipeline, we conduct a series of frequency-difference tests, comparing spectra derived from different frequency combinations. The objective is to assess the consistency among the various frequency channels and to identify any potential issues in the data or analysis pipeline. The methodology is described in §VIB1 and a sub...

    work page

  5. [5]

    Unlike the frequency-difference tests, which compare pairs of spectra, the conditional tests assess a given spectrum against its prediction based on all other spectra

    Conditional tests In addition to the frequency-difference tests, we conduct conditional tests to evaluate the consistency of the data across different frequency combinations. Unlike the frequency-difference tests, which compare pairs of spectra, the conditional tests assess a given spectrum against its prediction based on all other spectra. This approach ...

    work page 2018

  6. [6]

    Aghanim et al

    Planck Collaboration, Aghanim, N., Akrami, Y., et al. Planck 2018 results. VI. Cosmological parameters. 2020, A&A, 641, A6, doi:10.1051/0004-6361/201833910

    work page doi:10.1051/0004-6361/201833910 2018

  7. [7]

    G., Casertano, S., Yuan, W., Macri, L

    Breuval, L., Riess, A. G., Casertano, S., Yuan, W., Macri, L. M., Romaniello, M., Murakami, Y. S., Scolnic, D., Anand, G. S., & Soszyński, I. Small Magellanic Cloud Cepheids Observed with the Hubble Space Telescope Provide a New Anchor for the SH0ES Distance Ladder. 2024, The Astrophysical Journal, 973, 30, doi:10.3847/1538-4357/ad630e

    work page doi:10.3847/1538-4357/ad630e 2024

  8. [8]

    DESI DR2 Results II: Measurements of Baryon Acoustic Oscillations and Cosmological Constraints

    DESI Collaboration, Abdul-Karim, M., Aguilar, J., et al. DESI DR2 Results II: Measurements of Baryon Acoustic Oscillations and Cosmological Constraints. 2025, arXiv e-prints, arXiv:2503.14738, doi:10.48550/ arXiv.2503.14738

    work page internal anchor Pith review Pith/arXiv arXiv 2025

  9. [9]

    Abdul Karim et al

    DESI Collaboration, Abdul-Karim, M., Aguilar, J., et al. DESI DR2 Results I: Baryon Acoustic Oscillations from the Lyman Alpha Forest. 2025, arXiv e-prints, arXiv:2503.14739, doi:10.48550/arXiv.2503.14739

    work page doi:10.48550/arxiv.2503.14739 2025

  10. [10]

    CMB polarization can constrain cosmology better than CMB temperature

    Galli, S., Benabed, K., Bouchet, F., Cardoso, J.-F., Elsner, F., Hivon, E., Mangilli, A., Prunet, S., & Wandelt, B. CMB polarization can constrain cosmology better than CMB temperature. 2014, Phys. Rev. D, 90, 063504, doi:10.1103/PhysRevD.90.063504

    work page doi:10.1103/physrevd.90.063504 2014

  11. [11]

    J., et al

    Naess, S., Guan, Y., Duivenvoorden, A. J., et al. 2025, The Atacama Cosmology Telescope: DR6 Maps, arXiv, doi:10.48550/arXiv.2503.14451

    work page doi:10.48550/arxiv.2503.14451 2025

  12. [13]

    The Atacama Cosmology Telescope: DR6 Constraints on Extended Cosmological Models

    Calabrese, E., Hill, J. C., Jense, H. T., et al. The Atacama Cosmology Telescope: DR6 Constraints on Extended Cosmological Models. 2025, arXiv e-prints, arXiv:2503.14454, doi:10.48550/arXiv.2503.14454

    work page internal anchor Pith review doi:10.48550/arxiv.2503.14454 2025

  13. [14]

    E., Ade, P

    Carlstrom, J. E., Ade, P. A. R., Aird, K. A., et al. The 10 Meter South Pole Telescope. 2011, PASP, 123, 568, doi:10.1086/659879

    work page doi:10.1086/659879 2011

  14. [15]

    T., Reichardt, C

    Story, K. T., Reichardt, C. L., Hou, Z., et al. A Measurement of the Cosmic Microwave Background Damping Tail from the 2500-Square-Degree SPT-SZ Survey. 2013, Astrophys. J., 779, 86, doi:10.1088/ 0004-637X/779/1/86

    work page 2013

  15. [16]

