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The experimental data were summarized in
(1) T. Hirao, T. Okabayashi, and M. Tanimoto,
2001, J. Mol. Spectrosc. 208, 148.
The data set includes more accurate Fourier
transform microwave data from
(2) B. Kirchner, H. Huber, G. Steinebrunner,
H. Dreizler, J.-U. Grabow, and I. Merke,
1997, Z. Naturforsch. A 52, 297;
as well as Stark-modulation microwave data from
(3) C. Hirose, K. Okiye, and S. Maeda,
1976, Bull. Chem. Soc. Jpn. 49, 916.
The fit and the parameters are similar to those in (1).
No transition of (1) was assigned a larger uncertainty.
In fact, smaller uncertainties were used for almost all
data from (2) and for all lower frequency data from (1).
Far-infrared transition frequencies were also
included with slightly larger uncertainties than
reported in
(4) M. K. Bane, C. D. Thompson, D. R. T. Appadoo,
and D. McNaughton,
2012, J. Chem. Phys. 137, Art. No. 084306.
These data improve predictions for very high
frequencies somewhat. Predictions with uncertainties
larger than 0.5 MHz should be viewed with
caution. The predictions are deemed to be well
beyond the needs of astronomers.
Spin-statistics matter for the intensities.
The nuclear spin-weight ratio is 5 : 3
for ortho-c-C2H4S
: para-c-C2H4S.
The ortho states are described by
Ka even, the para
states by Ka odd.
The dipole moment was taken from
(5) G. L. Cunningham Jr., A. W. Boyd, R. J. Myers,
W. D. Gwinn, and W. I. Le Van,
1951, J. Chem. Phys. 19, 676 .
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