  We present imaging observations at 1.3 millimeters of the debris disk
surrounding the nearby M-type flare star AU Mic with beam size 3 arcsec (30 AU)
from the Submillimeter Array. These data reveal a belt of thermal dust emission
surrounding the star with the same edge-on geometry as the more extended
scattered light disk detected at optical wavelengths. Simple modeling indicates
a central radius of ~35 AU for the emission belt. This location is consistent
with the reservoir of planetesimals previously invoked to explain the shape of
the scattered light surface brightness profile through size-dependent dust
dynamics. The identification of this belt further strengthens the kinship
between the debris disks around AU Mic and its more massive sister star beta
Pic, members of the same ~10 Myr-old moving group.
