|
The observed lines are from
(1) M. C. McCarthy, G. W. Fuchs, J. Kucera,
G. Winnewisser, and P. Thaddeus,
2003, J. Chem. Phys. 118, 3549.
Additional spectroscopic parameters were estimated
from values of C2N from
(2) M. D. Allen, K. M. Evenson, D. A. Gillett,
and J. M. Brown,
2000, J. Mol. Spectrosc. 201, 18.
The spin-orbit coupling parameter A was
estimated from photoelectron spectroscopy of
C2nN– by
(3) E. Garand, T. I. Yacovitch, and D. M. Neumark,
2009, J. Chem. Phys. 130, 064304.
The fit has been carried out employing Hund's case (b).
Predictions for the lower spin-substate
2Π1/2, should be viewed with
increasing caution above 100 GHz, while those of
the upper spin-substate 2Π3/2
should be viewed with great caution throughout.
14N hyperfine structure was omitted in
the mai entry. It was resolved in (1) and is
probably resolvable in astronomical observations
at 7 mm or longer wavelengths. Predictions with
hyperfine splitting up to N" = 20.
The 14N spin-multiplicity was considered in
all calculations of the partition function.
The dipole moment is from an ab initio calculation
by
(4) J. Fiser and R. Polák,
2013, Chem. Phys. 425 126.
The calculated dipole moments differ considerably
depending on the method and the basis set, therefore,
this value should be viewed with caution.
|