In a viable f(R) model transitioning from early GR-like to late non-GR behavior, matter power spectra show higher monopole and quadrupole power at small scales with quadrupole elevated at large scales up to k~0.02, while scalaron mass decreases over time to GR limits on galactic scales.
Can modified gravity explain accelerated cosmic expansion?,
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Redundancy of cosmological evolution equations in FLRW models is inevitable in general relativity and accounts for the special role of one Friedmann equation in constraining initial values.
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Cosmological perturbations with $f(R)$ gravity scalarons : Galaxy power spectra and the scalaron mass
In a viable f(R) model transitioning from early GR-like to late non-GR behavior, matter power spectra show higher monopole and quadrupole power at small scales with quadrupole elevated at large scales up to k~0.02, while scalaron mass decreases over time to GR limits on galactic scales.
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Redundancy of the cosmological evolution equations and its relationship with the initial conditions
Redundancy of cosmological evolution equations in FLRW models is inevitable in general relativity and accounts for the special role of one Friedmann equation in constraining initial values.