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This theory was developed by W. D. Watson [Rev. Mod. Phys. 48, 513 (1976)]. Observations have been summarized, for example, by W. M. Irvine and R. F. Knacke (26) and E. F. van Dishoeck, G. A. Blake, B. T. Draine, and J. I. Lunine [in Protostars and Planets III, E. H. Levy and J. I. Lunine, Eds. (Univ. of Arizona Press, Tucson, 1993), pp. 163-241].
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The Submillimetre Common-User Bolometer Array (SCUBA) for JCMT. SCUBA can also observe at 450 μm with an array of 91 bolometers
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The Submillimetre Common-User Bolometer Array (SCUBA) for JCMT. SCUBA can also observe at 450 μm with an array of 91 bolometers.
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-1, consistent with low-resolution CO velocity maps of that area (28). In control measurements without the comet, we recovered all CO lines attributed to the cloud and demonstrated that an HCN 4-3 line (or any line other than CO lines) from the background sources was not detectable down to the 1% level relative to the cometary line at any of the positions of the comet. Summarizing, we exclude a contamination by emissions from the Taurus clouds for the following reasons: (i) Potential DCN lines from the cloud were either blueshifted or redshifted relative to the cometary line. (ii) For none of the positions in the cloud could we detect the HCN 4-3 or any line other than CO. (iii) On the basis of the Jet Propulsion Laboratory line atlas (29), there exists no line that - in the velocity frame of the cloud - may have serendipitously interfered with the cometary DCN position. (iv) Even if there were such a line, the observed FWHM still suggests a cometary origin because lines from the cloud are about half as wide. We were pointing 2° northwest of the deuterium-rich clumps TMC1 and TMC2.
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7144230034
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We thank the operators of the JCMT for their assistance, B. Marsden and D. Tholen for help with the ephemerides, and P. Eberhardt for valuable comments on the manuscript. Supported by NASA grants NAEW 2650 and NAEW 2631. D.C.J. acknowledges support from NSF grant AST96-15603, The JCMT is operated by the Joint Astronomy Centre on behalf of the Particle Physics and Astronomy Research Council of the United Kingdom, the Netherlands Organisation for Scientific Research, and the National Research Council of Canada.
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