Large scale structure of f ( R ) gravity

We study the evolution of linear cosmological perturbations in $f(R)$ models of accelerated expansion in the physical frame where the gravitational dynamics are fourth order and the matter is minimally coupled. These models predict a rich and testable set of linear phenomena. For each expansion history, fixed empirically by cosmological distance measures, there exists two branches of $f(R)$ solutions that are parametrized by $Bensuremath{propto}{d}^{2}f/d{R}^{2}$. For $B0$ branch, $f(R)$ models can reduce the large-angle CMB anisotropy, alter the shape of the linear matter power spectrum, and qualitatively change the correlations between the CMB and galaxy surveys. All of these phenomena are accessible with current and future data and provide stringent tests of general relativity on cosmological scales.