Notes. The spectral differences are calculated over 58% of the sky, and a delensing efficiency ϵ is defined as a scaling of our fiducial lensing B-mode power, so that , computed over the ℓ range 100 ≤ ℓ ≤ 2048 (i.e., ϵ is the fraction by which the lensing B-mode power can be reduced). The right-hand column gives the expected efficiency, as estimated from FFP10 simulations. We neglect the TB and EB quadratic estimators in the default MV estimator when building the combined TT, TE, and EE estimators used here; including them introduces large signals from disconnected correlators unrelated to actual delensing, for a negligible increase in delensing efficiency. The efficiency is scale-dependent, with a maximum close to 20% on large scales. Also listed are reduced χ² (, for ν = 9 degrees of freedom), for compared to the best-fit model . This model does not capture very well the delensing results including the CIB. However, all results are fully consistent with the simulation predictions.