HERSCHEL OBSERVATIONS OF EXTRA-ORDINARY SOURCES (HEXOS): ANALYSIS OF THE HIFI 1.2 THZ WIDE SPECTRAL SURVEY TOWARD ORION KL

Author Institution: Department of Astronomy, University of Michigan, 500 Church Street, Ann Arbor, MI 48109, USA; California Institute of Technology, Cahill Center for Astronomy and Astrophysics 301-17, Pasadena, CA 91125 USA; Jet Propulsion Laboratory, Caltech, Pasadena, CA 91109, USA; Centro de Astrobiologia (CSIC/INTA), Laboratiorio de Astrofisica Molecular, Ctra. de Torrejon a Ajalvir, km 4 28850, Torrejon de Ardoz, Madrid, Spain; Infrared Processing and Analysis Center, California Institute of Technology, MS 100-22, Pasadena, CA 91125; Department of Physics and Astronomy, University of Calgary, 2500 University Drive NW, Calgary, AB T2N 1N4, Canada; Physikalisches Institut, Universitat zu Koln, Zulpicher Str. 77, 50937 Koln, Germany; SRON Netherlands Institute for Space Research, PO Box 800, 9700 AV, Groningen, The NetherlandsWe present a full spectral survey of the Kleiman-Low nebula within the Orion Molecular Cloud (Orion KL), one of the most chemically rich regions in the galaxy, using the HIFI instrument on board the Herschel Space Observatory. These observations span a frequency range of 490 -- 1240~GHz and 1430 -- 1900~GHz at a spectral resolution of 1.1~MHz (corresponding to 0.7-0.2~km/s). These observations encompass the largest spectral coverage ever obtained of a star-forming region in the sub-mm with high spectral resolution. As a result, we are sensitive to lines with excitation energies over an unprecedented range observed with the same instrument and near uniform efficiency. Reliable multi-transitional studies using hundreds to thousands of lines emitted by the same molecule can therefore be carried out. We will present the results of a full band analysis of this survey exploring the spectral emissions of over 20 molecules within this range. Initial results hint at the presence of excitation gradients. In addition, some species exhibit emissions at very high energies ($>$ few hundred~K) and temperatures, while others only probe warm ($\sim$100~K) regions along the line of sight. These facets will be combined with an exploration of molecular origins in hot gas