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In the coming decade the Gaia satellite will precisely measure the positionsand velocities of millions of stars in the Galactic halo, including stars inmany tidal streams. These streams, the products of hierarchical accretion ofsatellite galaxies by the Milky Way (MW), can be used to infer the Galacticgravitational potential thanks to their initial compactness in phase space.Plans for observations to extend Gaia's radial velocity (RV) measurements tofaint stars, and to determine precise distances to RR Lyrae (RRLe) in streams,would further extend the power of Gaia's kinematic catalog to characterize theMW's potential at large Galactocentric distances. In this work I explore theimpact of these extra data on the ability to fit the potential using the methodof action clustering, which statistically maximizes the information content(clumpiness) of the action space of tidal streams, eliminating the need todetermine stream membership for individual stars. Using a mock halo in a toyspherical potential, updated post-launch error models for Gaia, and estimatesfor RV and distance errors for the tracers to be followed up, I show thatcombining either form of additional information with the Gaia catalog greatlyreduces the bias in determining the scale radius and total mass of the Galaxy,compared to the use of Gaia data alone.

Inferring the Galactic potential with Gaia and friends: synergies with other surveys