  The Magellanic Stream (MS) - an enormous ribbon of gas spanning $140^\circ$
of the southern sky trailing the Magellanic Clouds - has been exquisitely
mapped in the five decades since its discovery. However, despite concerted
efforts, no stellar counterpart to the MS has been conclusively identified.
This stellar stream would reveal the distance and 6D kinematics of the MS,
constraining its formation and the past orbital history of the Clouds. We have
been conducting a spectroscopic survey of the most distant and luminous red
giant stars in the Galactic outskirts. From this dataset, we have discovered a
prominent population of 13 stars matching the extreme angular momentum of the
Clouds, spanning up to $100^\circ$ along the MS at distances of $60-120$ kpc.
Furthermore, these kinemetically-selected stars lie along a
[$\alpha$/Fe]-deficient track in chemical space from $-2.5 < \mathrm{[Fe/H]} <
-0.5$, consistent with their formation in the Clouds themselves. We identify
these stars as high-confidence members of the Magellanic Stellar Stream. Half
of these stars are metal-rich and closely follow the gaseous MS, whereas the
other half are more scattered and metal-poor. We argue that the metal-rich
stream is the recently-formed tidal counterpart to the MS, and speculate that
the metal-poor population was thrown out of the SMC outskirts during an earlier
interaction between the Clouds. The Magellanic Stellar Stream provides a strong
set of constraints - distances, 6D kinematics, and birth locations - that will
guide future simulations towards unveiling the detailed history of the Clouds.
