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tokens: Rayleigh tail of the dust blackbody spectrum, we do not expect a significant shift in the sources probed or in the polarization of each source between 95 and 150 GHz. Supporting this position, Bonavera et al. ( 2017b ) found the DSFG 〈 p 〉 to not vary with frequency from 143 to 353 GHz. For a reasonable mask flux threshold of 2 mJy, which is achievable by existing experiments like SPT-3G, the total polarized foreground power is less than the EE power spectrum out to l ≲ 5700 (l ≲ 4700) and the BB lensing power spectrum out to l ≲ 5300 (l ≲ 3600) at 95 (150) GHz. Figure 5. CMB polarization surveys will be minimally impacted by polarized source power after masking radio and dusty galaxies above reasonable flux thresholds. The predicted AGN power at 95 GHz (left-hand panel) and 150 GHz (right-hand panel) for the 〈 p 2 〉 measured in this work is shown by the solid red (yellow) line for a 50 (2) mJy masking flux threshold in temperature. The filled area represents the 1σ uncertainties on 〈 p 2 〉 (no uncertainty in the source distribution has been included). The dashed blue line and the filled blue area show the mean and the 1σ upper limit on the predicted DSFG polarized power, respectively. We have assumed that the fractional polarization of the DSFGs remains constant from the value measured at 150 GHz down to 95 GHz. The total polarized foreground power will be less than the CMB EE power spectrum out to l ≲ 5700 (l ≲ 4700) and CMB lensing BB power spectrum out to l ≲ 5300 (l ≲ 3600) at 95 (150) GHz. The green arrow in the right-hand panel shows the 95 per cent CL upper limit from the recent SPTpol EE power spectrum measurement (Henning et al. 2018 ). The polarization fraction measurements in this work support the expectation that extragalactic foregrounds will be fractionally smaller for CMB polarization than temperature measurements, thus allowing more modes to be used in polarization analyses. The equivalent angular multipole for temperature is l ∼ 4000 and l ∼ 3100 at 95 and 150 GHz, respectively – more modes will be available to cosmological studies in polarization than temperature. Note that the results are not particularly sensitive to the flux cut since the polarized foreground power envelope is being driven by DSFGs. The DSFG intensity power varies slowly with mask threshold since most DSFGs are fainter than 2 mJy. It is also worth noting that better measurements of the DSFG 〈 p 2 〉 are likely to make the AGN power, and thus masking threshold, somewhat more important. We have reasons to believe that the polarization of DSFGs is lower than AGN, but 1σ limits in this work are higher (at 150 GHz) for DSFGs due to the limited number of DSFGs in the sample. The inferred power from the measured 〈 p 2 〉 values in this work are compatible with current observational constraints. Using the measured EE bandpowers from the SPTpol survey at 150 GHz, Henning et al. ( 2018 ) places a 95 per cent confidence level upper limit of on polarized point