  The Cepheus E outflow has been studied in the mid and far infrared using the
ISO CAM and LWS instruments, and at millimetric wavelengths using OVRO. In the
near and mid-IR, its morphology is similar to that expected for a jet driven
outflow, where the leading bow shocks entrain and accelerate the surrounding
molecular gas. As expected, fine structure atomic/ionic emission lines arise
from the bow shocks, at both the Mach Disk and the stagnation tip, where
J-shocks are dominant. The H2, H2O and CO molecular emission could arise
further `downstream' at the bow shock wings where the shocks (v = 8-35 km/s)
are oblique and more likely to be C-type. The 13CO emission arises from
entrained molecular gas and a compact high velocity emission is observed,
together with an extended low velocity component that almost coincides
spatially with the H2 near-IR emission. The millimetric continuum emission
shows two sources. We identify one of them with IRAS 23011+6126, postulating is
the driver of the Cepheus E outflow; the other, also an embedded source, is
likely to be driving one of other outflows observed in the region.
