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The observed frequencies and the theoretical value
for the dipole moment were taken from
(1) P. Botschwina, Ä. Heyl, W. Chen, M. C. McCarthy,
J.-U. Grabow, M. J. Travers, and P. Thaddeus,
1998, J. Chem. Phys. 109, 3108.
With respect to the first entry of May 2001, rest frequencies
from astronomical observations were added. With respect to
the second entry of Oct. 2020, slightly improved and extended
rest frequencies from astronomical observations were taken
from
(2) R. Fuentetaja, C. Cabezas, Y. Endo, M. Agúndez,
B. Tercero, N. Marcelino, P. de Vicente, and J. Cernicharo,
2024, Astron. Astrophys. 688, Art. No. L29.
The small 14N hyperfine splitting has been resolved
in the laboratory experiments.
The calculations should be accurate enough for all observations.
They should be viewed with caution if the calculated uncertainties
are larger than 0.1 MHz.
14N hyperfine splitting may matter
in astronomical observations. Therefore, a
separate hyperfine calculation is provided for
J' ≤ 14 below 40 GHz.
NOTE: The partition function
does take into account the spin multiplicity
of the 14N nucleus !
The dipole moment is from a quantum chemical calculatioj in (1).
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