Bohdan Novosyadlyj, Olga Sergijenko, Ruth Durrer, Volodymyr Pelykh
The dynamics of expansion and large scale structure formation of the Universe are analyzed for models with dark energy in the form of a phantom scalar field which initially mimics a $\Lambda$-term and evolves slowly to the Big Rip singularity. The discussed model of dark energy has three parameters -- the density and the equation of state parameter at the current epoch, $\Omega_{de}$ and $w_0$, and the asymptotic value of the equation of state parameter at $a\rightarrow\infty$, $c_a^2$. Their best-fit values are determined jointly with all other cosmological parameters by the MCMC method using observational data on CMB anisotropies and polarization, SNe Ia luminosity distances, BAO measurements and more. Similar computations are carried out for $\Lambda$CDM and a quintessence scalar field model of dark energy. It is shown that the current data slightly prefer the phantom model, but the differences of maximum likelihoods are not statistically significant. It is also shown that the phantom dark energy with monotonicaly increasing density in future will cause the decaying of large scale linear matter density perturbations due to the gravitational domination of dark energy perturbations long before the Big Rip singularity.
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http://arxiv.org/abs/1206.5194
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