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The O-protonated nitrous oxide is much lower in energy
than the N-protonated nitrous oxide. The transition
frequencies were reported by
(1) M. Bogey, C. Demuynck, J.-L. Destombes,
and A. R. W. McKellar,
1986, Astron. Astrophys. 167, L13.
Frequencies of the hyperfine resolved J =
1 – 0 transition were
published by
(2) M. C. McCarthy and P. Thaddeus,
2010, J. Mol. Spectrosc. 263, 71.
Additional data were given in the supplementary
material of
(3) M. Bogey, C. Demuynck, and J.-L. Destombes,
1988, J. Chem. Phys. 88, 2108.
Unfortunately, these data are not accessible anymore.
The predictions were truncated above
Ka = 4.
The quality of the predictions may be sufficient
for all astronomical purposes, at least for fairly
cold environments. Predictions with uncertainties
larger than 0.5 MHz should be viewed with caution.
14N hyperfine splitting can be resolved
at low quantum numbers. Therefore, a separate
calculation with
14N hyperfine splitting is provided
up to J" = 2 together with
partition function values.
The ab initio dipole moment value was reported
by
(4) X. Huang, R. C. Fortenberry, and T. J. Lee,
2013, J. Chem. Phys. 139, Art. No. 084313.
The molecules has a large b-dipole moment component
(2.18 D), but transitions can not be predicted with confidence
from the present data.
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