A λ = 1.3 Millimeter Aperture Synthesis Molecular Line Survey of Orion Kleinmann-Low

Creators: Blake, Geoffrey A.; Mundy, L. G.; Carlstrom, J. E.; Padin, S.; Scott, S. L.; Scoville, N. Z.; Woody, D. P.

Abstract

We present a 1".3 spatial resolution interferometric spectral line survey of the core of the Orion molecular cloud, obtained with the OVRO millimeter array. Covering 4 GHz bandwidth in total, the survey contains ~100 emission lines from 18 chemical species. The spatial distributions of a number of molecules point to source I near the IRc2 complex as the dominant energy source in the region but do not rule out the presence of additional lower luminosity objects. At arcsecond resolution, the offsets between dust emission and various molecular tracers suggest that the spectacular "hot core" emission in the Orion core arises via the heating and ablation of material from the surfaces of very high density clumps located ≳500 AU from source I and traced by the dust emission. We find no evidence for a strong internal heating source within the hot core condensation(s).

Additional Information

© 1996 American Astronomical Society. Received 1996 May 16; accepted 1996 September 6. Millimeter interferometry at OVRO is supported by the NSF, grant AST-9314079. G. A. B. would like to acknowledge additional support from NASA, grants NAGW-1955 and NAGW-2297, while L. G. M. acknowledges support from NSF grant AST-9314847 and NASA grant NAGW-3066. J. E. C. acknowledges support from the NSF-YI program and the David & Lucille Packard Foundation. L. G. M. and G. A. B. gladly thank Leiden Observatory for their hospitality during the course of this work.

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Published - 1996ApJ___472L__49B.pdf

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