|
The treatment of the Λ-doubling follows
(1) J. Xin and L. M. Ziurys,
1998, Astrophys. J. 495, L119;
the present parameters are very similar to the ones
reported there. The experimental transition frequencies
were published by
(2) B.-Z. Li and L. M. Ziurys,
1997, Astrophys. J. 488, L137.
23Na hyperfine splitting was not resolved;
it is probably negligible for observations of
late-type stars. Calculated transition frequencies
of the lower energy Π3/2 spin
component may be reliable throughout. Those in the
higher energy Π1/2 component should
be viewed with caution outside the range of the
experimental lines (260 to 385 GHz),
especially for the higher frequency f
component.
The dipole moment was taken from an ab initio
calculation by
(3) P. W. Fowler and A. J. Sadlej,
1991, Mol. Phys. 73, 43.
|