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Observational constraints on dark energy model

By Yungui Gong


Abstract. The recent observations support that our universe is flat and expanding with acceleration. A quintessence model with a general relation between the quintessence potential and the quintessence kinetic energy was proposed to explain the phenomenon. The dark energy potential includes both the hyperbolic and the double exponential potentials. We analyze this model in detail by using the recent supernova and the first year Wilkinson Microwave Anisotropy Probe (WMAP) observations. For a flat universe dominated by a dark energy with constant ω which is a special case of the general model, we find that Ωm0 = 0.30 +0.06 −0.08 and ωQ ≤ −0.82, and the turnaround redshift zT when the universe switched from the deceleration phase to the acceleration phase is zT = 0.65. For the general model, we find that Ωm0 ∼ 0.3, ωQ0 ∼ −1.0, β ∼ 0.5 and zT ∼ 0.67. A model independent polynomial parameterization is also considered, the best fit model gives Ωm0 = 0.40 ± 0.14, ωQ0 = −1.4 and zT = 0.37. PACS numbers: 98.80.-k, 98.80.EsObservational constraints on dark energy model 2 1

Year: 2004
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