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New laboratory data were included with respect to
the third entry of Mar. 2015. These data were reported
by
(1) C. Baddeliyanage, J. Karner, S. P. Melath,
W. G. D. P. Silva, S. Schlemmer, and O. Asvany,
2025, J. Mol. Spectrosc. 407, Art. No. 111978.
These data constrain the C3H+ rest
frequencies very well. The initial data were retained for
consistency reasons. They are from astronomical
observations by
(2) J. Pety, P. Gratier, V. Guzmán, E. Roueff,
M. Gerin, J. R. Goicoechea, S. Bardeau, A. Sievers, F. Le
Petit, J. Le Bourlot, A. Belloche, and D. Talbi,
2012, Astron. Astrophys. 548, Art. No. A68.
The estimated uncertainties appear to be too optimistic.
All values have been increased essentially uniformly
by a factor of 1.7 to achieve an rms error of slightly
smaller than 1.0. With respect to the first entry of
Nov. 2012, additional laboratory data were included
which were reported by
(3) S. Brünken, L. Kluge, A. Stoffels,
O. Asvany, and S. Schlemmer,
2014, Astrophys. J. 783, Art. No. L4.
With respect to the second entry of Feb. 2014,
additional laboratory data were included
from
(4) M. C. McCarthy, K. N. Crabtree, M.-A. Martin-Drumel,
O. Martinez, Jr., B. A. McGuire, and C. A. Gottlieb,
2015, Astrophys. J. Suppl. Ser. 217, Art. No. 10;
as well as rest frequencies from astronomical observations
between 200 and 300 GHz from
(5) S. Cuadrado, J. R. Goicoechea, P. Pilleri, J. Cernicharo,
A. Fuente, and C. Joblin,
2015, Astron. Astrophys. 575, Art. No. A82.
The calculated transition frequencies are accurate enough at least
up to 400 GHz, possibly 450 GHz.
A dipole moment was reported in (2) from a quantum chemical calculation.
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