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The initial experimental measurements were taken from
(1) G. Klapper, L. Surin, F. Lewen, H. S. P. Müller, I. Pak, G. Winnewisser,
2003, Astrophys. J., 582, 262;
covering J" = 0 – 2 and 7 and 8. Transitions up
to J" = 2 display resolved 17O hyperfine
structure (HFS) splitting.
With respect to the first entry from Jan. 2003,
more accurate low-J data (up to 4 – 3 near 429 GHz)
were included which come from
(2) C. Puzzarini, L. Dore, and G. Cazzoli,
2003, J. Mol. Spectrosc., 217, 19;
adding to and replacing the corresponding data from (1).
In addition, the J" = 23 frequency was added from
(3) J. C. Pearson, B. J. Drouin, A. Maestrini, I. Mehdi, J. Ward,
R. H. Lin, S. Yu, J. J. Gill, B. Thomas, C. Lee, G. Chattopadhyay,
E. Schlecht, F. W. Maiwald, P. F. Goldsmith, and P. Siegel,
2011, Rev. Sci. Instrum., 82, Art. No. 093105;
the J" = 24 frequency was omitted because of a large residual.
The transition frequencies should be quite reliable up to
about 3 THz. Please note that the partition function
still only refers to the ground vibrational state.
The HFS splitting caused by the 17O nucleus
may be resolved in quiescent sources for low values
of J. Therefore, a separate
hyperfine calculation is provided for J" up to 3
with 17O and 13C splitting;
the latter probably more for completeness reasons.
NOTE: The partition function
does take into account the spin multiplicities of the
17O (6) and 13C (2) nucleus !
The dipole moment and dipole centrifugal corrections are taken from
(2) D. Goorvitch,
1994, Astrophys. J. Suppl. 95, 535.
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