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Testing and selection cosmological models with dark energy
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abstract
It is described dynamics of a large class of accelerating cosmological models in terms of dynamical systems of the Newtonian type. The evolution of the models is reduced to the motion of a particle in a potential well parameterized by the scale factor. This potential function can be reconstructed from distant supernovae type Ia data and many cosmological models represented in terms of the potential becomes in a good agreement with current observational data. It is proposed to use the information criteria to overcome this degeneracy within a class of A) dark energy models and B) simple models basing on modification of the FRW equation. Two class of models can be recommended by the Akaike (AIC) and Schwarz (BIC) information criteria: the phantom and $\Lambda$CDM models.
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Do we really need alternatives to the $\omega_0\omega_a$CDM parameterization after the DESI DR2?
In a common physically motivated pivot basis, the standard CPL parameterization is mildly preferred over the fafbCDM density expansion and reproduces quintessence backgrounds at least as well.
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