Figure 1: Plots of the difference histogram illustrating the magnitudes of the deviation from isotropy as a function of separation angle calculated for two specific spherical caps, centered at and , with a of aperture. Plotted also, as a continuous line, is the mean corresponding to the set of spherical caps into which the sphere was subdivided, along with the corresponding two-standard deviation region as a shaded area. As can be seen, the measured anisotropy is significant in one cap [ ] but not in the other. | |
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Figure 2: The full sky map of calculated from 12 288 evenly distributed caps covering the ILC map. | |
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Figure 3: The power spectrum of the -map for the ILC map, for (solid dots). Note the high values of the first three multipoles. For comparison, the mean expected power spectrum of the -map obtained by averaging over a set of 1000 Monte Carlo-generated, statistically isotropic CMB maps (solid curve). Shown also are the corresponding cosmic variance bounds for -maps (shaded area). | |
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Figure 4: Depicted clockwise are the ILC -map's dipole, quadrupole, octopole, and the remaining -map from which all these components plus the monopole were removed. | |
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Figure 5: Depicted clockwise are the -maps: LILC, three-year coadded map (showing the effects of the unfiltered galactic contamination), OT and TOH WMAP maps. The one-year coadded and the PPG maps are not shown as they are very similar to the three-year coadded and the ILC maps, respectively. Note the high- region in the south eastern corner of the -maps, which remains robust for all maps. | |
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