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The polarization of the CMBR represents a powerful test for modern cosmology.It allows to break the degeneracy of fundamental cosmological parameters, andalso to observe the contribution of gravitational waves background to the CMBRanisotropy. To observe the CMBR polarization several experiments are either inprogress or planned and SPOrt is one of the most promising planned by ESA. Atthe same time the observation of the CMBR polarization is a difficult task andone of the reasons is the presence of polarized foreground emission. Forinstance, galactic polarized synchrotron emission (according to some estimates)can completely mimic the polarization of the CMBR. Nevertheless, one can usemathematical properties of the spherical harmonics of the distribution ofradiation over the sky to separate different contributions. In this paper themathematical properties of the polarized synchrotron foreground and thephysical mechanism that produces it are discussed. The separation ofsynchrotron polarization from the polarization generated by densitycosmological perturbations is discussed as well.Comment: 10 LaTeX pages, acceptted to AIP Conference Proceedin

Galactic synchrotron foreground and the CMB polarization measurements