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 H _ { 2 } , H _ { 2 } O and CO molecular emission could arise further ‘ downstream ’ at the bow shock wings where the shocks ( v = 8 - 35 km s ^ { -1 } ) are oblique and more likely to be C-type .
The ^ { 13 } CO 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 H _ { 2 } 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 .
Finally , we suggest that the strong [ C II ] 158 \mu m emission must originate from an extended photo-dissociation region , very likely excited by the nearby Cepheus OB3 association .