Cosmological implications of $n_s\approx 1$ in light of the Hubble tension

Fuminobu Takahashi; Wen Yin

doi:10.1016/j.physletb.2022.137143

paper

Cosmological implications of $n_{s} \approx 1$ in light of the Hubble tension

arXiv:2112.06710 · doi:10.1016/j.physletb.2022.137143

Abstract

Recently, a low- $z$ measurement of the Hubble constant, $H_{0} = 73.04 \pm 1.04 km/s/Mpc$ , was reported by the SH0ES Team. The long-standing Hubble tension, i.e. the difference between the Hubble constant from the local measurements and that inferred from the cosmic microwave background data based on the $Λ$ CDM model, was further strengthened. There are many cosmological models modifying the cosmology after and around the recombination era to alleviate this tension. In fact, some of the models alter the small-scale fluctuation amplitude relative to larger scales, and thus require a significant modification of the primordial density perturbation, especially the scalar spectral index, $n_{s}$ . In certain promising models, $n_{s}$ is favored to be larger than the $Λ$ CDM prediction, and even the scale-invariant one, $n_{s} = 1$ , is allowed. In this Letter, we focus on the very early Universe models to study the implication of such unusual $n_{s}$ . In particular, we find that an axiverse with an axion in the equilibrium distribution during inflation can be easily consistent with $n_{s} = 1$ . This is because the axion behaves as a curvaton with mass much smaller than the inflationary Hubble parameter. We also discuss other explanations of $n_{s}$ different from that obtained based on the $Λ$ CDM.

arXiv comment17pages, 1 figure

Cosmological implications of $n_{s} \approx 1$ in light of the Hubble tension

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Cosmological implications of $n_{s} \approx 1$ in light of the Hubble tension