The Cosmological Perturbation Theory on the Geodesic Light-Cone background

TL;DR

This paper develops a cosmological perturbation theory based on the Geodesic Light-Cone gauge, providing a new framework that simplifies the calculation of light-like observables and connects with standard perturbation approaches.

Contribution

It introduces a perturbation theory on the GLC background, linking it to standard gauge choices and constructing gauge-invariant variables aligned with GLC properties.

Findings

Derived gauge-invariant expressions for light-like observables.

Established correspondence between GLC gauge and standard perturbation gauges.

Applied framework to linearized angular distance-redshift relation.

Abstract

Inspired by the fully non-linear Geodesic Light-Cone (GLC) gauge, we consider its analogous set of coordinates which describes the unperturbed Universe. Given this starting point, we then build a cosmological perturbation theory on top of it, study the gauge transformation properties related to this new set of perturbations and show the connection with standard cosmological perturbation theory. In particular, we obtain which gauge in standard perturbation theory corresponds to the GLC gauge, and put in evidence how this is a useful alternative to the standard Synchronous Gauge. Moreover, we exploit several viable definitions for gauge invariant combinations. Among others, we build the gauge invariant variables such that their values equal the ones of linearized GLC gauge perturbations. This choice is motivated by two crucial properties of the GLC gauge: i) it admits simple expressions for light-like observables, e.g. redshift and angular distance, at fully non-linear level and ii) the GLC proper time coincides with the one of a free-falling observer. Thanks to the first property, exact expressions can then be easily expanded at linear order to obtain linear gauge invariant expression for the chosen observable. Moreover, the second feature naturally provides gauge invariant expressions for physical observables in terms of the time as measured by such free-falling observer. Finally, we explicitly show all these aspects for the case of the linearized angular distance-redshift relation.