A new derivation of the Hubble constant from ${\hat{I}}^3$-ray attenuation using improved optical depths for the Fermi and CTA era

Abstract

We present ${\hat{I}}^3$-ray optical-depth calculations from a recently published extragalactic background light (EBL) model built from multiwavelength galaxy data from the Hubble Space Telescope Cosmic Assembly Near-Infrared Deep Extragalactic Legacy Survey (HST/CANDELS). CANDELS gathers one of the deepest and most complete observations of stellar and dust emissions in galaxies. This model resulted in a robust derivation of the evolving EBL spectral energy distribution up to $z\sim 6$, including the far-infrared peak. Therefore, the optical depths derived from this model will be useful for determining the attenuation of ${\hat{I}}^3$-ray photons coming from high-redshift sources, such as those detected by the Large Area Telescope on board the Fermi Gamma-ray Space Telescope, and for multi-TeV photons that will be detected from nearby sources by the future Cherenkov Telescope Array. From these newly calculated optical depths, we derive the cosmic ${\hat{I}}^3$-ray horizon and also measure the expansion rate and matter content of the Universe including an assessment of the impact of the EBL uncertainties. We find $H_0=61.9$ ${}_{-2.4}^{+2.9}$ km s${}^{-1}$ Mpc${}^{-1}$ when fixing $\hat{I}{\text{c◯}}_m=0.32$, and $H_0=65.6$ ${}_{-5.0}^{+5.6}$ km s${}^{-1}$ Mpc${}^{-1}$ and $\hat{I}{\text{c◯}}_m=0.19\pm 0.07$, when exploring these two parameters simultaneously.

11 pages, 8 figures, 1 tables; Accepted by MNRAS