$\Lambda$CDM-like models with future singularities

Abstract

We consider new models of dark energy with finite time future singularities, by introducing the pressure density as a function of the scale factor. This approach gives acceptable phenomenological models of dark energy, practically indistinguishable from the cosmological constant up to the present, which face future singularities at finite time and finite scale factor. Exact scalar field model representation was found for quintessence, Big Rip and type III singularity models. The simple form of the equation of state allows to establish a relationship between its current value, $w_0$, and the time or redshift at which the singularity takes place. The effect on the growth of matter perturbations was calculated.

arXiv comment32 pages, 6 figures, to appear in EPJP

References in corpus (16)

• Five-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Cosmological Interpretation
• Exploring the Expansion History of the Universe
• Dark energy cosmology: the equivalent description via different theoretical models and cosmography tests
• Phantom Energy and Cosmic Doomsday
• Baryon Acoustic Oscillations in the Sloan Digital Sky Survey Data Release 7 Galaxy Sample
• Improved Cosmological Constraints from New, Old and Combined Supernova Datasets
• Improved Dark Energy Constraints from ~100 New CfA Supernova Type Ia Light Curves
• Inhomogeneous Equation of State of the Universe: Phantom Era, Future Singularity and Crossing the Phantom Barrier
• Cosmic Growth History and Expansion History
• Cosmic Structure Growth and Dark Energy
• Viscous Little Rip Cosmology
• Scalar dark energy models mimicking $\Lambda$CDM with arbitrary future evolution
• New Parametrization for the Scale Dependent Growth Function in General Relativity
• On the dangers of using the growth equation on large scales in the Newtonian gauge
• Observational constraints on the jerk parameter with the data of the Hubble parameter
• On the consistency of the expansion with the perturbations