  We estimate the black hole spin parameter in GRS 1915+105 using the
continuum-fitting method with revised mass and inclination constraints based on
the very long baseline interferometric parallax measurement of the distance to
this source. We fit Rossi X-ray Timing Explorer observations selected to be
accretion disk-dominated spectral states as described in McClinotck et al.
(2006) and Middleton et al. (2006), which previously gave discrepant spin
estimates with this method. We find that, using the new system parameters, the
spin in both datasets increased, providing a best-fit spin of $a_*=0.86$ for
the Middleton et al. data and a poor fit for the McClintock et al. dataset,
which becomes pegged at the BHSPEC model limit of $a_*=0.99$. We explore the
impact of the uncertainties in the system parameters, showing that the best-fit
spin ranges from $a_*= 0.4$ to 0.99 for the Middleton et al. dataset and allows
reasonable fits to the McClintock et al. dataset with near maximal spin for
system distances greater than $\sim 10$ kpc. We discuss the uncertainties and
implications of these estimates.
