Fig. 10
Angular power spectrum of the dimensionless signal field (thick solid line), along with a power law fit, Cℓ ∝ ℓ-2.17 (thick dashed line). The thin lines depict the angular power spectra corresponding to the maps reconstructed by Dineen & Coles (2005), corrected for the Galactic variance profile. The three RM catalogs used in their work are from Simard-Normandin et al. (1981, S81), Broten et al. (1988, B88), and Frick et al. (2001, F01).
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