  We present a combined analysis of the kinematics of the Large Magellanic
Cloud through its HI gas, carbon stars, and red supergiant stars. After
correcting the line-of-sight velocities for the recent accurate measurement of
the LMC's space motion, we find that each kinematic tracer clearly defines a
flat rotation curve with similar shape but different amplitude for each tracer:
61 km/s for the carbon stars, 80 km/s for the HI, and 107 km/s for the red
supergiants. Previously identified tidal HI features are seen to harbor
numerous carbon stars, with the tidally disturbed stars comprising 7-15% of the
total sample. This discovery implies that we cannot depend on the carbon star
sample alone to construct a reliable model of the LMC's gravitational
potential. We also find red supergiants with peculiar kinematics, but their
association with tidal features is unclear, and may instead be interacting with
supergiant HI shell SGS4. In addition, although the local velocity dispersion
of the red supergiants is small, ~8 km/s, their velocity dispersion about the
carbon star rotation solution is 17 km/s, equal to the velocity dispersion of
the carbon stars themselves. We thus appear to be witnessing the tidal heating
of the LMC's stellar disk.
