The data set was summarized in
(1) C. Vastel, K. Kawaguchi, D. Quénard, M. Ohishi, B. Lefloch, R. Bachiller, H. S. P. Müller, 2018, Mon. Not. R. Astron. Soc. 474, L76.
Besides earlier unpublished millimeter data, the line list contains extensive lower frequency data from
(2) Y. Hirahara, Y. Ohshima, Y. Endo, 1993, Astrophys. J. 403, L83.
Detailed ¹⁴N hyperfine splitting was resolved in (2). One poorly fitting lines from (2) was omitted.
The predictions should be accurate enough for all observations. Predictions with calculated uncertainties larger than 0.2 MHz should be viewed with caution.
¹⁴N hyperfine splitting may matter in astronomical observations. Therefore, a separate hyperfine calculation is provided for J' ≤ 6 below 60 GHz. NOTE: The partition function does take into account the spin multiplicity of the ¹⁴N nucleus !
The dipole moment is from a quantum chemical calculation by
(3) P. Botschwina, M. Horn, S. Seeger, and J. Flügge, 1992, Chem. Phys. Lett. 195, 427.