Cosmological Constraints on Neutrino Masses in Quintessential Inflation

TL;DR

This paper investigates how quintessential inflation models can tighten cosmological constraints on neutrino masses by breaking degeneracies, using current data and forecasting future observational improvements.

Contribution

It introduces a unified inflation-dark energy model that constrains neutrino masses more tightly than previous models, incorporating curvature effects and future observational forecasts.

Findings

Upper bounds on neutrino masses: < 0.067 eV (flat) and < 0.116 eV (curved)

Future experiments may reduce neutrino mass uncertainty by about 9%

Significant improvement in constraining the quintessential parameter lpha_{QI} by 72%

Abstract

Quintessential inflation provides a unified description of the early and late accelerated phases of the Universe, linking the inflationary epoch to the present-day dark energy-dominated era through a single scalar degree of freedom. In this work, we explore the implications of this unification for cosmological constraints on the sum of neutrino masses. Focusing on the $\alpha$-attractor scenario, we implement the model in a modified version of the Boltzmann solver CLASS to compute the relevant cosmological observables and perform a Bayesian parameter estimation analysis using data from the cosmic microwave background (CMB), baryon acoustic oscillations (BAOs), and Type Ia supernovae. The model naturally breaks the degeneracy between the dark energy equation of state and the total neutrino mass, yielding tight upper bounds of $\sum m_\nu< 0.067$ eV for flat spatial geometry and $\sum m_\nu< 0.116$ eV when curvature is included. We also provide forecasts for future probes, showing that the Simons Observatory, LiteBIRD, and Euclid configurations may reduce the uncertainty on $\sum m_\nu$ by $\approx 9\%$, while the precision on the quintessential parameter $\alpha_{QI}$ is improved by $\approx 72\%$. These results highlight the importance of consistently accounting for neutrino mass when assessing the viability of extensions to the standard cosmological model.