Cosmic Strings and Their Induced Non-Gaussianities in the Cosmic Microwave Background

Figure 9

Loop number density distribution at the end of a matter era numerical simulation. Apart for a few Kibble loops (), all loops of size with follow a scaling regime in which their number density is a power law. Smaller loops are still in the relaxation regime and will enter their scaling regime later (see Figure 10). The red dashed line if the best power law fit of the scaling function is given by (44).