The tangent point method (TPM) is commonly used to calculate the rotation curve of the inner portion of the Milky Way, relying on the assumption that along one line of sight, the point tangent to the Galactic center is the point where the observed radial velocity is an extremum. This work compares rotation curves derived from the TPM, using neutral hydrogen gas data, and direct measurements of stellar positions and velocities from the Gaia Satellite. The Gaia data indicate that the rotation curve based upon stellar kinematics is much shallower than that previously reported based on the TPM, especially in the inner regions of the Galaxy. Additionally, based on stellar kinematics, the locations of the extremum radial velocities and tangent points often differ. While these results are consistent with previously published simulations, future data from the Gaia satellite will allow for further confidence in determining an accurate rotation curve.

切点法（TPM）常用来计算银河系内部的旋转曲线，它依赖于假设沿着一条视线，与银心相切的点就是观测到的径向速度的点是一个极值。这项工作使用中性氢气数据和来自盖亚卫星的恒星位置和速度的直接测量值比较了从 TPM 得出的旋转曲线。Gaia 数据表明，基于恒星运动学的自转曲线比先前基于 TPM 报告的自转曲线要浅得多，尤其是在银河系的内部区域。此外，基于恒星运动学，极值径向速度和切点的位置通常不同。虽然这些结果与之前公布的模拟结果一致，