A sound horizon independent measurement of $H_0$ from BOSS, DESI and DES Y3

Abstract

We present a sound horizon independent measurement of the Hubble parameter using a multiprobe large-scale structure analysis. Removing the dependency on the sound horizon with a rescaling procedure at the matter power spectrum level, we analyse the BOSS full-shape power spectrum and bispectrum (for the first time) using the effective field theory of large-scale structure up to one loop. We combine this analysis with the auto- and cross-angular power spectra from the DESI Legacy Imaging Survey DR9, the $3 \times 2$pt analysis from DES Y3, and the CMB gravitational lensing power spectrum from Planck PR3. Our baseline analysis, that does not rely on supernovae data, yields $h = 0.702^{+0.022}_{-0.024}$, $Ω_m = 0.310 \pm 0.013$, and $σ_8 = 0.799 \pm 0.020$, corresponding to $3-4 \%$ precision measurements. When adding supernovae data from Pantheon+, we obtain a $2.6 \%$ measurement of $h$, with $h = 0.686 \pm 0.018$. We further note that our EFTBOSS analysis indicates a slight deviation of the BAO scale parameter (at $1.8 σ$) from its $Λ$CDM value, caused by the small scales of the bispectrum. We finally use the sound horizon-free EFTBOSS analysis as a diagnosis for the presence of new physics, finding that our results are consistent with the recent hints of evolving dark energy.

Figures (6)

• Figure 1: Summary of recent sound horizon-free determinations of the Hubble parameter $H_0$. In this plot, BAO data are always treated in a sound horizon-agnostic way, while "$n_s$", "$A_s$" and "$S_8$" indicate that Gaussian priors are imposed on these parameters (which are not necessarily the same for all analyses). The shaded bands denote the $1\sigma$ and $2\sigma$ regions from PlanckPlanck:2018vyg (in pink) and SH0ES Riess:2021jrx (in grey).
• Figure 2: Top left -- 2D posterior distributions from the individual sound horizon-free likelihoods considered in this work, with $\omega_b$ and $n_s$ fixed. Top right -- 2D posterior distributions from several EFTBOSS configurations. Bottom left -- 2D posterior distributions from several sound horizon-free likelihood combinations, using the prior on $n_s$ and $\omega_b$ defined in Sec. \ref{['sec:data']}. Bottom right -- 2D posterior distributions from several combinations between our baseline analysis, Pantheon+ and DESI DR2 BAO. In all panels, the dashed lines correspond to the Planck mean values from TTTEEE + Lensing Planck:2018vyg.
• Figure 3: 1D posterior distributions of $\{h, \, \Omega_m, \, \sigma_8, \, \alpha_{r_s} \}$ from the EFTBOSS 2+3pt analysis for several maximum bispectrum scales $k_{\rm max}^B$. We display the constraints of the analysis with (in green) and without (in black) the marginalization on the sound horizon.
• Figure 4: 2D posterior distributions from the full dataset, namely Lensing + EFTBOSS (2+3pt) + DESI$C_\ell$ + EFTDES + PanPlus + $\Omega_m^{\rm DESIDR2BAO}$, for the $\alpha_{r_s}$-free and $\alpha_{r_s}$-fix analyses. For comparison, we display the posteriors from PlanckPlanck:2018vyg in red and the SH0ES constraint on $H_0$Riess:2021jrx in grey shaded bands.
• Figure 5: 2D posterior distributions from the $\Lambda$CDM fit to the EFTBOSS 2+3pt mock data generated with the early dark energy cosmology (left panel) and evolving dark energy cosmology (right panel) displayed in Tab. \ref{['table:mock_cosmology']}. The fiducial cosmologies are shown in dashed lines. We show the reconstructed parameters from both the $\alpha_{r_s}$-free and the $\alpha_{r_s}$-fix analyses, with the two values of $k^B_{\rm max}$ considered in this work, fixing $n_s = 0.965$ and $\omega_b = 0.02235$.