The cumulative mass profile of the Milky Way's dark matter halo is one of the most fundamental properties of the Galaxy. However, estimating this property is not an easy problem, as evidenced by the range of results present in the literature. There are many methods for estimating the Milky Way's mass, but I will focus on our method, which relies on a Bayesian analysis, a physical model, and the kinematic information of Galactic satellites. One issue with using kinematic data is that they are incomplete and subject to significant measurement uncertainty. The advantage of using the Bayesian approach is two-fold: we can incorporate both the incomplete kinematic data and the measurement errors using a hierarchical model. In this seminar, I will explain our method and will present preliminary results of our estimate for the Milky Way's mass profile.