Stacked Bayesian GLS periodogram analysis of the HARPS-N dataset. Top: Periodogram of the original HARPS-N RV dataset (left) and the HARPS-N RV dataset after modeling of the transiting planet TOI-2141 b (right). The amount of observations is plotted against period, with the color scale indicating the logarithm of the power or probability of a coherent long-lived signal, where darker is more likely. Bottom: Power as a function of the number of observations for the three RV signals of interest in the system: the transiting planet at 18.26 d (top), the inner non-transiting planet at 5.46 d (middle), and the outer non-transiting planet at 60.45 d (bottom). The first panel is computed from the original RV dataset, the next two from the residuals of fitting the transiting planet. The monotonic increase of power as afunction of number of observations is typical of bonafide planets and not of astrophysical or instrumental origin (Mortier & Collier Cameron 2017).