Cosmic microwave background and large-scale structure constraints on a simple quintessential inflation model

Abstract

We derive constraints on a simple quintessential inflation model, based on a spontaneously broken 4 theory, imposed by the Wilkinson Microwave Anisotropy Probe three-year data (WMAP3) and by galaxy clustering results from the Sloan Digital Sky Survey (SDSS). We find that the scale of symmetry breaking must be larger than about 3 Planck masses in order for inflation to generate acceptable values of the scalar spectral index and of the tensor-to-scalar ratio. We also show that the resulting quintessence equation of state can evolve rapidly at recent times and hence can potentially be distinguished from a simple cosmological constant in this parameter regime.

Quintessential inflation with canonical and noncanonical scalar fields and Planck 2015 results

“…It is clear from the aforesaid that (49) can give rise to a viable model of quintessential inflation by adding a nonminimal coupling between the scalar field and the neutrinos described in subsection II B. In the following subsection we shall describe inflation using the noncanonical model (49), and we will derive constraints on the model parameters in the light of Planck 2015 results [27,28]. Finally, in a separate subsection we will examine the latetime, post-inflationary evolution.…”

The dynamics of quintessence, the quintessence of dynamics

“…For more on PNGB models, see Frieman et al (1995); Kaloper & Sorbo (2006); Rosenfeld & Frieman (2006). These have fields starting frozen on their 1 + cos(φ/f ) potential and, after the Hubble drag diminishes, are released to roll.…”

“…The second parameterization w ′ = F (1 + w) is motivated by PNGB models, and is an excellent approximation to their dynamics (Caldwell & Linder, 2005), with F inversely proportional to the symmetry breaking energy scale f . For more on PNGB models, see Frieman et al (1995); Kaloper & Sorbo (2006); Rosenfeld & Frieman (2006). These have fields starting frozen on their 1 + cos(φ/f ) potential and, after the Hubble drag diminishes, are released to roll.…”

Unified early and late Universe cosmology through dissipative effects in steep quintessential inflation potential models

“…In the present work, we propose a model implementing a typical quintessential inflation behavior, i.e., through a scalar field model that can play both the roles of the inflaton and the dark energy (in the form of a dynamical scalar-quintessence field), in the early and late cosmology histories of the Universe, respectively. Quintessential inflation models are abundant in the literature [16][17][18][19][20][21][22][23][24][25].…”