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tokens: Collaboration XI (2014) . This map is corrected for zodiacal emission and the brightest extragalactic point sources are subtracted. The Galactic reference offsets of the underlying IRAS and Planck data were obtained through a method based on correlation with 21 cm data from the LAB H i survey ( Kalberla et al. 2005 ) integrated in velocity, effectively removing the CIB monopole in the model map. The mean dust intensity, , listed for each LR region in Table 1 , ranges from to for increasing . The mean column density calculated from the LAB survey data is also listed in Table 1 , with values ranging from to . For all of the LR regions, we fit the and spectra with a power law in , using the fixed exponent , over the -ranges defined in Sect. 4.2 . The amplitudes derived from these fits are listed in Table 1 ; the amplitudes can be retrieved from the ratio. These amplitudes are plotted as a function of in Fig. 4 after normalization by the maximum value found for the largest region (LR72). We fit the empirical dependence of these amplitudes on as a power law of the form where . The two fitted exponents are quite similar, and . The exponent that we find for polarization is close to the one observed in the diffuse interstellar medium for the dust intensity, consistent with , where is the mean value of the dust specific intensity ( Miville-Deschênes et al. 2007 ). Values close to 2 are expected, because we compute angular power spectra, which deal with squared quantities. Although the data points roughly follow this dependence, the empirical law fails to fully describe individual dust amplitudes (e.g., the estimate is off by about 20% for on LR33). The scaling can help to asses the order of magnitude of the dust polarization level on a specific region, but is not a substitute for actually characterizing the polarized angular power spectra. Fig. 5 Ratio of the amplitudes of the and dust power spectra at 353 GHz for the different LR regions defined in Sect. 3.3.1 , distinguished here with . The mean value is plotted as a dashed line. 4.4. Amplitude of <inline-formula><alternatives><tex-math id="tex_eq104"></tex-math><inline-graphic mime-subtype="png" mimetype="image" xlink:href="aa25034-14-eq211.png"></inline-graphic><mml:math id="mml_eq104" type="inline"> <mml:msubsup> <mml:mi mathvariant="normal">D</mml:mi> <mml:mi mathvariant="italic">l</mml:mi> <mml:mi mathvariant="slanted">BB</mml:mi> </mml:msubsup> </mml:math></alternatives></inline-formula> relative to <inline-formula><alternatives><tex-math id="tex_eq105"></tex-math><inline-graphic mime-subtype="png" mimetype="image" xlink:href="aa25034-14-eq212.png"></inline-graphic><mml:math id="mml_eq105" type="inline"> <mml:msubsup> <mml:mi mathvariant="normal">D</mml:mi> <mml:mi mathvariant="italic">l</mml:mi> <mml:mi mathvariant="slanted">EE</mml:mi> </mml:msubsup> </mml:math></alternatives></inline-formula> We examine the ratio of the amplitudes of the fitted power laws found in Sect. 4.3 . The ratios