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The experimental data were taken from
(1) J. Demaison, I. Pohl, H. D. Rudolph,
1985, J. Mol. Spectrosc. 114, 210.
With respect to the first entry from Nov. 2018,
hyperfine transition frequencies were added.
These were reported by
(2) B. A. McGuire, A. M. Burkhardt, R. A. Loomis,
C. N. Shingledecker, K. L. K. Lee, S. B. Charnley,
M. A. Cordiner, E. Herbst, S. Kalenskii, E. Momjian,
E. R. Willis, C. Xue, A. J. Remijan, and M. C. McCarthy,
2020, Astrophys. J. Lett. 900, Art. No. L10.
Some lines from (2) and (1) with large residuals were omitted
from the fit. The parameter set differs somewhat from that in (1).
The calculations are probably sufficient for all astronomers.
Transition frequencies with calculated uncertainties larger than
0.2 MHz should be viewed with caution.
A
separate hyperfine calculation is provided for
J ≤ 11 and frequencies below 52 GHz.
NOTE: The partition function takes
into account the spin multiplicity of the 14N nucleus.
The dipole moment was determined in (1).
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