Fluctuations in a Cosmology with a Space-Like Singularity and their Gauge Theory Dual Description

TL;DR

This paper explores how cosmological fluctuations evolve through a space-like singularity using the AdS/CFT correspondence, revealing that the spectral index remains unchanged while the amplitude increases, providing insights into quantum gravity effects.

Contribution

It demonstrates a method to track scalar field fluctuations across a cosmological singularity via boundary gauge theory, extending the AdS/CFT framework to time-dependent, singular spacetimes.

Findings

Spectral index remains unchanged after the singularity.

Fluctuation amplitude increases due to squeezing during evolution.

Boundary theory allows extension of bulk perturbations beyond the singularity.

Abstract

We consider a time-dependent deformation of anti-de-Sitter (AdS) space-time which contains a cosmological "singularity" - a space-like region of high curvature. Making use of the AdS/CFT correspondence we can map the bulk dynamics onto the boundary. The boundary theory has a time dependent coupling constant which becomes small at times when the bulk space-time is highly curved. We investigate the propagation of small fluctuations of a test scalar field from early times before the bulk singularity to late times after the singularity. Under the assumption that the AdS/CFT correspondence extends to deformed AdS space-times, we can map the bulk evolution of the scalar field onto the evolution of the boundary gauge field. The time evolution of linearized fluctuations is well defined in the boundary theory as long as the coupling remains finite, so that we can extend the boundary perturbations to late times after the singularity. Assuming that the spacetime in the future of the singularity has a weakly coupled region near the boundary, we reconstruct the bulk fluctuations after the singularity crossing making use of generic properties of boundary-to-bulk propagators. Finally, we extract the spectrum of the fluctuations at late times given some initial spectrum. We find that the spectral index is unchanged, but the amplitude increases due to the squeezing of the fluctuations during the course of the evolution. This investigation can teach us important lessons on how the spectrum of cosmological perturbations passes through a bounce which is singular from the bulk point of view but which is resolved using an ultraviolet complete theory of quantum gravity.