    W., Ade, P., Aird, K

    Henning, J. W., Ade, P., Aird, K. A., et al. Feedhorn- coupled TES polarimeter camera modules at 150 GHz for CMB polarization measurements with SPTpol. 2012, in Proc. SPIE, Vol. 8452, Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, doi:10.1117/12.927172

    work page doi:10.1117/12.927172 2012

  16. [17]

    A., Ade, P

    Sobrin, J. A., Ade, P. A. R., Ahmed, Z., et al. Design and characterization of the SPT-3G receiver. 2018, in Proc. SPIE, Vol. 10708, Proc. SPIE, 107081H, doi:10. 1117/12.2314366

    work page 2018

  17. [18]

    Dutcher, D., Balkenhol, L., Ade, P. A. R., et al. Mea- surementsoftheE-modepolarizationandtemperature- E -mode correlation of the CMB from SPT-3G 2018 data. 2021, Phys. Rev. D, 104, 022003, doi:10.1103/ PhysRevD.104.022003

    work page 2018

  18. [19]

    Balkenhol, L., Dutcher, D., Ade, P. A. R., et al. Constraints onΛCDM extensions from the SPT-3G 2018 E E and T E power spectra. 2021, Phys. Rev. D, 104, 083509, doi:10.1103/PhysRevD.104.083509

    work page doi:10.1103/physrevd.104.083509 2018

  19. [20]

    Balkenhol, D

    Balkenhol, L., Dutcher, D., Spurio Mancini, A., 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. 2023, Phys. Rev. D, 108, 023510, doi:10.1103/PhysRevD.108.023510

    work page doi:10.1103/physrevd.108.023510 2018

  20. [21]

    Pan, Z., Bianchini, F., Wu, W. L. K., et al. Measure- ment of gravitational lensing of the cosmic microwave background using SPT-3G 2018 data. 2023, Phys. Rev. D, 108, 122005, doi:10.1103/PhysRevD.108.122005

    work page doi:10.1103/physrevd.108.122005 2018

  21. [22]

    Cosmology fromCMBlensinganddelensedEEpowerspectrausing 2019–2020 SPT-3G polarization data

    Ge, F., Millea, M., Camphuis, E., et al. Cosmology fromCMBlensinganddelensedEEpowerspectrausing 2019–2020 SPT-3G polarization data. 2025, Phys. Rev. D, 111, 083534, doi:10.1103/PhysRevD.111.083534

    work page doi:10.1103/physrevd.111.083534 2019

  22. [23]

    A., Reichardt, C

    Zebrowski, J. A., Reichardt, C. L., Anderson, A. J., et al. Constraints on Inflationary Gravitational Waves with Two Years of SPT-3G Data. 2025, arXiv e-prints, arXiv:2505.02827, doi:10.48550/arXiv.2505.02827

    work page doi:10.48550/arxiv.2505.02827 2025

  23. [24]

    A., Takakura, S., et al

    Coerver, A., Zebrowski, J. A., Takakura, S., et al. Measurement and Modeling of Polarized Atmosphere at the South Pole with SPT-3G. 2025, Astrophys. J., 982, 15, doi:10.3847/1538-4357/ada35d

    work page doi:10.3847/1538-4357/ada35d 2025

  24. [25]

    Ade, P. A. R., Ahmed, Z., Amiri, M., et al. Im- proved Constraints on Primordial Gravitational Waves using Planck, WMAP, and BICEP/Keck Observations through the 2018 Observing Season. 2021, Phys. Rev. Lett., 127, 151301, doi:10.1103/PhysRevLett.127. 151301

    work page doi:10.1103/physrevlett.127 2018

  25. [26]

    Raghunathan, S., Ade, P. A. R., Anderson, A. J., 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. 2024, Phys. Rev. Lett., 133, 121004, doi:10.1103/PhysRevLett.133.121004

    work page doi:10.1103/physrevlett.133.121004 2024

  26. [27]

    L., Riedinger , J

    Pilbratt, G. L., Riedinger, J. R., Passvogel, T., Crone, G., Doyle, D., Gageur, U., Heras, A. M., Jewell, C., Metcalfe, L., Ott, S., & Schmidt, M. Herschel Space Observatory. An ESA facility for far-infrared and submillimetre astronomy. 2010, A&A, 518, L1, doi:10.1051/0004-6361/201014759

    work page doi:10.1051/0004-6361/201014759 2010

  27. [28]

