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The lines have been reported by
(1) H. Odashima, D. Wang, F. Matsushima, S. Tsunekawa, and K. Takagi,
1995, J. Mol. Spectrosc. 171, 513; and by
(2) T. Okabayashi and M. Tanimoto,
2000, Astrophys. J. 543, 275.
In contrast to (1) we were able to determine the centrifugal
distortion constant L.
Extrapolations to J > 18 should be viewed with caution
because of the large centrifugal distortion effects.
The 39K 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" |
404445.1762 | 0.0109 | –0.7442 | 2 – 1 |
404445.2833 | 0.0120 | –0.7108 | 3 – 3 |
404446.2184 | 0.0160 | –1.6650 | 2 – 3 |
404446.4939 | 0.0102 | –0.7442 | 1 – 1 |
404446.6180 | 0.0085 | –0.3428 | 3 – 2 |
404446.6222 | 0.0095 | –0.0629 | 4 – 3 |
404447.5531 | 0.0121 | –0.6370 | 2 – 2 |
404448.8707 | 0.0196 | –1.4431 | 1 – 2 |
The dipole moment is from an ab initio calculation by
(3) S. R. Langhoff, C. W. Bauschlicher, and H. Partridge,
1986, J. Chem. Phys. 85, 5158.
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