Ruling Out Dark Energy Model induced by de-Sitter Regions of Non-Singular Black Holes with Planck2018, DESI BAO, and Union3 Supernovae

Abstract

Dark energy(DE) remains one of the most important subjects in modern cosmology, and its physical origin is still under intensive discussion. While an astrophysical origin of DE is a highly challenging scenario, black holes stand out the most promising candidates as the astrophysical origin. In this paper, we explore a new model of DE induced by black holes, in which cosmic accelerated expansion caused by de-Sitter like space-time regions around the non-singular black holes. It is difficult to examine such a phenomena by measuring black hole mass because the energy density of the cosmological constant is much smaller than the mass density of a black hole near a black hole. On the other hand, this modification becomes dominant on the cosmological scale. Therefore, we focus on the cosmological probes and perform the MCMC analysis using Planck2018+DESI DR2+Supernovae. Since the total amount of DE density depends on the contributions of all black holes, we use the simulated results for the evolution of the number of black holes. As a result, we obtain the best-fitted total chi-squared value, $\chi_\mathrm{total}^2 = 2871.13$ compared to $\Lambda \mathrm{CDM}$ case $\chi_\mathrm{total, \, \Lambda CDM}^2 = 2819.00$, and $\Delta \chi^2 \sim 50$. We conclude that this $\Delta \chi^2$ is enough large to rule out this model, because the number of parameters is same between this model and $\Lambda \mathrm{CDM}$.