    M., Hivon, E., Banday, A

    Górski, K. M., Hivon, E., Banday, A. J., Wandelt, B. D., Hansen, F. K., Reinecke, M., & Bartelmann, M. HEALPix: A Framework for High-Resolution Discretization and Fast Analysis of Data Distributed on the Sphere. 2005, Astrophys. J., 622, 759, doi:10. 1086/427976

    work page 2005

  28. [29]

    S., & Bond, J

    Szapudi, I., Prunet, S., Pogosyan, D., Szalay, A. S., & Bond, J. R. Fast Cosmic Microwave Background Analyses via Correlation Functions. 2001,Ap. J. Lett., 548, L115, doi:10.1086/319105

    work page doi:10.1086/319105 2001

  29. [30]

    Comparingthepropertiesoflocalglobularclustersystems:implicationsfortheformationoftheGalactic halo,

    Chon, G., Challinor, A., Prunet, S., Hivon, E., & Szapudi, I. Fast estimation of polarization power spectra using correlation functions. 2004, MNRAS, 350, 914, doi:10.1111/j.1365-2966.2004.07737.x

    work page doi:10.1111/j.1365-2966.2004.07737.x 2004

  30. [31]

    Accurate cosmic microwave background covariance matrices: Exact calculation and approxi- mations

    Camphuis, E., Benabed, K., Galli, S., Hivon, E., & Lilley, M. Accurate cosmic microwave background covariance matrices: Exact calculation and approxi- mations. 2022, Astronomy & Astrophysics, 668, A62, doi:10.1051/0004-6361/202243948 80

    work page doi:10.1051/0004-6361/202243948 2022

  31. [32]

    J., Leary, C., Maclaurin, D., Necula, G., Paszke, A., Van- derPlas, J., Wanderman-Milne, S., & Zhang, Q

    Bradbury, J., Frostig, R., Hawkins, P., Johnson, M. J., Leary, C., Maclaurin, D., Necula, G., Paszke, A., Van- derPlas, J., Wanderman-Milne, S., & Zhang, Q. 2018, JAX: composable transformations of Python+NumPy programs, 0.3.13.http://github.com/google/jax

    work page 2018

  32. [34]

    Uncertainty-aware and Data-efficient Cosmological Emulation using Gaussian Processes and PCA

    Günther, S. Uncertainty-aware and Data-efficient Cosmological Emulation using Gaussian Processes and PCA. 2023, arXiv e-prints, arXiv:2307.01138, doi:10. 48550/arXiv.2307.01138

    work page arXiv 2023

  33. [35]

    Spurio Mancini, A., Piras, D., Alsing, J., Joachimi, B., & Hobson, M. P. COSMOPOWER: emulating cosmological power spectra for accelerated Bayesian inference from next-generation surveys. 2022, MNRAS, 511, 1771, doi:10.1093/mnras/stac064

    work page doi:10.1093/mnras/stac064 2022

  34. [36]

    CosmoPower-JAX: high-dimensional Bayesian inference with differentiable cosmological emulators

    Piras, D., & Spurio Mancini, A. CosmoPower-JAX: high-dimensional Bayesian inference with differentiable cosmological emulators. 2023, The Open Journal of Astrophysics, 6, 20, doi:10.21105/astro.2305.06347

    work page doi:10.21105/astro.2305.06347 2023

  35. [37]

    Compressed ’CMB-lite’ Likelihoods Using Automatic Differentiation

    Balkenhol, L. Compressed ’CMB-lite’ Likelihoods Using Automatic Differentiation. 2025, The Open Journal of Astrophysics, 8, 17, doi:10.33232/001c.129886

    work page doi:10.33232/001c.129886 2025

  36. [38]

    J., et al

    Planck Collaboration, Akrami, Y., Andersen, K. J., et al. Planck intermediate results. LVII. Joint Planck LFI and HFI data processing. 2020, A&A, 643, A42, doi:10.1051/0004-6361/202038073

    work page doi:10.1051/0004-6361/202038073 2020

  37. [39]

