Free Access

Fig. 6


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°.

Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.

Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.

Initial download of the metrics may take a while.