Low-energy modified gravity signatures on the large-scale structures

Abstract

A large number of dark energy and modified gravity models lead to the same expansion history of the Universe, hence, making it difficult to distinguish them from observations. To make the calculations transparent, we consider $f(R)$ gravity with a pressureless matter without making any assumption about the form of $f(R)$. Using the late-time expansion history realizations constructed by Shafieloo et al~\cite{2018-Shafieloo.etal-PRD}, we explicitly show for any $f(R)$ model that the Bardeen potentials $\Psi$ and $\Phi$ evolve differently. For an arbitrary $f(R)$ model that leads to late-time accelerated expansion, we explicitly show that $|\Psi +\Phi |$ and its time-derivative evolves differently than the $\Lambda$CDM model at lower redshifts. We show that the $\Psi /\Phi$ has a significant deviation from unity for larger wave-numbers. We discuss the implications of the results for the cosmological observations.

arXiv comment21 figures, 22 pages

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• Modified theories of Gravity: Why, How and What?
• Unifying Holographic Inflation with Holographic Dark Energy: a Covariant Approach
• Observational constraints and predictions of the interacting dark sector with field-fluid mapping
• Can we bypass no-go theorem for Ricci-inverse Gravity?
• Cylindrical black hole solutions in $f(\mathcal{R})$ and $f(\mathcal{R},\mathcal{A},A^{\mu \nu }{A}_{\mu \nu })$ modified gravity
• Black holes in $f(R)$ gravity coupled to nonlinear electromagnetic fields