Reconstruction of Dynamical Dark Energy Potentials: Quintessence, Tachyon and interacting models

Abstract

Dynamical models for dark energy are an alternative to the cosmological constant. It is important to investigate properties of perturbations in these models and go beyond the smooth FRLW cosmology. This allows us to distinguish different dark energy models with the same expansion history. For this, one often needs the potential for a particular expansion history. We study how such potentials can be reconstructed obtaining closed formulae for potential or reducing the problem to quadrature. We consider three classes of models here: tachyons, quintessence, and, interacting dark energy. We present results for constant w and the CPL parameterization. The method given here can be generalized to any arbitrary form of w(z).

arXiv comment9 pages, 5 figures, minor corrections and references updated. Final version

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• The Hubble Tension, The $M$ Crisis of Late Time $H(z)$ Deformation Models and the Reconstruction of Quintessence Lagrangians
• Multi-field Inflation in High-Slope Potentials
• Reconstruction of late-time cosmology using Principal Component Analysis
• Non-linear spherical collapse in tachyon models, and a comparison of collapse in tachyon and quintessence models of dark energy
• Inference of cosmological models with principal component analysis