Observational signatures of a non-singular bouncing cosmology

TL;DR

This paper explores a bouncing cosmology model where a non-singular bounce precedes inflation, analyzing how perturbations evolve through the bounce and impact observable cosmic microwave background and matter spectra.

Contribution

It provides a detailed analysis of perturbation transfer through a symmetric bounce and predicts observable oscillations in primordial spectra due to the bounce's effects.

Findings

Perturbations are in an excited state at the start of inflation.

Oscillations are superimposed on the primordial spectra.

Potential observational signatures in CMB and matter power spectrum.

Abstract

We study a cosmological scenario in which inflation is preceded by a bounce. In this scenario, the primordial singularity, one of the major shortcomings of inflation, is replaced by a non-singular bounce, prior to which the universe undergoes a phase of contraction. Our starting point is the bouncing cosmology investigated in Falciano et al. (2008), which we complete by a detailed study of the transfer of cosmological perturbations through the bounce and a discussion of possible observational effects of bouncing cosmologies. We focus on a symmetric bounce and compute the evolution of cosmological perturbations during the contracting, bouncing and inflationary phases. We derive an expression for the Mukhanov-Sasaki perturbation variable at the onset of the inflationary phase that follows the bounce. Rather than being in the Bunch-Davies vacuum, it is found to be in an excited state that depends on the time scale of the bounce. We then show that this induces oscillations superimposed on the nearly scale-invariant primordial spectra for scalar and tensor perturbations. We discuss the effects of these oscillations in the cosmic microwave background and in the matter power spectrum. We propose a new way to indirectly measure the spatial curvature energy density parameter in the context of this model.