B. Novosyadlyj, O. Sergijenko, R. Durrer, V. Pelykh
We analyze the possibility to distinguish between quintessence and phantom scalar field models of dark energy using observations of luminosity distance moduli of SNe Ia, CMB anisotropies and polarization, matter density perturbations and baryon acoustic oscillations. None of the present observations can decide between quintessence or phantom scalar field models at a statistically significant level: for each model a set of best-fit parameters exists, which matches all data with similar goodness of fit. We compare the relative differences of best-fit model predictions with observational uncertainties for each type of data and we show that the accuracy of SNe Ia luminosity distance data is far from the one necessary to distinguish these types of dark energy models, while the CMB data (WMAP, SPT and Planck) are close to being able to distinguish them. Also a significant improvement of the large-scale structure data (e.g. Euclid or BigBOSS) will enable us to decide between quintessence and phantom dark energy.
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http://arxiv.org/abs/1212.5824
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