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The entry was substantially modified from the first entry dated Sep. 2000.
Transition frequencies were reported by
(1) S. Yamamoto, S. Saito, M. Guélin, J. Cernicharo,
H. Suzuki, and M. Ohishi,
1987, Astrophys. J. 323, L149.
Additional transition frequencies with hyperfine splitting were
taken from
(2) A. L. Cooksy, C. A. Gottlieb, T. C. Killian, P. Thaddeus,
N. A. Patel, K. H. Young, and M. C. McCarthy,
2015, Astrophys. J. Suppl. Ser. 216, Art. No. 30.
Transition frequencies with calculated uncertainties exceeding
0.2 MHz should be viewed with caution.
The vibrational energy was taken from
(3) F. J. Mazzotti, R. Raghunandan, A. M. Esmail, M. Tulej,
and J. P. Maier,
2011, J. Chem. Phys. 134, Art. No. 164303.
The new dipole moment was assumed to be the same as in the
X 2Σ+ ground vibrational state,
see e049503.cat. This assumption may be reasonable.
The partition function of the main species takes into account all
states presently available in the CDMS. It is converged fairly well up
to about 150 K. Vibrational contributions to the
partition function are also available. These should be viewed
cautiously because of several estimates concerning vibrational
energies.
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