Early Modified Gravity: Implications for Cosmology

Abstract

We study the effects of modifications of gravity after Big Bang Nucleosynthesis (BBN) which would manifest themselves mainly before recombination. We consider their effects on the Cosmic Microwave Background (CMB) radiation and on the formation of large scale structure. The models that we introduce here represent all screened modifications of General Relativity (GR) which evade the local tests of gravity such as the violation of the strong equivalence principle as constrained by the Lunar Ranging experiment. We use the tomographic description of modified gravity which defines models with screening mechanisms of the chameleon or Damour-Polyakov types and allows one to relate the temporal evolution of the mass and the coupling to matter of a scalar field to its Lagrangian and also to cosmological perturbations. The models with early modifications of gravity all involve a coupling to matter which is stronger in the past leading to effects on perturbations before recombination while minimising deviations from Lambda-CDM structure formation at late times. We find that a new family of early transition models lead to discrepancies in the CMB spectrum which could reach a few percent and appear as both enhancements and reductions of power for different scales.

22 pages, 7 figures

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Cited by in corpus (13)

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• The Observational Future of Cosmological Scalar-Tensor Theories
• Finite-time Cosmological Singularities and the Possible Fate of the Universe
• hi_class: Background Evolution, Initial Conditions and Approximation Schemes
• Diagnostic of Horndeski Theories
• Constraints on decaying early modified gravity from cosmological observations
• Current constraints on early and stressed dark energy models and future 21 cm perspectives
• Dark Energy Scaling from Dark Matter to Acceleration
• Intensity mapping of post-reionization 21-cm signal and its cross-correlations as a probe of $f(R)$ gravity
• Quartic Chameleons: Safely Scale-Free in the Early Universe
• Is Dark Energy an Effective Manifestation of Non-equilibrium Thermodynamics? -- Insights from DESI