Cutting out the cosmological middle man: General Relativity in the light-cone coordinates

TL;DR

This paper introduces a novel light-cone coordinate system for relativistic cosmology that simplifies the computation of observables by directly relating initial conditions to observations, bypassing traditional intermediate steps.

Contribution

The authors develop and detail a new light-cone coordinate framework, extending existing methods, and formulate Einstein and conservation equations in these coordinates at full non-linearity.

Findings

Derived compact Einstein equations in light-cone coordinates.

Established gauge-invariant linear perturbation equations.

Demonstrated statistical homogeneity in the new coordinate system.

Abstract

Analytical computations in relativistic cosmology can be split into two sets: time evolution relating the initial conditions to the observer's light-cone and light propagation to obtain observables. Cosmological perturbation theory in the FLRW coordinates constitutes an efficient tool for the former task, but the latter is dramatically simpler in light-cone-adapted coordinates that trivialize the light rays towards the observer world-line. Here we point out that time evolution and observable reconstruction can be combined into a single computation that relates directly initial conditions to observables. This is possible if one works uniquely in such light-cone coordinates, thus completely bypassing the FLRW "middle-man" coordinates. We first present in detail these light-cone coordinates, extending and generalizing the presently available material in the literature, and construct a particularly convenient subset for cosmological perturbation theory. We then express the Einstein and energy-momentum conservation equations in these coordinates at the fully non-linear level. This is achieved through a careful 2+1+1 decomposition which leads to relatively compact expressions and provides good control over the geometrical interpretation of the involved quantities. Finally, we consider cosmological perturbation theory to linear order, paying attention to the remaining gauge symmetries and consistently obtaining gauge-invariant equations. Moreover, we show that it is possible to implement statistical homogeneity on stochastic fluctuations, despite the fact that the coordinate system privileges the observer world-line.