(top) Best-fit radial velocity orbital solution for MML 53, and (bottom) residuals. The orbital period and ephemeris are held fixed at the values determined by the photometric light curve (Hebb et al. 2010). Phase 0.0 corresponds to T₀, the time of minimum light of the primary eclipse. The eccentricity is also held fixed at 0 (i.e. circular orbit). Plotted are the radial velocity measurements for the primary (circles) and secondary (triangles) components. The solid symbols are used to derive the orbit solution fits for the primary (solid line) and secondary (dashed line). Open symbols were not used to fit the radial velocity curve because the primary and secondary cross-correlation peaks were blended.