Amplitude detection limit from a prewhitening strategy using the S/N stopping criterion and a high amplitude version of the AFFOGATO SPB sample (cf. Sect. 6.2). This plot illustrates the general noise budget in the frequency domain enforced by random and systematic noise sources. Like in the time domain (see Fig. C.1), the detection limit at mission level is a clear function of the camera observability (colour scale). The dark grey data points are stars with a SPR value larger than 6% (a critical threshold explained in Sect. 6.5). The dotted horizontal lines are reference limits. We highlight that multiple stars have a camera visibility different from n_CAM ∈ {6, 12, 18, 24} due to the usage of pointing error sources in our simulations (cf. Sect. 5.1). The same is true for Figs. 14 and 15. While we illustrate the star count histogram (versus n_CAM) of this figure in Fig. C.4, the effect in this plot is most noticeable from the four (upper-most) purple/blue data points with n_CAM ∈ {1, 2}.