Detection limits of our study. Shaded bands show the +3σ RV semi-amplitude posterior of a modelled planet of a third potential planet added to the best model, in 100 log-spaced orbital-period bins. Stellar rotation somewhat degrades detection for orbital periods near P_rot (solid blue line) and P_rot/2 (dashed blue line). Dotted lines show the RV semiamplitudes that an Earth-mass planet and a Neptune-mass planet would inject in the system RV.