  The debris disk closest to Earth is the one around the star epsilon Eridani
at a distance of 3.2 pc. It is the prime target for detailed studies of a belt
of planetesimals left from the early phase of planet formation other than the
Kuiper Belt. The non-uniform ring-like structure around epsilon Eridani,
originally discovered at lambda=850 microns with the bolometer camera SCUBA,
could be the signpost of unseen long-period planets interior to the disk that
gravitationally interact with it through mean-motion resonances. However, the
reliability of the structure at 850 microns, which has been debated, has not
been verified with independent observations until now. We present a high
signal-to-noise ratio image of this structure at lambda=1.2 mm made with the
bolometer camera MAMBO and compare this with the SCUBA image. We have found
that three of the four emission clumps (NE, NW, SW) and the two deep hollows to
the east and west are at the same positions in the MAMBO and SCUBA images
within astrometric uncertainty. The SE clump is at odds, significantly brighter
and more extended in the SCUBA than in the MAMBO images, but it is possible
that this mismatch is an artifact. We conclude that this degree of positional
coincidence provides tentative evidence that the observed structure is robust.
In addition, we present the radial brightness profile of our MAMBO image and
show that the width of the planetesimal belt around epsilon Eridani is narrower
than 22 AU, a more stringent upper limit than determined from previous
observations. The corresponding relative width is $0.1 < \Delta R / R < 0.4$,
which is lower than for the Kuiper Belt.
