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The low frequency transitions (up to 0.704 THz) were
taken from
(1) G. Cazzoli, C. Puzzarini, and J. Gauss,
2005, Astrophys. J. Suppl Ser., 159, 181.
Higher frequency transitions (0.632 – 1.965 THz)
were taken from
(2) S. Brünken, U. Fuchs, F. Lewen, S. Urban,
T. Giesen, and G. Winnewisser,
2004, J. Mol. Spectrosc., 225, 152.
Several transitions from (1) have resolved the D or 15N
hyperfine structure to a varying degree. Because of the
small splitting and the low abundance of this species in
astronomical sources no hyperfine splitting was considered
in the predictions. No hyperfine splitting and no excited
vibrational states were considered in the calculation of the
partition function.
The dipole moment was assumed to agree with that of
DCN, see e028509.cat.
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