Early Dark Energy During Big Bang Nucleosynthesis

TL;DR

This paper investigates how an early dark energy component during Big Bang Nucleosynthesis affects elemental abundances and relativistic degrees of freedom, using observational data to constrain model parameters and address helium abundance tensions.

Contribution

It introduces a simple model of early dark energy with a transition to different components and analyzes its effects on BBN and CMB observables, providing new constraints on EDE parameters.

Findings

Constraints on EDE parameters from observed abundances and $N_{eff}$

Correlation between EDE parameters and BBN inputs

Potential to alleviate primordial helium abundance tension

Abstract

We study the impact of an early dark energy component (EDE) present during big bang nucleosynthesis (BBN) on the elemental abundances of deuterium D/H, and helium $Y_p$, as well as the effective relativistic degrees of freedom $N_{\rm eff}$. We consider a simple model of EDE that is constant up to a critical time. After this critical time, the EDE transitions into either a radiation component that interacts with the electromagnetic plasma, a dark radiation component that is uncoupled from the plasma, or kination that is also uncoupled. We use measured values of the abundances and $N_{\rm eff}$ as determined by CMB observations to establish limits on the input parameters of this EDE model. In addition, we explore how those parameters are correlated with BBN inputs; the baryon to photon ratio $\eta_b$, neutron lifetime $\tau_n$, and number of neutrinos $N_\nu$. Finally, we study whether this setup can alleviate the tension introduced by recent measurements of the primordial helium abundance.