III we describe the current observational data used in this paper. Phys. Phys. In this paper, we choose ten typical, popular dark energy models to analyze. [75, 76]), but we do not discuss this aspect in this paper. For the RDE model, we have ΔAIC=290.337 and ΔBIC=294.994. The χ2 function for BAO is. (22), we have, Here in our work the radiation density parameter Ωr is given by. Thus we have ¯¯¯¯¯¯¯Rb=31500Ωbh2(Tcmb/2.7K)−4. The original Chaplygin gas model has been excluded by observations [54], thus here we only consider the generalized Chaplygin gas (GCG) model [51] and the new generalized Chaplygin gas (NGCG) model [52]. Standard big bang nucleosynthesis predictions for the Planck LCDM cosmology are in excellent agreement with observations. Phys. Constraining dynamical dark energy with a divergence-free parametrization in the presence of spatial curvature and massive neutrinos, Some dynamical dark energy models are built based on deep theoretical considerations. Holographic Ricci dark energy: Current observational constraints, quintom feature, and the reconstruction of scalar-field dark energy, Z. Ma and X. Zhang, Dark energy and modified gravity . Planck 2015 results: XIV. Thus, in this sense, the UV problem of the calculation of vacuum energy density is converted to an IR problem. In this work, we apply the IC method to do the analysis. Theor. ; Rachen, J.P.; Zonca, A.; et al. Rev. Publication year: 2016 In this work, we choose ten typical, popular dark energy models to make a uniform, fair comparison. All results that include only background parameterizations (expansion of the equation of state, early DE, general potentials in minimally-coupled scalar fields or principal component analysis) are in agreement with ΛCDM. JCAP. Constraints on oscillating quintom from supernova, microwave background and galaxy clustering, Since a non-vanishing anisotropic. Planck Constraints on Holographic Dark Energy, Lett. Ann. D. E. V. Linder, Exploring the expansion history of the universe, Phys. The spherical average gives us the expression of DV(z), The comoving sound horizon size rs(zd) is given by Eq. We study the implications of Planck data for models of dark energy (DE) and modified gravity (MG), beyond the cosmological constant scenario. Title: Planck 2015 results. Rev. J. D. J. Eisenstein and W. Hu, Baryonic features in the matter transfer function, Astrophys. Output The Chaplygin gas model [50], which is commonly viewed as arising from the d-brane theory, can describe the cosmic acceleration, and it provides a unification scheme for vacuum energy and cold dark matter. Because we consider a flat universe, DA can be expressed as. G. Efstathiou, H0 revisited, Mon. Phys. arXiv:1607.05643 [astro-ph.CO]. Among many models, one can choose the model with minimal value of AIC as a reference model. We notice that the NADE model yields a large χ2min, much larger than that of ΛCDM. Phys. "Surprisingly, the amount of early dark energy was … Read this paper on arXiv.org. Northeastern University, Shenyang 110004, China, Center for High Energy Physics, Peking University, Beijing 100080, China, V. Sahni and A. Roy. Phys. Request PDF | Planck 2015 results. The χ2 function for CMB is. XIV. Dark energy and modified gravity | 32 pages, 22 figures. The NADE, DGP, and RDE models are excluded by the current observations. We make a comparison for ten typical, popular dark energy models according to their capabilities of fitting the current observational data. Dark energy is a diffuse, very weakly interacting with matter and very low energy phenomenon. For the NGCG model, we have ΔAIC=2.956 and ΔBIC=12.191. For the GCG model, we have ΔAIC=1.006 and ΔBIC=5.623. Lett. Probing the dark energy: Methods and strategies, We can confirm that, in the sense of explaining observations, according to our analysis results, the NADE, DGP, and RDE models are excluded by current observations. We make a comparison for ten typical, popular dark energy models according to their capabilities of fitting the current observational data. where N is the number of data points used in the fit. An alternative to quintessence, Such an interacting dark energy model is a large-scale stable model, naturally avoiding the usual super-horizon instability problem existing in the interacting dark energy models [77]. M. Li, A model of holographic dark energy, Phys. A 4 per cent distance measure at. Astron. The 1–2σ posterior possibility contours in the Ωm–w and Ωm–h planes for the wCDM model are plotted in Fig. A global fit study on the new agegraphic dark energy model, Note that the various observations used in this paper are consistent with each other. Journal Article, Planck intermediate results. D. M. Kamionkowski, Dark matter and dark energy, arXiv: 0706.2986 [astro-ph]. 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