Infrared and Millimetric Study of the Young Outflow Cepheus E
by
A. Moro-Martin(1), A. Noriega-Crespo(2), S. Molinari (3), L. Testi (4), J. Chernicharo (5), A. Sargent (6)
(1) Steward Observatory, University of Arizona, Tucson, Az 85721
(2) SIRTF Science Center, Caltech, MS 100-22, Pasadena, CA 91125
(3) Infrared Processing and Analysis Center, Caltech MS 100-22, Pasadena, CA 91125
(4) Osservatorio Astrofisico di Arcetri,
Largo Enrico Fermi 5, I-50125 Firenze, Italy
(5) Instituto de Estructura de la Materia, CSIC, Calle Serrano 40, Madrid, Spain
(6) Department of Mathematics, Physics and Astronomy,
California Institute of Technology, MS105-24, Pasadena, CA 91125
Abstract:
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 = $8 - 35$ \kms) 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 {\it 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~\mum~emission must originate
from an extended photo-dissociation region, very likely excited by the nearby
Cepheus OB3 association.
Mantained by:
Leonardo Testi