Observed RV semi-amplitudes, 0.5(v_rad,max − v_rad,min), for all stars observed with MUSE (gray), the 708 MUSE binaries (blue), and the hypothetically observable CMC binaries from the best-fit model (dark blue line). For reference, the histogram of observed RV amplitudes is also shown for all stars without the cut on photometric variables (see Sect. 2.5, dashed line), though the differences are negligible. The subset of simulated binaries with remnant (mostly white dwarf) companions is highlighted in orange. The observed lack of stars with high RV amplitudes, compared to simulations, suggests fewer stars with massive companions and/or short periods.