We present results obtained from a series of 5 Å resolution spectra of the X-ray Nova GRO J0422+32 obtained in 1993 October , when the system was approximately 2 magnitudes above quiescence , with { R \sim 19 } .
The data were obtained in an effort to measure the orbital radial velocity curve of the secondary , but detection of the narrow photospheric absorption lines needed to do this proved elusive .
Instead we found wide absorption bands reminiscent of M star photospheric features .
The parameters determined by fitting accretion disk line profiles ( Smak profiles ) to the H \alpha line are similar to those found in several strong black-hole candidates .
Measurements of the velocity of the H \alpha line are consistent with an orbital period of 5.1 hours and a velocity semi-amplitude of the primary of 34 \pm 6 km s ^ { -1 } .
These measurements , when combined with measurements of the velocity semi-amplitude of the secondary made by others , indicate that the mass ratio q \sim 0.09 .
If the secondary follows the empirical mass-radius relation found for CVs , the low q implies a primary mass of M _ { x } \sim 5.6 M _ { \odot } , and a rather low ( face-on ) inclination .
The H \alpha EW is found to be modulated on the orbital period with a phasing that implies a partial eclipse of the disk by the secondary , but simultaneous R band photometry shows no evidence for such an eclipse .