Evolution of the RV semiamplitude of the binary motion as a function of the orbital period (top), stellar radius of the primary from Gaia parameters (middle), and the seismically inferred mass (bottom panel). The colors of the dots represent the various evolutionary states and are identical to Fig. 1. The dotted and solid horizontal lines in the top and bottom panels depict the detection threshold of the RVS instrument for faint (G ≤ 14 mag) and bright stars (G ≤ 12 mag), respectively. The gray lines in the middle panel depict the RV for binary systems whose Roche lobe radius is filled. The vertical purple line marks the chosen separation between RC and 2RC stars.