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 \pm 0.13 ~ { } M _ { \odot } for the compact object .
We constrain the rotational broadening , \upsilon \sin i \leq 79 km s ^ { -1 } , at the 90 % confidence level , which gives a mass ratio q \leq 0.053 .
The K-type companion star of Nova Oph 1977 contributes 28–37 % of the light at red wavelengths .
The abnormal \ion Li1 \lambda 6708 absorption line from the companion star is not detected ( EW < 0.12 Å ) , in contrast to four other X-ray binaries .
An H \alpha Doppler image of the system shows emission from the companion star in addition to the accretion disk .