Left: Expected A_ell for a 1 M_⊙ MS star with an 8 M_⊙ dark companion (i.e. mass ratio q = 8) at a range of orbital periods (denoted in days in the legend) as a function of orbital inclination cos i (0 is edge-on, 1 is face-on). Because the probability distribution of cos i is uniform for a randomly oriented orbit, every y value plotted here is equally likely. We note that this binary system will overflow its Roche lobe at a period of ≈0.37 days. Middle: Derived values of q_min for the same binary systems, assuming perfect knowledge of M₁ and R₁. The differences between the curves in this panel come solely from neglecting of the Gomel et al. (2021c) correction factor, C, which depends on Roche lobe filling factor. Neglecting C also explains why values of q_min > 8 are possible, as is discussed in the text. The dotted grey line shows the true value of q. We do not plot the P_orb = 0.4 day model here, as the large value of C produces an unphysical value of ℳ_ell > 1 and causes a breakdown of the q_min calculation. Right: Derived values of MMMR for the same binary systems. We note that most binary configurations result in MMMR < 1, and even the P_orb = 0.4 day track produces MMMR > 1 for less than half of the range of cos i.