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The observed transition frequencies were taken from
(1) M. C. McCarthy and P. Thaddeus,
2002, Astrophys. J. 569, L55;
and from astronomical observations by
(2) R. Fuentetaja, M. Agúndez, C. Cabezas, B. Tercero,
N. Marcelino, J. R. Pardo, P. de Vicente, and J. Cernicharo,
2022, Astron. Astrophys. 667, Art. No. L4.
Uncertainties in (1) were conservative for the most part and
were changed from 2 to 1 kHz. Uncertainties in (2) were
too optimistic and were changed from 10 to 20 kHz to
20 to 50 kHz. Two lines from (1) and one line from (2)
with large residuals were omitted from the line list.
The parameter set differs slightly from that in (1) and (2).
Transitions were limited to J ≤ 40 because of the
limited line list. The a-type transitions were
truncated at Ka = 10 and b-type
transitions at Ka = 2.
The calculations are sufficiently accurate for observations of
cold sources and may be sufficient for luke-warm sources.
Transition frequencies with calculated uncertainties
exceeding 0.1 MHz should be viewed with caution.
The calculated values for the dipole moment components
was taken from
(3) K. W. Sattelmeyer and J. F. Stanton,
2000, J. Am. Chem. Soc. 122, 8220.
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