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Polarized foregrounds are going to be a serious challenge for detecting CMBcosmological B-modes. Both diffuse Galactic emission and extragalactic sourcescontribute significantly to the power spectrum on large angular scales. At lowfrequencies, Galactic synchrotron emission will dominate with fractionalpolarization $\sim 20-40%$ at high latitudes while radio sources can contributesignificantly even on large ($\sim 1^{\circ}$) angular scales. Nevertheless,simulations suggest that a detection at the level of $r=0.001$ might beachievable if the foregrounds are not too complex.

Polarized CMB Foregrounds: What do we know and how bad is it?