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Infrared and Millimetric Study of the Young Outflow Cepheus E

AutorMoro-Martín, A.; Noriega-Crespo, A.; Molinari, S.; Testi, Leonardo; Cernicharo, José ; Sargent, A.
Palabras claveStars: formation
Stars: pre-main-sequence
ISM: jets and outflows
Infrared: ISM: lines and bands
Fecha de publicación5-mar-2001
ResumenThe 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.
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