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Transition frequencies were reported by
(1) Y. Motoki, F. Isobe, H. Ozeki, and K. Kobayashi,
2014, Astron. Astrophys. 566, Art. No. A28.
Also included in the analysis were most data
from
(2) R. Pearson, Jr. and F. J. Lovas,
1977, J. Chem. Phys. 66, 4149.
Data with uncertainties of 100 kHz or more
were not merged.
The predictions should be accurate enough for all
radioastronomical observations. Specifically,
predictions with uncertainties larger than
0.3 MHz should be viewed with some caution.
14N hyperfine splitting may matter
in astronomical observations. Therefore, a
separate hyperfine calculation is provided for
J' ≤ 20 and
Ka' ≤ 5 up to 1 THz.
NOTE: The
partition function does take into account
the spin multiplicity of the 14N
nucleus !
The dipole moment components were derived in (1)
from those of the main species reported by
(3) M. Allegrini, J. W. C. Johns, and
A. R. W. McKellar,
1979, J. Chem. Phys. 70, 2829.
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