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The Hubble Tension in Light of the Full-Shape Analysis of Large-Scale Structure Data

Guido D'Amico, Leonardo Senatore, Pierre Zhang, Henry Zheng

TL;DR

This paper tests whether full-shape analyses of large-scale structure, via the EFTofLSS framework, can resolve the Hubble tension by introducing early-universe physics in the form of Early Dark Energy or Rock 'n' Roll. By combining BOSS full-shape data with Planck+BAO+SN, the authors show that FS information breaks key parameter degeneracies (notably between the sound horizon $r_s$ and $H_0$), forcing the proposed models to align with ΛCDM predictions in many respects. When SH0ES $H_0$ data are included, both EDE and RnR yield only modest improvements, with residual tension persisting (typically around a few sigma) and no large gain in fit quality. The results imply that FS-LSS constraints strongly limit early-universe modifications as a solution to the $H_0$ tension, underscoring the need for alternative explanations or data to achieve concordance. Key finding: the combination of FS information and CMB data locks $r_s$ close to the ΛCDM value, constraining the room to raise $H_0$ without spoiling the observed large-scale structure.

Abstract

The disagreement between direct late-time measurements of the Hubble constant from the SH0ES collaboration, and early-universe measurements based on the $Λ$CDM model from the Planck collaboration might, at least in principle, be explained by new physics in the early universe. Recently, the application of the Effective Field Theory of Large-Scale Structure to the full shape of the power spectrum of the SDSS/BOSS data has revealed a new, rather powerful, way to measure the Hubble constant and the other cosmological parameters from Large-Scale Structure surveys. In light of this, we analyze two models for early universe physics, Early Dark Energy and Rock 'n' Roll, that were designed to significantly ameliorate the Hubble tension. Upon including the information from the full shape to the Planck, BAO, and Supernovae measurements, we find that the degeneracies in the cosmological parameters that were introduced by these models are well broken by the data, so that these two models do not significantly ameliorate the tension.

The Hubble Tension in Light of the Full-Shape Analysis of Large-Scale Structure Data

TL;DR

This paper tests whether full-shape analyses of large-scale structure, via the EFTofLSS framework, can resolve the Hubble tension by introducing early-universe physics in the form of Early Dark Energy or Rock 'n' Roll. By combining BOSS full-shape data with Planck+BAO+SN, the authors show that FS information breaks key parameter degeneracies (notably between the sound horizon and ), forcing the proposed models to align with ΛCDM predictions in many respects. When SH0ES data are included, both EDE and RnR yield only modest improvements, with residual tension persisting (typically around a few sigma) and no large gain in fit quality. The results imply that FS-LSS constraints strongly limit early-universe modifications as a solution to the tension, underscoring the need for alternative explanations or data to achieve concordance. Key finding: the combination of FS information and CMB data locks close to the ΛCDM value, constraining the room to raise without spoiling the observed large-scale structure.

Abstract

The disagreement between direct late-time measurements of the Hubble constant from the SH0ES collaboration, and early-universe measurements based on the CDM model from the Planck collaboration might, at least in principle, be explained by new physics in the early universe. Recently, the application of the Effective Field Theory of Large-Scale Structure to the full shape of the power spectrum of the SDSS/BOSS data has revealed a new, rather powerful, way to measure the Hubble constant and the other cosmological parameters from Large-Scale Structure surveys. In light of this, we analyze two models for early universe physics, Early Dark Energy and Rock 'n' Roll, that were designed to significantly ameliorate the Hubble tension. Upon including the information from the full shape to the Planck, BAO, and Supernovae measurements, we find that the degeneracies in the cosmological parameters that were introduced by these models are well broken by the data, so that these two models do not significantly ameliorate the tension.

Paper Structure

This paper contains 19 sections, 16 equations, 9 figures, 4 tables.

Table of Contents

  1. Introduction and Summary
  2. The EFTofLSS:
  3. The Hubble Tension:
  4. Data Sets:
  5. Main Results:
  6. Future directions:
  7. Codes:
  8. Mini-review of Models
  9. Physical Considerations
  10. (Axion) Early Dark Energy
  11. Rock 'n' Roll
  12. Data Analysis
  13. RnR Analysis
  14. EDE Analysis
  15. Shift of the Sound Horizon
  16. ...and 4 more sections

Figures (9)

  • Figure 1: One dimensional and two dimensional posterior distributions of some of the parameters of the RnR model analyzed with several combinations of data sets: Planck+BAO+Pantheon, Planck+FS+BAO+Pantheon, Planck+BAO+Pantheon+SH0ES and Planck+FS+BAO+SN+SH0ES.
  • Figure 2: One dimensional and two dimensional posterior distributions of some of the parameters of the EDE model analyzed with several combinations of data sets: Planck+BAO+Pantheon, Planck+FS+BAO+Pantheon, Planck+BAO+Pantheon+SH0ES and Planck+FS+BAO+SN+SH0ES. Here we define $\theta_{i, scf} = \theta_i$ and $CC_{scf} = V_{\Lambda}$.
  • Figure 3: Plots of the sound horizon $r_s$, angular diameter distance to recombination $D_A$, $H_0$ and $\omega_{cdm}$ for the four different dataset combinations analyzed. Left: RnR model. Right: EDE model.
  • Figure 4: Plots of the cosmological parameters in the three models for the Planck+BAO+SN dataset.
  • Figure 5: Plots of the cosmological parameters in the three models for the Planck+FS+BAO+SN dataset.
  • ...and 4 more figures