Differentiating G-inflation from String Gas Cosmology using the Effective Field Theory Approach

TL;DR

This paper compares String Gas Cosmology and G-inflation using the Effective Field Theory approach, identifying key observational differences in tensor spectra, non-Gaussianities, and scale dependence to distinguish these models.

Contribution

It provides a detailed perturbation analysis highlighting unique observational signatures that differentiate String Gas Cosmology from G-inflation.

Findings

String Gas Cosmology predicts a specific ns-nt consistency relation.

G-inflation can produce large non-Gaussianities, unlike String Gas Cosmology.

The scale dependence of nonlinearity parameter can break model degeneracy.

Abstract

A characteristic signature of String Gas Cosmology is primordial power spectra for scalar and tensor modes which are almost scale-invariant but with a red tilt for scalar modes but a blue tilt for tensor modes. This feature, however, can also be realized in the so-called G-inflation model, in which Horndeski operators are introduced which leads to a blue tensor tilt by softly breaking the Null Energy Condition. In this article we search for potential observational differences between these two cosmologies by performing detailed perturbation analyses based on the Effective Field Theory approach. Our results show that, although both two models produce blue tilted tensor perturbations, they behave differently in three aspects. Firstly, String Gas Cosmology predicts a specific consistency relation between the index of the scalar modes ns and that of tensor ones nt, which is hard to be reproduced by G-inflation. Secondly, String Gas Cosmology typically predicts non-Gaussianities which are highly suppressed on observable scales, while G-inflation gives rise to observationally large non-Gaussianities because the kinetic terms in the action become important during inflation. However, after finely tuning the model parameters of G-inflation it is possible to obtain a blue tensor spectrum and negligible non-Gaussianities with a degeneracy between the two models. This degeneracy can be broken by a third observable, namely the scale dependence of the nonlinearity parameter, which vanishes for G-inflation but has a blue tilt in the case of String Gas Cosmology. Therefore, we conclude that String Gas Cosmology is in principle observationally distinguishable from the single field inflationary cosmology, even allowing for modifications such as G-inflation.