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The spectrum was described in
(1) M. C. McCarthy, C. A. Gottlieb, and P. Thaddeus,
1995, J. Mol. Spectrosc. 173, 303.
The experimental lines were kindly provided by Dr. McCarthy.
Because some lines have residuals substantially larger than the
estimated uncertainties, the reduced standard deviation of the
fit is 2.5 (see also (1)).
With respect to the May 2000 entry, rest frequencies
for the N = 1 – 0 transition
from astronomical observations were used in the fit.
These were reported by
(2) N. Sakai, O. Saruwatari, T. Sakai, S. Takano,
and S. Yamamoto,
2010, Astron. Astrophys. 512, Art. No. 31.
In addition, γD was kept fixed
to the value of the main isotopolog, see e025501.cat.
Only data from (2) were merged. It is worthwhile
mentioning that the residuals of the remaining data
from (1), though in part much larger than the estimated
uncertainties, did not exceed 150 kHz.
The predictions are probably reliable up to 1.0 or
1.2 THz.
The dipole moment is assumed to the same as for the main
isotopomer, see e025501.cat.
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