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

## TL;DR

This paper investigates how $f(R)$ modified gravity models, which mimic dark energy, produce distinct signatures in large-scale structure evolution, especially in gravitational potentials, offering potential observational tests to distinguish them from standard cosmology.

## Contribution

The study explicitly demonstrates the evolution differences of gravitational potentials in arbitrary $f(R)$ models without assuming specific forms, highlighting observable deviations from $ extit{ extbf{Lambda}}$CDM.

## Key findings

- $| ext{ extbf{Psi}} + ext{ extbf{Phi}}|$ evolves differently than $ ext{ extbf{Lambda}}$CDM at low redshifts.
- $ ext{ extbf{Psi}}/ ext{ extbf{Phi}}$ significantly deviates from unity at larger wave-numbers.
- Differences in potential evolution can be used to observationally distinguish $f(R)$ gravity from standard cosmology.

## 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.