The influence of the effective number of active and sterile neutrinos on the determination of the values of cosmological parameters

TL;DR

This paper investigates how active and sterile neutrinos influence the estimation of cosmological parameters, particularly the Hubble constant, and explores their role in addressing the H0 tension within the ΛCDM model.

Contribution

It introduces a detailed analysis of sterile neutrino effects on cosmological parameters and their potential to resolve the H0 tension problem.

Findings

Sterile neutrinos with 1 and 2.7 eV masses decrease H0 estimates.

Increasing N_eff raises H0, helping resolve the H0 tension.

Most other cosmological parameters remain consistent with ΛCDM.

Abstract

In the presented work we consider the influence of a hypothetical sterile neutrino (with eV-scale mass) on the determination of cosmological parameters. If it is detected, it will be necessary to include it into the $\Lambda \rm CDM$ model with the fixed values of its mass $m_{\rm s}$ and mixing angle $\theta_{s}$, which is the main method used through this paper. Apart from that, the seesaw mechanism requires there to be at least two sterile states, one of them being much heavier than the active ones. The heavier sterile state ($m_{s}\sim1$ keV) would decay and increase the effective number of active neutrinos. Therefore, the influence of a change in the effective number of relativistic neutrino species $N_{\rm eff}$ was studied as well, which could be caused by, for example, the decay processes of the above-mentioned sterile neutrinos, as well as processes leading to an increase in the temperature of relic neutrinos $T_{\rm C\nu B}$. The effects studied in this work lead to a significant change in the estimates of the cosmological parameters, including the value of $H_{0}$. It has been discovered that the accounting of the sterile neutrino with masses $m=1$ and $2.7$ eV leads to a decrease in the estimate of the current Hubble parameter value $H_{0}$ and, therefore, exacerbates the ``$H_{0}$-tension'' problem. An increase in the value of the effective number of relativistic neutrino species leads, on the contrary, to an increase in the $H_{0}$ estimate, resolving the above-mentioned problem at $N_{\rm eff}=3.0+0.9$, which is equivalent to an increase of the neutrino temperature up to $T ^{\,0}_{\rm C\nu B}=1.95+0.14\,\rm K$. At the same time, the rest of the cosmological parameters do not change significantly, leaving us within the framework of the standard $\Lambda \rm CDM$ model.