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dc.creator Moro-Martín, A.
dc.creator Noriega-Crespo, A.
dc.creator Molinari, S.
dc.creator Testi, Leonardo
dc.creator Cernicharo, José
dc.creator Sargent, A.
dc.date 2008-01-09T16:06:18Z
dc.date 2008-01-09T16:06:18Z
dc.date 2001-03-05
dc.date.accessioned 2017-01-31T00:59:39Z
dc.date.available 2017-01-31T00:59:39Z
dc.identifier arXiv:astro-ph/0103065v1
dc.identifier http://hdl.handle.net/10261/2663
dc.identifier.uri http://dspace.mediu.edu.my:8181/xmlui/handle/10261/2663
dc.description 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.
dc.description Peer reviewed
dc.format 710901 bytes
dc.format application/pdf
dc.language eng
dc.relation Preprint
dc.rights openAccess
dc.subject Stars: formation
dc.subject Stars: pre-main-sequence
dc.subject ISM: jets and outflows
dc.subject Infrared: ISM: lines and bands
dc.title Infrared and Millimetric Study of the Young Outflow Cepheus E
dc.type Pre-print


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