  We present a reanalysis of the outburst radial velocity data for X-Ray Nova
Scorpii 1994. Using a model based on X-ray heating of the secondary star we
suggest a more realistic treatment of the radial velocity data. Solutions are
obtained in the (K_2,q) plane which, when combined with the published value for
the binary mass ratio and inclination, constrain the mass of the black hole to
within the region 4.1<M_1<6.6 Msun (90 per cent confidence), which is
significantly lower than the value obtained by Orosz & Bailyn (1997). This
reduced lower bound for the black hole mass together with the high space
velocity of the system is consistent with the idea that it was formed by the
post-supernova collapse of a neutron star.
