(Left-hand panel:) Radial velocities. Velocities of the brighter star are shown as black crosses, while those obtained from the envelope spectra are shown as blue (He I) and red (Si II emission lines) crosses. (Right-hand panel:) Velocities from the left-hand panel phased using the ephemeris found by Hutchings & Redman (1973). The green squares are the means of the velocities for He I and metal lines listed in Table 1 of Merrill (1949) with phases computed from the Hutchings & Redman (1973) ephemeris. The velocities for the bright star measured from the DAO spectra agree with the Merrill measurements, indicating that the orbital properties of the system have then been stable to within ±10⁻³% over the time span of a century. That the amplitude of the radial-velocity curve of the bright star is larger than the range in radial velocities obtained from the envelope spectra indicates that the brighter star is less massive than the companion.