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Many theoretical resolutions to the so-called "Hubble tension" rely onmodifying the sound horizon at recombination, $r_s$, and thus the acousticscale used as a standard ruler in the cosmic microwave background (CMB) andlarge scale structure (LSS) datasets. As shown in a number of recent works,these observables can also be used to compute $r_s$-independent constraints on$H_0$ by making use of the horizon scale at matter-radiation equality, $k_{\rmeq}$, which has different sensitivity to high redshift physics than $r_s$. Assuch, $r_s$- and $k_{\rm eq}$-based measurements of $H_0$ (within a$\Lambda$CDM framework) may differ if there is new physics presentpre-recombination. In this work, we present the tightest constraints on thelatter from current data, finding $H_0=64.8^{+2.2}_{-2.5}$ at 68% CL (in$\mathrm{km}\,\mathrm{s}^{-1}\mathrm{Mpc}^{-1}$ units) from a combination ofBOSS galaxy power spectra, Planck CMB lensing, and the newly released Pantheon+supernova constraints, as well as physical priors on the baryon density,neutrino mass, and spectral index. The BOSS and Planck measurements havedifferent degeneracy directions, leading to the improved combined constraints,with a bound of $H_0 = 67.1^{+2.5}_{-2.9}$ ($63.6^{+2.9}_{-3.6}$) from BOSS(Planck) alone. The results show some dependence on the neutrino mass bounds,with the constraint broadening to $H_0 = 68.0^{+2.9}_{-3.2}$ if we insteadimpose a weak prior on $\sum m_\nu$ from terrestrial experiments, or shiftingto $H_0 = 64.6\pm2.4$ if the neutrino mass is fixed to its minimal value. Evenwithout dependence on the sound horizon, our results are in $\approx 3\sigma$tension with those obtained from the Cepheid-calibrated distance ladder, whichbegins to cause problems for new physics models that vary $H_0$ by changingacoustic physics or the expansion history immediately prior to recombination.

Determining the Hubble Constant without the Sound Horizon: A $3.6\%$ Constraint on $H_0$ from Galaxy Surveys, CMB Lensing and Supernovae