The Cosmology of Ricci-Tensor-Squared Gravity in the Palatini Variational Approach

TL;DR

This paper explores the cosmological implications of Ricci-tensor-squared gravity in the Palatini formalism, analyzing background evolution, perturbations, and observational constraints from supernovae and CMB data.

Contribution

It introduces a general method for deriving covariant perturbation equations in Ricci-tensor-squared Palatini gravity and constrains model parameters using observational data.

Findings

Best fit to data suggests a non-zero correction to Einstein gravity.

Current observations do not strongly favor deviations from the standard model.

Matter power spectrum constrains the model parameter |eta| extless{} O(10^{-5}).

Abstract

We consider the cosmology of the Ricci-tensor-squared gravity in the Palatini variational approach. The gravitational action of standard general relativity is modified by adding a function f(R^abR_ab) to the Einstein-Hilbert action, and the Palatini variation is used to derive the field equations. A general method of obtaining the background and first-order covariant and gauge-invariant perturbation equations is outlined. As an example, we consider the cosmological constraints on such theories arising from the supernova type Ia and cosmic microwave background observations. We find that the best fit to the data is a non-null leading-order correction to Einstein gravity, but the current data exhibit no significant preference over the concordance model. The growth of non-relativistic matter density perturbations at late times is also analyzed, and we find that a scale-dependent (positive or negative) sound-speed-squared term generally appears in the growth equation for small-scale density perturbations. We also estimate the observational bound imposed by the matter power spectrum for the model with f(R^abR_ab) = alpha(R^abR_ab)^beta to be roughly |\beta| \lesssim O(10^{-5}) so long as the dark matter does not possess compensating anisotropic stresses.