Non-linear Equation of State:
Dark Energy Parametrization,
Dynamics
 and Singularities
Credits
Outline
Standard cosmology
Standard FRW models in GR
Main dynamical components
Observational Constraints
Singularities in GR
Motivations for a non-linear EoS
"Isotropy and singularities:"
Motivations for a quadratic EoS
Energy cons. & effective rL
Energy cons. & effective rL
Energy cons. & effective rL
Energy cons. & effective rL
RW dynamics
P=r(a + e r/rc)
P=r(a + r/rc)
P=r(a - r/rc)
Affine EoS: P=Po+ar
P=Po+ar
Full quadratic EoS
Anisotropic dynamics and singularities
 Bianchi I dynamics
Bianchi V dynamics
The isotropic past attractor IS
Perturbations of IS
Perturbations of IS
Perturbations of IS
Work in progress
 Flat model,  UDM with Affine EoS
Likelihood: Age of the Universe
Likelihood: Supernovae
Likelihood: Baryon oscillations
Likelihood: CMB first peak
Likelihood: Total
Scalar field for affine UDM
Potential
Summary
Some open questions