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The lines have been reported by
(1) K. R. Leopold, L. R. Zink, K. M. Evenson, and D. A. Jennings,
1987, J. Mol. Spectrosc. 122, 150; and by
(2) T. Okabayashi and M. Tanimoto,
2000, Astrophys. J. 543, 275.
Extrapolations to J > 10 should be viewed with caution
because of the large centrifugal distortion effects.
The 23Na hyperfine splitting was resolved for the
J = 1 – 0 transition only.
It may be resolvable for the J = 2 – 1 transitions.
The calculated frequencies, uncertainties, and intensities are given below.
| frequency | unc. | int. | F' – F" |
579481.2428 | 0.0161 | –0.4574 | 2 – 1 |
579481.3239 | 0.0169 | –0.4239 | 3 – 3 |
579482.2598 | 0.0188 | –1.3782 | 2 – 3 |
579482.6049 | 0.0152 | –0.4574 | 1 – 1 |
579482.7900 | 0.0138 | –0.0560 | 3 – 2 |
579482.8159 | 0.0141 | –0.2239 | 4 – 3 |
579483.7258 | 0.0158 | –0.3502 | 2 – 2 |
579485.0880 | 0.0203 | –1.1563 | 1 – 2 |
The dipole moment is from
(3) E. S. Sachs, J. Hinze, and N. H. Switalski,
1975, J. Chem. Phys. 62, 3367.
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