    Planck 2018 results

    Planck Collaboration, Aghanim, N., Akrami, Y., et al. Planck 2018 results. I. Overview and the cosmological legacy of Planck. 2020, A&A, 641, A1, doi:10.1051/ 0004-6361/201833880

    work page 2018

  38. [40]

    Planck 2018 results

    —. Planck 2018 results. V. CMB power spectra and likelihoods. 2020, A&A, 641, A5, doi:10.1051/ 0004-6361/201936386

    work page 2018

  39. [41]

    CMB lensing from Planck PR4 maps

    Carron, J., Mirmelstein, M., & Lewis, A. CMB lensing from Planck PR4 maps. 2022, J. of Cosm. & Astropart. Phys., 2022, 039, doi:10.1088/1475-7516/2022/09/ 039

    work page doi:10.1088/1475-7516/2022/09/ 2022

  40. [42]

    J., Sherwin, B

    Qu, F. J., Sherwin, B. D., Madhavacheril, M. S., et al. The Atacama Cosmology Telescope: A Measurement of the DR6 CMB Lensing Power Spectrum and Its Implications for Structure Growth. 2024, Astrophys. J., 962, 112, doi:10.3847/1538-4357/acfe06

    work page doi:10.3847/1538-4357/acfe06 2024

  41. [44]

    Abbott, T. M. C., Aguena, M., Alarcon, A., et al. Dark Energy Survey Year 3 results: Cosmological constraints from galaxy clustering and weak lensing. 2022, Phys. Rev. D, 105, 023520, doi:10.1103/PhysRevD.105. 023520

    work page doi:10.1103/physrevd.105 2022

  42. [45]

    J., Ge, F., Wu, W

    Qu, F. J., Ge, F., Wu, W. L. K., et al. 2025, Unified and consistent structure growth measurements from joint ACT, SPT and {Planck} CMB lensing, arXiv, doi:10.48550/arXiv.2504.20038

    work page doi:10.48550/arxiv.2504.20038 2025

  43. [47]

    2024, TestingtheΛCDMCosmologicalModelwithForthcom- ingMeasurementsoftheCosmicMicrowaveBackground with SPT-3G, arXiv, doi:10.48550/ARXIV.2403.17925

    Prabhu, K., Raghunathan, S., Millea, M., et al. 2024, TestingtheΛCDMCosmologicalModelwithForthcom- ingMeasurementsoftheCosmicMicrowaveBackground with SPT-3G, arXiv, doi:10.48550/ARXIV.2403.17925

    work page doi:10.48550/arxiv.2403.17925 2024

  44. [48]

    ApJ , volume =

    Hivon, E., Górski, K. M., Netterfield, C. B., Crill, B. P., Prunet, S., & Hansen, F. MASTER of the Cosmic Microwave Background Anisotropy Power Spectrum: A Fast Method for Statistical Analysis of Large and Complex Cosmic Microwave Background Data Sets. 2002, Astrophys. J., 567, 2, doi:10.1086/338126

    work page doi:10.1086/338126 2002

  45. [49]

    E., et al

    Archipley, M., Hryciuk, A., Bleem, L. E., et al. 2025, Millimeter-wave observations of Euclid Deep Field South using the South Pole Telescope: A data release of temperature maps and catalogs, arXiv, doi:10.48550/ arXiv.2506.00298

    work page arXiv 2025

  46. [50]

    Filtering in CMB data analysis with application to ACT DR4 and Planck observations

    Rosenberg, E., Gratton, S., & Challinor, A. Filtering in CMB data analysis with application to ACT DR4 and Planck observations. 2025, Phys. Rev. D, 112, 023534, doi:10.1103/rvhm-fsdc

    work page doi:10.1103/rvhm-fsdc 2025

  47. [51]

    Mea- surements of Secondary Cosmic Microwave Background Anisotropies with the South Pole Telescope

    Lueker, M., Reichardt, C.L., Schaffer, K.K., etal. Mea- surements of Secondary Cosmic Microwave Background Anisotropies with the South Pole Telescope. 2010, Astrophys. J., 719, 1045, doi:10.1088/0004-637X/719/ 2/1045

    work page doi:10.1088/0004-637x/719/ 2010

  48. [52]

    Planck Collaboration, Adam, R., Ade, P. A. R., et al. Planck 2015 results. X. Diffuse component separation: Foreground maps. 2016, A&A, 594, A10, doi:10.1051/ 0004-6361/201525967

    work page 2015

  49. [53]

