Blake, Geoffrey A. and Sutton, E. C. and Masson, C. R. and Phillips, T. G. and Herbst, Eric and Plummer, Grant M. and De Lucia, Frank C. (1984) ^(13)CH_3OH in OMC-1. Astrophysical Journal, 286 . pp. 586-590. ISSN 0004-637X. http://resolver.caltech.edu/CaltechAUTHORS:20120912-070230231
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We report the identification of several previously unidentified or misidentified lines toward OMC-1 as components the J = 5 → 4 α-type band of ^(13)CH_30H, deduced by combining accurate laboratory spectroscopy with sensitive broad-band astronomical line searches. An LTE fit to the data yields a rotational temperature of T_(rot)~ 120 K and a ^(13)CH_30H column density of ~1.3 x 10^(15) cm^(-2), averaged over a 30" beam. A ^(12)C/^(13)C ratio of ~30 is derived. The assignment of the feature at 236063 MHz to the blended K = ±2 E transitions of ^(13)CH_30H, rather than to CO^+, removes a major discrepancy between observation and the predictions of ion-molecule chemical models of dense interstellar clouds.
|Additional Information:||© 1984 American Astronomical Society. Provided by the NASA Astrophysics Data System. Received 1984 April 3; accepted 1984 June 4. Single dish millimeter-wave astronomy at the Owens Valley Radio Observatory is supported by NSF grant AST 82-14693.The authors would also like to thank R. E. Miller of AT & T Bell Laboratories, Murray Hill, for supplying the SIS junctions used in this work. E. H., G. M. P., and F. C. D. L. acknowledge support from NASA via grant NAGW-189. E. H. also wishes to acknowledge the support of the NSF via grant AST 83-12270 for his theoretical program.|
|Subject Keywords:||interstellar: abundances; interstellar: molecules; line identifications|
|Official Citation:||C-13H3OH in OMC-1 Blake, G. A., Sutton, E. C., Masson, C. R., Phillips, T. G., Herbst, E., Plummer, G. M., , Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 286, Nov. 15, 1984, p. 586-590.|
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|Deposited By:||Ruth Sustaita|
|Deposited On:||12 Sep 2012 15:02|
|Last Modified:||26 Dec 2012 16:09|
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