Observational constraints on cosmological future singularities

Abstract

In this work we consider a family of cosmological models featuring future singularities. This type of cosmological evolution is typical of dark energy models with an equation of state violating some of the standard energy conditions (e.g. the null energy condition). Such kind of behavior, widely studied in the literature, may arise in cosmologies with phantom fields, theories of modified gravity or models with interacting dark matter/dark energy. We briefly review the physical consequences of these cosmological evolution regarding geodesic completeness and the divergence of tidal forces in order to emphasize under which circumstances the singularities in some cosmological quantities correspond to actual singular spacetimes. We then introduce several phenomenological parameterizations of the Hubble expansion rate to model different singularities existing in the literature and use SN Ia, BAO and H(z) data to constrain how far in the future the singularity needs to be (under some reasonable assumptions on the behaviour of the Hubble factor). We show that, for our family of parameterizations, the lower bound for the singularity time can not be smaller than about 1.2 times the age of the universe, what roughly speaking means about 2.8 Gyrs from the present time.

13 pages, 3 figures, analysis extended, version published in EPJC

References in corpus (19)

• Dynamics of dark energy
• Unified cosmic history in modified gravity: from F(R) theory to Lorentz non-invariant models
• Dark energy cosmology: the equivalent description via different theoretical models and cosmography tests
• Raising the bar: new constraints on the Hubble parameter with cosmic chronometers at z$\sim$2
• The 1% Concordance Hubble Constant
• The new form of the equation of state for dark energy fluid and accelerating universe
• Reconstructing the universe history, from inflation to acceleration, with phantom and canonical scalar fields
• Quintessence and phantom cosmology with non-minimal derivative coupling
• Worse than a big rip?
• Classification of cosmological milestones
• A cosmic vector for dark energy
• On the way from matter-dominated era to dark energy universe
• Avoidance of Big Rip In Phantom Cosmology by Gravitational Back Reaction
• Cosmological dynamics of Scalar--Tensor Gravity
• Barotropic index w-singularities in cosmology
• The little sibling of the big rip singularity
• Cosmology for quadratic gravity in generalized Weyl geometry
• Hidden past of dark energy cosmological models
• Parametrizing the transition to the phantom epoch with Supernovae Ia and Standard Rulers

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