Top panel: Distribution of companion masses for the MSP sample. The solid red lines show a power-law distribution with a slope of −4, plotted for comparison. Bottom panel: Distribution of binary orbital periods for the MSP sample. Overplotted are the estimated pulsar detection efficiencies in radio surveys, based on the modelling by Bagchi et al. (2013). Two search strategies are shown: γ₁ for a standard (non-accelerated) search, and γ₂ for an acceleration search. These detection efficiency curves are computed assuming the following orbital parameters: eccentricity e = 0, M_MSP = 1.4 M_⊙, integration time Tobs = 1000 s, WD companion mass derived from the Tauris & Savonije (1999) relation, spin period of 3 ms, orbital inclination i = 60°, and longitude of periastron Ω = 30°.