  We have reanalyzed Keck observations of Nova Oph 1977 to extend the work done
by Filippenko et al. (1997), who recently determined a mass function f(M_x) =
4.86 +/- 0.13 M_o for the compact object. We constrain the rotational
broadening, v sin i < 79 km/s, at the 90% confidence level, which gives a mass
ratio q < 0.053. The K-type companion star of Nova Oph 1977 contributes 28-37%
of the light at red wavelengths. The abnormal LiI 6708 absorption line from the
companion star is not detected (EW < 0.12 A), in contrast to four other X-ray
binaries. An Halpha Doppler image of the system shows emission from the
companion star in addition to the accretion disk.
