Detection limits for the β Pictoris system based on the calculations presented in Hey et al. (2020b) assuming 1.8 M_⊙ for the star and an inclination of 90° for both planets. The detectable parameter space for companions depending on their orbital period P_orb and mass is shaded red, assuming β Pictoris is a non-ideal δ Scuti pulsator (see Sect. 5.5 for a discussion on the pulsational modes of β Pictoris as seen by TESS). β Pictoris c is generally not detectable due to the intrinsic noise of the pulsations, and the time delay caused by β Pictoris b has a period that is too long in comparison to the baseline of our observations. The masses corresponding to brown dwarfs (13 M_J ≲ M ≲ 80 M_J) are shaded in yellow, and the stellar regime (M > 80 M_J) is in magenta, with M_J being a Jupiter mass. The figure is adapted from Hey et al. (2020b).