Search for Non-Gaussianities in the WMAP Data with the Scaling Index Method
Figure 2
A simulated CMB map, in which the central regions were masked out and filled with nearly white noise, whereby the spatial noise patterns are preserved (see Section 3.1) (a), and its scaling index responses for three different scaling ranges: (b), (c), and (d). Different values of correspond to different types of structure in the underlying map. Small scaling ranges examine the behaviour of the small structures, while the characteristics of the larger structure displayed by the higher scaling ranges. Note the different structure inside and outside the masked region of the simulated map, which is clearly identified by the scaling indices. These maps (and all following ones) are shown in a conventional scheme, namely, the Mollweide projection in the galactic reference frame with the Galactic Centre at the centre of the image and the longitude increasing from there to the left-hand side.
