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The experimental lines are from
(1) Y. Hirahara, Y. Ohshima, and Y. Endo,
1994, J. Chem. Phys. 101, 7342.
With respect to the first entry from Feb. 2018, transition
frequencies from astronomical observations were added.
These were reported by
(2) R. Fuentetaja, M. Agúndez, C. Cabezas, B. Tercero,
N. Marcelino, J. R. Pardo, P. de Vicente, and J. Cernicharo,
2022, Astron. Astrophys. 667, Art. No. L4.
The reported uncertainties of 10 kHz were slightly
optimistic and were doubled.
The spin-orbit splitting is very uncertain. Therefore,
calculations for the higher Π1/2 spin
component were omitted. In addition, calculations were
truncated above 180 GHz. Caution is advised for
calculations higher than 93 GHz.
The dipole moment is from an estimate based on
ab initio calculations by
(3) H. S. P. Müller, 2018, unpublished;
and should be taken cautiously.
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