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The first entry of Dec. 2009 was improved considerably.
The transition fequencies were summarized by
(1) H. S. P. Müller, A. Belloche, F. Lewen, and S. Schlemmer,
2026, ACS Earth Space Chem., accepted.
The line list includes new measurements employing a sample
highly enriched in CH313CN.
These are transitions with (partially) resolved 14N
hyperfine structure (HFS) splitting between 53 and 179 GHz
along with transitions without HFS spliiting between
160 and 927 GHz. Retained in the fit were data from
(2) H. S. P. Müller; B. J. Drouin, and J. C. Pearson,
2009, Astron. Astrophys. 506, 1487.
This work provides data between 249 and 1139 GHz
obtained from samples in natural isotopic composition.
The experimental line lists
with hyperfine splitting as well as
without hyperfine splitting can be accessed with source codes.
The purely K-dependent terms A and
DK were assumed to agree with
those of the main isotopolog, see e041505.cat.
The transition frequencies should be viewed with caution
if the calculated uncertainties exceed 0.1 MHz.
14N hyperfine splitting may be resolvable
at low values of J and possibly at the highest
K. Therefore, a calculation
with hyperfine splitting is provided up to
J' = 15 (268 GHz).
Please note that the partition function does include now the
spin-multiplicities of 14N !
The partition function values below refer to the ground
vibrational state only.
Vibrational correction factors have been derived
in the harmonic approximation.
At low temperatures, it may be necessary to discern between
A-13CH313CN and
E-13CH313CN.
The A state levels are described by
K = 3n, those of E state
by K = 3n ± 1.
The nuclear spin-weight ratio is 2 : 1 for
A-13CH313CN with
K > 0 and all other states, respectively.
The JK = 11
level is the lowest E state level.
It is 5.5713 cm–1 above ground.
The dipole moment was assumed to agree with
that of the main isotopolog, see e041505.cat.
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