Thawing quintessence from the inflationary epoch to today

Abstract

Using the latest observational data we obtain a lower bound on the initial value of the quintessence field in thawing quintessence models of dark energy. For potentials of the form V(ϕ) ϕ^{\pm2} we find that the initial value |ϕ_i|>7x10^{18}\gev. We then relate ϕ_i to the duration of inflation by assuming that the initial value of the quintessence field is determined by quantum fluctuations of the quintessence field during inflation. From the lower bound on ${\varphi }_i$ we obtain a lower bound on the number of e-foldings of inflation, namely, N>2x10^{11}. We obtain similar bounds for other power law potentials for which too we obtain |ϕ_{i}|>O(M_{P}.

8 pages, 5 figures; replaced some figures and expanded discussion to include general monomial potentials. Accepted for publication in Physical Review D

References in corpus (4)

• Dynamics of dark energy
• Eternal inflation and its implications
• Thawing quintessence with a nearly flat potential
• How Many $e$-Folds Should We Expect from High-Scale Inflation?

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• Observational constraints on quintessence models of dark energy
• The BAHAMAS project: Effects of dynamical dark energy on large-scale structure
• One-point probability distribution function from spherical collapse: Early Dark Energy (EDE) vs. $\Lambda$CDM
• Dynamical evolution of quintessence cosmology in a physical phase space
• Discerning Dark Energy Models with High-Redshift Standard Candles
• Pure Natural Quintessential Inflation and Dark Energy