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dc.contributor.authorGoicoechea, Javier R.-
dc.contributor.authorCernicharo, José-
dc.contributor.authorDaniel, Fabien-
dc.contributor.authorBarlow, Michael J.-
dc.contributor.authorSwinyard, Bruce M.-
dc.contributor.authorLim, Tanya L.-
dc.contributor.authorViti, S.-
dc.contributor.authorYates, J.-
dc.descriptionAccepted in ApJ letters, 2006 March 2en_US
dc.description.abstractAs part of the first far-IR line survey towards Orion KL, we present the detection of seven new rotationally excited OH Lambda-doublets (at 48, 65, 71, 79, 98 and 115 um). Observations were performed with the Long Wavelength Spectrometer (LWS) Fabry-Perots on board the Infrared Space Observatory (ISO). In total, more than 20 resolved OH rotational lines, with upper energy levels up to 620 K, have been detected at an angular and velocity resolutions of 80$'' and 33 km s^-1 respectively. OH line profiles show a complex behavior evolving from pure absorption, P-Cygni type to pure emission. We also present a large scale 6' declination raster in the OH ^2\Pi_3/2 J=5/2^+-3/2^- and ^2\Pi_3/2 J=7/2^-5/2^+ lines (at 119.441 and 84.597 um) revealing the decrease of excitation outside the core of the cloud. From the observed profiles, mean intrinsic line widths and velocity offsets between emission and absorption line peaks we conclude that most of the excited OH arises from Orion outflow(s), i.e. the ``plateau'' component. We determine an averaged OH abundance relative to H_2 of X(OH)=(0.5-1.0)x10^-6, a kinetic temperature of 100 K and a density of n(H_2)=5x10^5 cm^-3. Even with these conditions, the OH excitation is heavily coupled with the strong dust continuum emission from the inner hot core regions and from the expanding flow itself.en_US
dc.format.extent747560 bytes-
dc.subjectInfrared: ISMen_US
dc.subjectISM: individual (Orion KL)en_US
dc.subjectISM: jets and outflowsen_US
dc.subjectISM: moleculesen_US
dc.subjectRadiative transferen_US
dc.titleFar-IR Excited OH Lines from Orion KL Outflowsen_US
dc.description.peerreviewedPeer revieweden_US
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