We present results obtained from a series of 5~\AA\ 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∼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 Hα line are similar to those
found in several strong black-hole candidates. Measurements of the velocity of
the Hα line are consistent with an orbital period of 5.1~hours and a
velocity semi-amplitude of the primary of 34±6~\kms. These measurements,
when combined with measurements of the velocity semi-amplitude of the secondary
made by others, indicate that the mass ratio q∼0.09. If the secondary
follows the empirical mass-radius relation found for CVs, the low q implies a
primary mass of Mx​∼5.6\mo, and a rather low (face-on) inclination. The
Hα 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.Comment: Accepted for ApJ, plain latex, 5 figures available as self-extracting
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