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The dark matter halo of the Milky Way is expected to be triaxial and filledwith substructure. It is hoped that streams or shells of stars produced bytidal disruption of stellar systems will provide precise measures of thegravitational potential to test these predictions. We develop a method forinferring the Galactic potential with tidal streams based on the idea that thestream stars were once close in phase space. Our method can flexibly adapt toany form for the Galactic potential: it works in phase-space rather thanaction-space and hence relies neither on our ability to derive actions nor onthe integrability of the potential. Our model is probabilistic, with alikelihood function and priors on the parameters. The method can properlyaccount for finite observational uncertainties and missing data dimensions. Wetest our method on synthetic datasets generated from N-body simulations ofsatellite disruption in a static, multi-component Milky Way including atriaxial dark matter halo with observational uncertainties chosen to mimiccurrent and near-future surveys of various stars. We find that with just fourwell-measured stream stars, we can infer properties of a triaxial potentialwith precisions of order 5-7 percent. Without proper motions we obtain 15percent constraints on potential parameters and precisions around 25 percentfor recovering missing phase-space coordinates. These results are encouragingfor the eventual goal of using flexible, time-dependent potential modelscombined with larger data sets to unravel the detailed shape of the dark matterdistribution around the Milky Way.

Inferring the gravitational potential of the Milky Way with a few precisely measured stars