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dc.creatorWatson, J. K. G.en_US
dc.date.accessioned2006-06-15T20:09:48Z
dc.date.available2006-06-15T20:09:48Z
dc.date.issued2001en_US
dc.identifier2001-MH-08en_US
dc.identifier.urihttp://hdl.handle.net/1811/20075
dc.description$^{a}$G. Herzberg and J. W. C. Johns, Ap. J. 158, 399 (1969). $^{b}$J. A. Cardelli, B. D. Savage, and D. C. Ebbets, Ap. J. 383, L23 (1991). $^{c}$I. Dabrowski, D. W. Tokaryk, M. Vervloet, and J. K. G. Watson, J. Chem. Phys. 104, 8245 (1996). $^{d}$T. M. Tripp, J. A. Cardelli, B. D. Savage, Ap. J. 107, 645 (1994). $^{e}$S. R. Federman, J. A. Cardelli, E. F. van Dishoeck, D. L. Lambert, and J. H. Black, Ap. J. 445, 325 (1995).en_US
dc.descriptionAuthor Institution: National Research Council of Canadaen_US
dc.description.abstractA far-ultraviolet flash-photolysis spectrum of CH was published in 1969 by $Herzberg and Johns^{a}$, but no rotational assignments were made. From their list of 45 lines in the $3d - X^{2}\Pi$ band, there are three near-coincidences with unidentified (UID) interstellar $lines^{b}$ at 1368.74, 1369.13, and 1370.87 \AA towards the star $\zeta$ Ophiuchi. The spectra of other electronic transitions of CH towards this star are well known, and it was decided to use the interstellar lines as giving the positions of lines with $J^{\prime\prime} = 0.5$, as is found for the other interstellar bands. From this, a rotational analysis of the complete band was possible, using a Rydberg-state program previously used for the ArH and ArD $molecules^{c}$. An interesting aspect of this assignment is that the 1369.13 \AA line is $classified^{d}$ as the only established ultraviolet `diffuse interstellar line' (DIB). Different broadening of different lines is also seen in the laboratory spectrum, and is attributed to predissociation, which is found to be greater for lines with upper levels of d parity, including the DIB, than for lines with upper levels of c parity, consistent with the dominant predissociating state being a $^{2}\Sigma^{-}$ state. From the $n^{*-3}$-dependence of the splittings of the nd complexes, the rotational structure of the $4d - X^{2}\Pi$ band is predicted, and allows the assignment of the UID interstellar line at 1270.96 $\AA^{e}$ to the strongest $J^{\prime\prime} = 0.5$ line of this band.en_US
dc.format.extent298389 bytes
dc.format.mimetypeimage/jpeg
dc.language.isoEnglishen_US
dc.publisherOhio State Universityen_US
dc.titleFAR-ULTRAVIOLET LINES OF INTERSTELLAR CH, INCLUDING ONE DIBen_US
dc.typearticleen_US


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