The magnetic field investigations of the rapidly-oscillating (ro)Ap star ϒ Equ show a very long magnetic (rotational) period of about 74 years (Leroy et al. 1994; Bychkov & Shtol 1997). No significant changes of radial velocities were detected during the history of investigations of this star. Recently, Scholz et al. (1997) (hereafter S97) reported a rapid increase of radial velocity (RV) of ϒ Equ from the mean value of -16.81 km s−1 up to a maximum at -4.28 km s−1 within the interval JD 2449608 – JD 2450356, and suggested that ϒ Equ is a long-period binary star with high eccentricity. Such a probable discovery of binary motion of ϒ Equ is very interesting, since it opens the possibility to compare asteroseismic parameters of the star with those obtained from the binary orbit.