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The angular CMB power spectrum of cosmic strings, from a simulation by Contaldi et al. [26]. The ÿgure shows the result for strings decaying into a uid obeying the equation of state p = w with w = 1=3; 0:1; 0:01, respectively. The old data overlaid to the graph is to be ignored. R. Durrer et al. / Physics Reports 364 (2002) 1 – 81 43 quite high [26,121]. We can maybe understand this di erence between global and local defects as being due to the larger di erence between the source functions in the radiation and matter dominated era: for the global O(N ) defects, the ratio between the sources in the two epochs is about 1:2, while for strings it is rather in the vicinity of 4 [160].
2. Energy momentum conservation of numerical simulations is shown. The lines represent the sum of the terms which has to vanish if energy (solid), respectively, momentum (dashed) is conserved, divided by the sum of the absolute values of these terms. The abscissa indicates the wavelength of the perturbation as fraction of the size of the entire grid (from [47]). Fig. 3. The C‘ power spectrum is shown for the large-N limit (bold line) and for the texture model. The main di erence is clearly that the large-N curve shows some acoustic oscillations which are nearly entirely washed out in the texture case.
The analysis described here does not take into account the e ects of non-linearities and redshift distortions. Redshift distortions in the texture case should be less important than in the in ationary case since the peculiar velocities are rather low (see next paragraph). Non-linearities typically set in at k ¿ 0:5h Mpc−1 and should not have a big e ect on our main conclusions which come from much larger scales. Inclusion of these corrections will result in more small-scale power and in a broadening of the spectra, which even enhances the con ict between models and data.