Description

The transition frequencies were taken from
(1) J. Casado, L. Nygaard, and G. O. Sørensen, 1971, J. Mol. Struct., 8, 211;
from
(2) E. Fliege, G. Bestmann, R.Schwarz, and H. Dreizler, 1981, Z. Naturforsch. A, 36, 1124;
from
(3) K. Vormann, U. Andresen, N. Heineking, and H. Dreizler, 1988, Z. Naturforsch. A, 43, 283;
from
(4) G. Wlodarczak, J. Burie, J. Demaison, K. Vormann, and A. G. Császár, 1989, J. Mol. Spectrosc., 134, 297;
and from
(5) K. Wohlfahrt, M. Schnell, J.-U. Grabow, and J. Küpper, 2008, J. Mol. Spectrosc., 247, 119.
Uncertainties were used as published, except for those in 4, which were reduced from 50 to 25kHz. Two lines from that work with large residuals were omitted. Uncertainties reported in (2), (3), and (5) are somewhat conservative.
Predictions with uncertainties exceeding 500kHz should be viewed with caution.
Benzonitrile has a very low vapor pressure. Therefore, we assume that the 14N hyperfine structure, which was resolved in the laboratory in (2), (3), and (5), is unlikely to be resolved in astronomical observations.
Spin-statistics have been considered in the calculation of the intensities. They are 5:3 for transitions with even and odd Ka, respectively.
The dipole moment was determined in (5).