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 McClintock 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 data sets 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. data set, 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. data set and allows reasonable fits to the McClintock et al. data set with near-maximal spin for system distances greater than ∼10 kpc. We discuss the uncertainties and implications of these estimates.

我们使用连续拟合方法估计 GRS 1915+105 中的黑洞自旋参数，该方法基于到该源的距离的超长基线干涉视差测量，并具有修正的质量和倾角约束。我们拟合了被选择为吸积盘主导的光谱状态的 Rossi X 射线时序探索器观测值，如 McClintock 等人所述。(2006) 和 Middleton 等人。(2006)，之前用这种方法给出了不一致的自旋估计。我们发现，使用新的系统参数，两个数据集中的自旋都增加了，为Middleton 等人提供了a _* = 0.86的最佳自旋。数据和麦克林托克等人的拟合不佳。数据集，它与一个 _*的 BHSPEC 模型限制挂钩= 0.99。我们探讨了系统参数中不确定性的影响，表明Middleton 等人的最佳自旋范围从a _* = 0.4 到 0.99。数据集并允许对 McClintock 等人的合理拟合。系统距离大于 10 kpc 时具有接近最大自旋的数据集。我们讨论了这些估计的不确定性和影响。