Polarization amplitude root-mean-square (RMS) as a function of frequency and astrophysical component and polarized emission. Each component map is smoothed to a common angular resolution of 1° FWHM, and the lower and upper edges of each band are defined by the RMS outside masks covering 27% and 88% of the sky, respectively. An artificial broadening has been applied to the low-amplitude tails of the foreground spectra to visually indicate uncertainties in regions of low S/N for the relevant components. The EE CMB spectrum is generated from ideal CMB simulations based on the best-fit PlanckΛCDM model, while the BB limits are derived with tensor-to-scalar ratios of r = 10⁻² and 10⁻⁴, respectively. Additionally, we visualize an upper limit on the polarization fraction of spinning dust of 1% as has been reported in literature (Génova-Santos et al. 2017; Macellari et al. 2011; Herman et al. 2023).