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We present a dynamical study of the Galactic black hole binary system NovaMuscae 1991 (GS/GRS 1124-683). We utilize 72 high resolution MagellanEchellette (MagE) spectra and 72 strictly simultaneous V-band photometricobservations; the simultaneity is a unique and crucial feature of thisdynamical study. The data were taken on two consecutive nights and cover thefull 10.4-hour orbital cycle. The radial velocities of the secondary star aredetermined by cross-correlating the object spectra with the best-match templatespectrum obtained using the same instrument configuration. Based on ourindependent analysis of five orders of the echellette spectrum, thesemi-amplitude of the radial velocity of the secondary is measured to be K_2 =406.8+/-2.7 km/s, which is consistent with previous work, while the uncertaintyis reduced by a factor of 3. The corresponding mass function is f(M) =3.02+/-0.06 M_\odot. We have also obtained an accurate measurement of therotational broadening of the stellar absorption lines (v sin i = 85.0+/-2.6km/s) and hence the mass ratio of the system q = 0.079+/-0.007. Finally, wehave measured the spectrum of the non-stellar component of emission that veilsthe spectrum of the secondary. In a future paper, we will use ourveiling-corrected spectrum of the secondary and accurate values of K_2 and q tomodel multi-color light curves and determine the systemic inclination and themass of the black hole.

A Dynamical Study of the Black Hole X-ray Binary Nova Muscae 1991