    AGORA: Multicomponent simulation for cross-survey science

    Omori, Y. AGORA: Multicomponent simulation for cross-survey science. 2024, MNRAS, 530, 5030, doi:10. 1093/mnras/stae1031

    work page 2024

  50. [54]

    CARPool: fast, accurate computation of large-scale structure statistics by pairing costly and cheap cosmological simulations

    Chartier, N., Wandelt, B., Akrami, Y., & Villaescusa- Navarro, F. CARPool: fast, accurate computation of large-scale structure statistics by pairing costly and cheap cosmological simulations. 2021, Monthly Notices of the Royal Astronomical Society, 503, 1897, doi:10. 1093/mnras/stab430

    work page 2021

  51. [55]

    2024, The Ata- cama Cosmology Telescope: Semi-Analytic Covariance Matrices for the DR6 CMB Power Spectra, arXiv, doi:10.48550/arXiv.2412.07068

    Atkins, Z., Li, Z., Alonso, D., et al. 2024, The Ata- cama Cosmology Telescope: Semi-Analytic Covariance Matrices for the DR6 CMB Power Spectra, arXiv, doi:10.48550/arXiv.2412.07068

    work page doi:10.48550/arxiv.2412.07068 2024

  52. [56]

    QuickPol: Fast calculation of effective beam matrices for CMB polarization

    Hivon, E., Mottet, S., & Ponthieu, N. QuickPol: Fast calculation of effective beam matrices for CMB polarization. 2017, Astronomy & Astrophysics, 598, A25, doi:10.1051/0004-6361/201629626

    work page doi:10.1051/0004-6361/201629626 2017

  53. [57]

    M., & Zaldarriaga, M

    Hu, W., Hedman, M. M., & Zaldarriaga, M. Benchmark parameters for CMB polarization experiments. 2003, Phys. Rev. D, 67, 043004, doi:10.1103/PhysRevD.67. 043004

    work page doi:10.1103/physrevd.67 2003

  54. [59]

    Constrained realizations of Gaussian fields - A simple algorithm

    Hoffman, Y., & Ribak, E. Constrained realizations of Gaussian fields - A simple algorithm. 1991, The Astrophysical Journal, 380, L5, doi:10.1086/186160

    work page doi:10.1086/186160 1991

  55. [60]

    B., & Pedersen, M

    Petersen, K. B., & Pedersen, M. S. 2012, The Matrix Cookbook, Technical University of Denmark.http:// www2.compute.dtu.dk/pubdb/pubs/3274-full.html

    work page 2012

  56. [61]

    Full-sky CMB lensing reconstruction in presence of sky-cuts

    Benoit-Lévy, A., Déchelette, T., Benabed, K., Cardoso, J.-F., Hanson, D., & Prunet, S. Full-sky CMB lensing reconstruction in presence of sky-cuts. 2013, A&A, 555, 81 A37, doi:10.1051/0004-6361/201321048

    work page doi:10.1051/0004-6361/201321048 2013

  57. [62]

    2012, MNRAS, 427, 127, doi: 10.1111/j.1365-2966.2012.21948.x

    Bucher, M., & Louis, T. Filling in cosmic microwave background map missing data using constrained Gaus- sian realizations: Filling in missing CMB data. 2012, MonthlyNoticesoftheRoyalAstronomicalSociety, 424, 1694, doi:10.1111/j.1365-2966.2012.21138.x

    work page doi:10.1111/j.1365-2966.2012.21138.x 2012

  58. [63]

    Planck Collaboration, Ade, P. A. R., Aghanim, N., Armitage-Caplan, C., Arnaud, M., Ashdown, M., Atrio- Barandela, F., Aumont, J., Baccigalupi, C., Banday, A. J., & et al. Planck 2013 results. XVII. Gravitational lensing by large-scale structure. 2014, A&A, 571, A17, doi:10.1051/0004-6361/201321543

    work page doi:10.1051/0004-6361/201321543 2013

  59. [64]

    A 2500 deg2 CMB Lensing Map from Combined South Pole Telescope and Planck Data

    Omori, Y., Chown, R., Simard, G., et al. A 2500 deg2 CMB Lensing Map from Combined South Pole Telescope and Planck Data. 2017, Astrophys. J., 849, 124, doi:10.3847/1538-4357/aa8d1d

    work page doi:10.3847/1538-4357/aa8d1d 2017

  60. [65]

