Transition frequencies were reported by
(1) H. S. P. Müller, A. Maeda, S. Thorwirth, F. Lewen, S. Schlemmer, I. R. Medvedev, M. Winnewisser, F. C. De Lucia, and E. Herbst, 2019, Astron. Astrophys. 621, Art. No. A143.
Higher order distortion parameters were estimated as detailed in (1) and were kept fixed in the fit. This entry is sufficiently accurate for all astronomical purposes. Transition frequencies with calculated uncertainties exceeding 0.2 MHz should be viewed with caution.
The dipole moment was assumed to agree with that of the main species, see e046509.cat.
At low temperatures, it may be necessary to discern between ortho-H₂C³⁶S and para-H₂C³⁶S. The ortho states are described by K_a odd, the para states by K_a even. The nuclear spin-weights are 3 and 1 for ortho-H₂C³⁶S and para-H₂C³⁶S, respectively. The J_KaKc = 1₁₁ is the lowest ortho state. It is 10.2643 cm^–1 above ground.