Angular EE (left panel) and BB (right panel) power spectra for polarized synchrotron (at 30 GHz) and thermal dust emission (at 353 GHz), evaluated with 1deg FWHM apodization and including a total effective sky fraction of 73% of the sky. The dashed lines show the best-fit power-law models to each case, and the solid black lines shows the best-fit ΛCDM power spectrum as fitted to temperature observations only (Planck Collaboration XI 2016; Planck Collaboration XIII 2016). The dashed black line in the BB panel shows the spectrum for a model with a tensor-to-scalar ratio of r = 0.05.