    P., Bartlett, J

    Raghunathan, S., Holder, G. P., Bartlett, J. G., Patil, S., Reichardt, C. L., & Whitehorn, N. An inpainting approach to tackle the kinematic and thermal SZ induced biases in CMB-cluster lensing estimators. 2019, J. of Cosm. & Astropart. Phys., 2019, 037, doi:10. 1088/1475-7516/2019/11/037

    work page 2019

  61. [66]

    J., Chang, C., et al

    Omori, Y., Baxter, E. J., Chang, C., et al. Joint analysis of Dark Energy Survey Year 3 data and CMB lensing from SPT and Planck. I. Construction of CMB lensing maps and modeling choices. 2023, Phys. Rev. D, 107, 023529, doi:10.1103/PhysRevD.107.023529

    work page doi:10.1103/physrevd.107.023529 2023

  62. [67]

    candl: cosmic microwave background analysis with a differentiable likelihood

    Balkenhol, L., Trendafilova, C., Benabed, K., & Galli, S. candl: cosmic microwave background analysis with a differentiable likelihood. 2024, A&A, 686, A10, doi:10. 1051/0004-6361/202449432

    work page 2024

  63. [68]

    The Local Structure of Turbulence in Incompressible Viscous Fluid for Very Large Reynolds’ Numbers.1941, AkademiiaNaukSSSRDoklady, 30, 301

    Kolmogorov, A. The Local Structure of Turbulence in Incompressible Viscous Fluid for Very Large Reynolds’ Numbers.1941, AkademiiaNaukSSSRDoklady, 30, 301

    work page 1941

  64. [69]

    Non-Gaussian structure of the lensed CMB power spectra covariance matrix

    Benoit-Lévy, A., Smith, K.M., &Hu, W. Non-Gaussian structure of the lensed CMB power spectra covariance matrix. 2012, Phys. Rev. D, 86, 123008, doi:10.1103/ PhysRevD.86.123008

    work page 2012

  65. [70]

    C., Meyers, J., Trendafilova, C., Green, D., & Van Engelen, A

    Hotinli, S. C., Meyers, J., Trendafilova, C., Green, D., & Van Engelen, A. The benefits of CMB delensing. 2022, Journal of Cosmology and Astroparticle Physics, 2022, 020, doi:10.1088/1475-7516/2022/04/020

    work page doi:10.1088/1475-7516/2022/04/020 2022

  66. [71]

    L., Ade, P

    Chou, T. L., Ade, P. A. R., Anderson, A. J., et al. Mea- surements of the Temperature and E-mode Polarization of the Cosmic Microwave Background from the Full 500-square-degreeSPTpolDataset.2025, arXive-prints, arXiv:2501.06890, doi:10.48550/arXiv.2501.06890

    work page doi:10.48550/arxiv.2501.06890 2025

  67. [72]

    Terzo, et al., Novel 3D Pixel Sensors for the Upgrade of the ATLAS Inner Tracker, Front

    Gerbino, M., Lattanzi, M., Migliaccio, M., Pagano, L., Salvati, L., Colombo, L., Gruppuso, A., Natoli, P., & Polenta, G. Likelihood methods for CMB experiments. 2020, Frontiers in Physics, 8, 15, doi:10.3389/fphy. 2020.00015

    work page doi:10.3389/fphy 2020

  68. [73]

    Super-sample CMB lensing

    Manzotti, A., Hu, W., & Benoit-Lévy, A. Super-sample CMB lensing. 2014, Phys. Rev. D, 90, 023003, doi:10. 1103/PhysRevD.90.023003

    work page 2014

  69. [74]

    Effect of aberration on partial-sky measurements of the cosmic microwave background temperature power spectrum

    Jeong, D., Chluba, J., Dai, L., Kamionkowski, M., & Wang, X. Effect of aberration on partial-sky measurements of the cosmic microwave background temperature power spectrum. 2014, Phys. Rev. D, 89, 023003, doi:10.1103/PhysRevD.89.023003

    work page doi:10.1103/physrevd.89.023003 2014

  70. [75]

