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The inflationary paradigm solves the three classical problems in standard cosmology: the flatness problem, the horizon problem, and the unwanted relics problem. In particular the flatness problem is solved by explaining how the relative contribution of the spatial curvature of the Universe to the total energy density decreases exponentially during inflation. In addition, the inflationary scenario offers us an efficient mechanism to generate small perturbations in the spatial curvature that would explain the observed temperature anisotropies in the cosmic microwave background radiation (CMB). The traditional inflationary models that neglect the relative contribution reproduce the recent observations from the WMAP satellite on the angular spectrum C1 of the temperature anisotropies in the CMB, except for the lower multipoles, and specially for the quadrupole (l = 2) for which the observed value presents an unexpected fati. Such a strange behaviour leads us to analyze the angular spectrum C1 on large scales (low multipoles) taking into account the relative contribution. We determine in this way the type of characteristic curvature of the observed Universe most favoured by the observational data regarding the quadrupole.
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