The first entry from Feb. 2017 was revised. The experimental data have been taken from
(1) L. Kolesniková, E. R. Alonso, S. Mata, J. Cernicharo, and J. L. Alonso, 2017, Astrophys. J. Suppl. Ser. 233 Art. No. 24..
Additional data were taken from
(2) B. E. Arenas, S. Gruet, A. L. Steber, B. M. Giuliano, and M. Schnell, 2017, Phys. Chem. Chem. Phys., 19 1751.
Initial parameters were taken from
(3) H. S. P. Müller, A. Coutens, A. Walters, J.-U. Grabow, and S. Schlemmer, 2011, J. Mol. Spectrosc., 267 100;
in particular, higher order parameters were kept from that work. Most of the uncertainties in (1) were deemed to be slightly conservative.
¹⁴N hyperfine splitting may be resolvable for some transitions at MW frequencies, but is unlikely to be resolved in astronomical observations. The HFS pattern is expected to be very close to that of the main species, see e069506.cat.
Predictions should be sufficient for secure identification in the ISM up to around 300 GHz. They have been truncated at J = 60. Predictions with higher J or higher K_a as well as those with calculated uncertainties exceeding 0.2 MHz should be viewed with caution.
The dipole moment components were assumed to agree with those of the main species, see e069506.cat.