The first entry of Jan. 2003 was based on
(1) G. Klapper, L. Surin, F. Lewen, H. S. P. Müller, I. Pak, G. Winnewisser, 2003, Astrophys. J., 582, 262.
We retain J" = 4, 6, and 7 in the present evaluation.
The J" = 0 – 3 transitions frequencies with ¹⁷O hyperfine structure splitting were taken from
(2) G. Cazzoli, L. Dore, C. Puzzarini, and S. Beninati, 2002, Phys. Chem. Chem. Phys., 4, 3575.
The J" = 22 frequency was taken 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 transition frequencies should be quite reliable up to about 2.5 THz. Great caution is advised above 3.6 THz. Please note that the partition function still only refers to the ground vibrational state.
The ¹⁷O HFS splitting can be resolved in some astronomical observations. Therefore, a separate hyperfine calculation is provided for J" ≤ 4 below 562 GHz. NOTE: The partition function does take into account the spin multiplicity of the ¹⁷O nucleus !
The dipole moment and dipole centrifugal corrections are taken from
(4) D. Goorvitch, 1994, Astrophys. J. Suppl. 95, 535.