    Planck Collaboration, Ade, P. A. R., Aghanim, N., Armitage-Caplan, C., Arnaud, M., Ashdown, M., Atrio- Barandela, F., Aumont, J., Baccigalupi, C., Banday, A. J., & et al. Planck 2013 results. VII. HFI time responseandbeams.2014, A&A,571, A7, doi:10.1051/ 0004-6361/201321535

    work page 2013

  71. [76]

    Planck 2013 results

    —. Planck 2013 results. XV. CMB power spectra and likelihood. 2014, A&A, 571, A15, doi:10.1051/ 0004-6361/201321573

    work page 2013

  72. [77]

    W., Sayre, J

    Henning, J. W., Sayre, J. T., Reichardt, C. L., et al. Measurements of the Temperature and E-mode Polarization of the CMB from 500 Square Degrees of SPTpol Data. 2018, Astrophys. J., 852, 97, doi:10. 3847/1538-4357/aa9ff4

    work page 2018

  73. [78]

    Galli, S., Wu, W. L. K., Benabed, K., Bouchet, F., Crawford, T. M., & Hivon, E. Breaking the degen- eracy between polarization efficiency and cosmological parameters in CMB experiments. 2021, Phys. Rev. D, 104, 023518, doi:10.1103/PhysRevD.104.023518

    work page doi:10.1103/physrevd.104.023518 2021

  74. [79]

    Modeling Extragalactic Foregrounds and Secondaries for Un- biased Estimation of Cosmological Parameters from Primary Cosmic Microwave Background Anisotropy

    Millea, M., Doré, O., Dudley, J., Holder, G., Knox, L., Shaw, L., Song, Y.-S., & Zahn, O. Modeling Extragalactic Foregrounds and Secondaries for Un- biased Estimation of Cosmological Parameters from Primary Cosmic Microwave Background Anisotropy. 2012, Astrophys. J., 746, 4, doi:10.1088/0004-637X/ 746/1/4

    work page doi:10.1088/0004-637x/ 2012

  75. [80]

    Aghanim, et al., Astron

    Planck Collaboration, Akrami, Y., Ashdown, M., et al. Planck 2018 results. IV. Diffuse component separa- tion. 2020, A&A, 641, A4, doi:10.1051/0004-6361/ 201833881

    work page doi:10.1051/0004-6361/ 2018

  76. [81]

    M., Reichardt, C

    George, E. M., Reichardt, C. L., Aird, K. A., et al. A Measurement of Secondary Cosmic Microwave Back- ground Anisotropies from the 2500-Square-degree SPT- SZ Survey. 2015, Astrophys. J., 799, 177, doi:10.1088/ 0004-637X/799/2/177

    work page 2015

  77. [82]

    The Atacama Cosmology Telescope: likelihood for small- scale CMB data

    Dunkley, J., Calabrese, E., Sievers, J., et al. The Atacama Cosmology Telescope: likelihood for small- scale CMB data. 2013, J. of Cosm. & Astropart. Phys., 7, 25, doi:10.1088/1475-7516/2013/07/025

    work page doi:10.1088/1475-7516/2013/07/025 2013

  78. [83]

    Mak, D. S. Y., Challinor, A., Efstathiou, G., & Lagache, G. Measurement of CIB power spectra over large sky areas from Planck HFI maps. 2017, Monthly Notices of the Royal Astronomical Society, 466, 286, doi:10.1093/ mnras/stw3112

    work page 2017

  79. [84]

    L., Patil, S., Ade, P

    Reichardt, C. L., Patil, S., Ade, P. A. R., et al. An Improved Measurement of the Secondary Cosmic Microwave Background Anisotropies from the SPT- SZ + SPTpol Surveys. 2021, Astrophys. J., 908, 199, doi:10.3847/1538-4357/abd407

    work page doi:10.3847/1538-4357/abd407 2021

  80. [85]

    D., Nagai, D., Bhattacharya, S., & Lau, E

    Shaw, L. D., Nagai, D., Bhattacharya, S., & Lau, E. T. Impact of Cluster Physics on the Sunyaev- Zel’dovich Power Spectrum. 2010, Astrophys. J., 725, 1452, doi:10.1088/0004-637X/725/2/1452

    work page doi:10.1088/0004-637x/725/2/1452 2010

Showing first 80 references.