Detection limits of planetary signals once the stellar activity signal is removed from the raw RVs using the model proposed in Eq. (5) (solid lines) or the usual correction based on RV_activity = β₀ + β₁γ + β₂SN FWHM for the SN fitand on RV_activity = β₀ + β₁BIS SPAN + β₂FWHM for the Normal fit (dashed lines). The correction for stellar activity based on Eq. (5) improves on average the detection limit by 12% and the different RV estimators have similar detection limits.