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We present results from an extensive spectroscopic survey of field stars inthe Small Magellanic Cloud (SMC). 3037 sources, predominantly first-ascent redgiants, spread across roughly 37.5 sq. deg, are analysed. The line of sightvelocity field is dominated by the projection of the orbital motion of the SMCaround the LMC/Milky Way. The residuals are inconsistent with both anon-rotating spheroid and a nearly face on disk system. The current sample andprevious stellar and HI kinematics can be reconciled by rotating disk modelswith line of nodes position angle, theta, ~ 120-130 deg., moderate inclination(i ~ 25-70 deg.), and rotation curves rising at 20-40 km/s/kpc. The metal-poorstars exhibit a lower velocity gradient and higher velocity dispersion than themetal-rich stars. If our interpretation of the velocity patterns as bulkrotation is appropriate, then some revision to simulations of the SMC orbit isrequired since these are generally tuned to the SMC disk line-of-nodes lying ina NE-SW direction. Residuals show strong spatial structure indicative ofnon-circular motions that increase in importance with increasing distance fromthe SMC centre. Kinematic substructure in the north-west part of our surveyarea is associated with the tidal tail or Counter-Bridge predicted bysimulations. Lower line-of-sight velocities towards the Wing and the largervelocities just beyond the SW end of the SMC Bar are probably associated withstellar components of the Magellanic Bridge and Counter-Bridge, respectively.Our results reinforce the notion that the intermediate-age stellar populationof the SMC is subject to substantial stripping by external forces.

Red Giants in the Small Magellanic Cloud. I. Disk and Tidal Stream Kinematics