Observational signatures of the theories beyond Horndeski

TL;DR

This paper investigates the observational signatures of beyond Horndeski theories, focusing on how deviations in tensor propagation speed affect scalar perturbations and potential observable imprints on cosmic microwave background and weak lensing.

Contribution

It derives the equations of motion for linear perturbations in beyond Horndeski theories and analyzes their observational implications, especially regarding deviations in propagation speeds.

Findings

Deviations of tensor speed squared from 1 cause large modifications in scalar propagation.

Scaling solutions can mitigate the problem of large scalar modifications.

Distinct observational signatures in CMB and weak lensing can arise from these theories.

Abstract

In the approach of the effective field theory of modified gravity, we derive the equations of motion for linear perturbations in the presence of a barotropic perfect fluid on the flat isotropic cosmological background. In a simple version of Gleyzes-Langlois-Piazza-Vernizzi (GLPV) theories, which is the minimum extension of Horndeski theories, we show that a slight deviation of the tensor propagation speed squared $c_{\rm t}^2$ from 1 generally leads to the large modification to the propagation speed squared $c_{\rm s}^2$ of a scalar degree of freedom $\phi$. This problem persists whenever the kinetic energy $\rho_X$ of the field $\phi$ is much smaller than the background energy density $\rho_m$, which is the case for most of dark energy models in the asymptotic past. Since the scaling solution characterized by the constant ratio $\rho_X/\rho_m$ is one way out for avoiding such a problem, we study the evolution of perturbations for a scaling dark energy model in the framework of GLPV theories in the Jordan frame. Provided the oscillating mode of scalar perturbations is fine-tuned so that it is initially suppressed, the anisotropic parameter $\eta=-\Phi/\Psi$ between the two gravitational potentials $\Psi$ and $\Phi$ significantly deviates from 1 for $c_{\rm t}^2$ away from 1. For other general initial conditions, the deviation of $c_{\rm t}^2$ from 1 gives rise to the large oscillation of $\Psi$ with the frequency related to $c_{\rm s}^2$. In both cases, the model can leave distinct imprints for the observations of CMB and weak lensing.