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Better understanding of Galactic foregrounds is one of the main obstacles todetection of primordial gravitational waves through measurement of the B modein the polarized microwave sky. We generalize the method proposed in\cite{2011PhRvD..83h3003B} and decompose the polarization signals into the Eand B families directly in the domain of the Stokes $Q$, $U$ parameters as$(Q,U)\equiv(Q_E, U_E)+(Q_B,U_B)$. This also enables an investigation of themorphology and the frequency dependence of these two families, which has beendone in the WMAP K, Ka (tracing synchrotron emission) and Planck 2015 HFI maps(tracing thermal dust). The results reveal significant differences in spectrabetween the E and B families. The spectral index of the E family fluctuatesless across the sky than that of the B family, and the same tendency occurs forthe polarization angles of the dust and synchrotron channels. The new insightfrom WMAP and Planck data on the North Polar Spur and BICEP2 zones through ourmethod clearly indicates that these zones are characterized by very lowpolarization intensity of the B family compared to the E family. We havedetected global structure of the B family polarization angles at high Galacticlatitudes which cannot be attributed to the cosmic microwave background orinstrumental noise. However, we cannot exclude instrumental systematics as apartial contributor to these anomalies.

E and B families of the Stokes parameters in the polarized synchrotron and thermal dust foregrounds