distant halo stars has been almost entirely based on one velocity component. For large enough samples over a wide area of sky, kinematic signatures such as rotation can be teased out using line-of-sight velocities alone. However, at larger and larger radii this line-of-sight component gives less and less information on the azimuthal velocities of the halo stars. Moreover, the presence of cold structures in line-of-sight velocity space [@schlaufman09] can also bias results. It is clearly more desirable to infer a direct rotation estimate from the 3D kinematics of the stars. Studies of distant halo stars with proper motion measurements are scarce [@deason13; @koposov13; @sohn15; @sohn16], but this limitation will become a distant memory as we enter the era of *Gaia*.

*Gaia* is an unprecedented astrometric mission that will measure proper motions for hundreds of millions of stars in our Galaxy. In this contribution, we exploit the first data release of *Gaia* (DR1, @gaia16) to measure the net rotation of the Milky Way stellar halo. Although the first *Gaia* data release does not contain any proper motions, we combine the exquisite astrometry of DR1 with the Sloan Digital Sky Survey (SDSS) images taken some $\sim 10-15$ years earlier to provide a 