Early dark energy, the Hubble-parameter tension, and the string axiverse

TL;DR

This paper investigates whether early dark energy, inspired by string axiverse scenarios, can resolve the Hubble tension by increasing the early universe's expansion rate, but finds tight constraints limit its effectiveness.

Contribution

It introduces a model of early dark energy that decays rapidly and assesses its impact on the Hubble tension within current observational constraints.

Findings

Early dark energy can shift H0 by at most 1.6 km/s/Mpc under current bounds.

Planck data tightly constrains early dark energy contribution to less than 2% at recombination.

Resolving the Hubble tension with early dark energy requires reionization optical depth to be significantly higher than Planck bounds.

Abstract

Precise measurements of the cosmic microwave background (CMB) power spectrum are in excellent agreement with the predictions of the standard $\Lambda$CDM cosmological model. However, there is some tension between the value of the Hubble parameter $H_0$ inferred from the CMB and that inferred from observations of the Universe at lower redshifts, and the unusually small value of the dark-energy density is a puzzling ingredient of the model. In this paper, we explore a scenario with a new exotic energy density that behaves like a cosmological constant at early times and then decays quickly at some critical redshift $z_c$. An exotic energy density like this is motivated by some string-axiverse-inspired scenarios for dark energy. By increasing the expansion rate at early times, the very precisely determined angular scale of the sound horizon at decoupling can be preserved with a larger Hubble constant. We find, however, that the Planck temperature power spectrum tightly constrains the magnitude of the early dark-energy density and thus any shift in the Hubble constant obtained from the CMB. If the reionization optical depth is required to be smaller than the Planck 2016 $2\sigma$ upper bound $\tau\lesssim 0.0774$, then early dark energy allows a Hubble-parameter shift of at most 1.6 km~s$^{-1}$~Mpc$^{-1}$ (at $z_c\simeq 1585$), too small to fully alleviate the Hubble-parameter tension. Only if $\tau$ is increased by more than $5\sigma$ can the CMB Hubble parameter be brought into agreement with that from local measurements. In the process, we derive strong constraints to the contribution of early dark energy at the time of recombination---it can never exceed $\sim2\%$ of the radiation/matter density for $10 \lesssim z_c \lesssim 10^5$.