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Fig. 6

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Theoretical CMB power spectrum due solely to Sachs-Wolfe-induced fluctuations in the Rh = ct Universe (solid, thick curve), in comparison with the power spectrum measured from the full WMAP sky (thin, jagged line; Spergel et al. 2003; Tegmark et al. 2003). The gray region represents the one-sigma uncertainty. The power spectrum for l > 10−20 is dominated by small-scale physical effects, such as baryon acoustic oscillations near the surface of last scattering, which are not included in our analysis. For comparison, we also show the WMAP best-fit (dashed) curve, calculated with all of the physical effects producing the fluctuations. This curve fits the data very well, particularly at very high l’s, corresponding to fluctuations on scales smaller than ~10°.

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