Unifying inflation with early and late dark energy epochs in axion F(R) gravity

We provide a theoretical model of F(R) gravity in which it is possible to describe in a unified way inflation, an early and a late dark energy era, in the presence of a light axion particle which plays the role of the dark matter component of the Universe. Particularly, the early time phenomenology is dominated by an R-2 term, while the presence of the other terms F(R) ensure the occurrence of the early and late-time dark energy eras. The inflationary phenomenology is compatible with the Planck 2018 data for inflation, while the late-time dark energy era is compatible with the Planck 2018 constraints on the cosmological parameters. Also, the model exhibits an early dark energy era, at z similar to 2.5 approximately, followed by a deceleration era, which starts at approximately z similar to 1.5, which in turn is followed by a late-time dark energy era for redshifts z similar to 0.5, which lasts for approximately 5 billion years up to present time. A notable feature of our model is that the dark energy era is free from dark energy oscillations, at least in the redshift interval z = [0, 10]. In addition, we also discuss several features related to observational data at z similar to 2.34, at which redshift intricate observational data exist in the literature. Moreover, the numerical code for the dark energy phenomenology, written in PYTHON3, is presented in the end of the article. Finally, the model has another interesting characteristic, a sudden jump of the value of the Hubble rate in the redshift interval z similar to [2, 2.6] where its value suddenly increases and then decreases until z similar to 0.

Automated summary

This article introduces a theoretical model of F(R) gravity that can describe inflation, early and late dark energy eras in the presence of a light axion particle as the dark matter component of the Universe. The model exhibits early and late-time dark energy eras, with an early dark energy era followed by a deceleration era and then a late-time dark energy era. A notable feature is the absence of dark energy oscillations in the dark energy era within the redshift interval z = [0, 10]. The model also shows a sudden jump in the value of the Hubble rate within the redshift interval z ≈ [2, 2.6], increasing and then decreasing until z ≈ 0.