The data were taken from
(1) L. Margulès, M. A. Martin-Drumel, O. Pirali, S. Bailleux, G. Wlodarczak, P. Roy, E. Roueff, and M. Gerin, 2016, Astron Astrophys. 591, Art. No. A110.
Some parameters were kept fixed to value from the main species.
Since ¹⁵N is quite rare in molecular clouds, the entry should be well sufficient for all astronomical observations. Predictions with uncertainties larger than 0.5 MHz should be viewed with some caution, those with uncertainties larger than 10 MHz with great caution.
The dipole moment was assumed to agree with that of the main isotopolog, see e014501.cat.
At low temperatures, it may be necessary to discern between ortho-¹⁵NH₂ and para-¹⁵NH₂. The ortho states are described by K_a + K_c even, the para states by K_a + K_c odd. There are three times as many levels for ortho-¹⁵NH₂ than there are for para-NH₂. Thus, for transitions with unresolved ¹H hyperfine splitting the nuclear spin-weight ratio is 3 : 1 between ortho-¹⁵NH₂ and para-¹⁵NH₂. However, for transitions with resolved ¹H hyperfine splitting no non-trivial spin-statistics have to be considered. The N_KaKc = 1₀₁; J, F₁ = 1.5, 2 is the lowest para state. It is 21.0864 cm^–1 above ground. Separate para and ortho predictions are available along with separate para and ortho partition function values. NOTE: The redundant quantum number I_tot has been omitted !