Phantom crossing dark energy in Horndeski's theory

Abstract

The $\Lambda$CDM model is a remarkably successful model which is consistent with the observations of cosmic microwave background radiation (CMB), baryon acoustic oscillation (BAO), and large scale structure of the Universe. However, the discrepancy in the value of $H_0$ between the local observations and PLANCK observation of CMB was recently pointed out. One of the way to ease the discrepancy is to introduce phantom dark energy instead of the cosmological constant. While, phantom dark energy often suffer from the instabilities. We will investigate the general solution to overcome the difficulty of phantom dark energy and construct some particular models which have a phantom crossing and can be consistent with the observations.

16 pages, 5 figures. References added, sentences and expressions polished, version to appear in PRD

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Cited by in corpus (14)

• Constraints on the sum of the neutrino masses in dynamical dark energy models with $w(z)\ge -1$ are tighter than those obtained in $\Lambda$CDM
• Dark Energy with Phantom Crossing and the $H_0$ tension
• DESI 2024: Reconstructing Dark Energy using Crossing Statistics with DESI DR1 BAO data
• Is Local $H_0$ At Odds With Dark Energy EFT?
• Omnipotent dark energy: A phenomenological answer to the Hubble tension
• Towards a possible solution to the Hubble tension with Horndeski gravity
• The H0 trouble: Confronting Non-thermal Dark Matter and Phantom Cosmology with the CMB, BAO, and Type Ia Supernovae data
• Exploring cosmological imprints of phantom crossing with dynamical dark energy in Horndeski gravity
• Structure Formation in the Effective Field Theory of Holographic Dark Energy
• New measures to test modified gravity cosmologies
• Oscillating solutions of the matter density contrast in Horndeski's theory
• A short review on Quintom dark energy theory
• Quintom Dark Energy: Future Attractor and Phantom Crossing in Light of DESI DR2 Observation
• Dynamical Shortcomings in the Generalized SU(2) Proca Theory: Challenges for Cosmic Acceleration