SH, v = 1
Sulfanyl, X 2Πi, v = 1
Species tag 033509
Version1*
Date of EntryMar. 2015
ContributorH. S. P. Müller

Several sets of rotational, rovibrational, and electronic data were fit simultaneously. These include the v = 0 ground state rotational transitions along with extensive higher frequency v = 0 and 1 terahertz and FIR data from
(1) M. A. Martin-Drumel, S. Eliet, O. Pirali, M. Guinet, F. Hindle, G. Mouret, and A. Cuisset, 2012, Chem. Phys. Lett. 550, 8.
Also included are rotational data from
(2) E. Klisch, T. Klaus, S. P. Belov, A. Dolgner, R. Schieder, G. Winnewisser, and E. Herbst, 1996, Astrophys. J. 473, 1118;
as well as radiofrequency data from
(3) W. L. Meerts and A. Dymanus, 1974, Astrophys. J. 187, L45.
Terahertz data from
(4) B. J. Drouin, J. C. Pearson, S. Yu, and H. Gupta, 2013, IEEE Trans. Terahertz Sci. Technol. 3, 314;
were omitted from the fit because a considerable fraction of the data is not compatible with the remaining data within uncertainties. Additional v = 0 FIR rotational data from
(5) I. Morino and K. Kawaguchi, 1995, J. Mol. Spectrosc. 170, 172;
were superseded by the more extensive and more accurate data from (1).
Also included in the fit were rovibrational data from
(6) P. F. Bernath, T. Amano, and M. Wong, 1983, J. Mol. Spectrosc. 98, 20;
from
(7) R. J. Winkel, Jr., and S. P. Davis, 1984, Can. J. Mol. Phys. 62, 1420;
and from
(8) R. S. Ram, P. F. Bernath, R. Engleman, Jr., and J. W. Brault, 1995, J. Mol. Spectrosc. 172, 34.
P. F. Bernath is thanked for an output file of his fit in (8) which was used as orientation of uncertainties of (6-8).
In addition, v = 0 – 0 rovibronic data were employed in the fit which were taken from
(9) D. A. Ramsay, 1952, J. Chem. Phys. 20, 1920.
No experimental transitions frequencies were merged.
The transitions may be observable toward late-type stars. Predictions of transitions within each spin-substate should be reliable throughout mainly because of the extensive data from (1) and (7). Transitions between the spin-substates as well as the hyperfine splitting should be viewed with some caution.
Hund's case (b) quantum numbers were employed, as usual. Levels with J + 0.5 = N correlate with 2Π1/2 and levels with J – 0.5 = N correlate with 2Π3/2.
The dipole moment was derived from the ground state values of SH from (3) and that of SD from
(10) W. L. Meerts and A. Dymanus, 1975, Can. J. Phys. 53, 2123.
Rotational corrections to the dipole moment may matter at higher rotational quantum numbers.

Lines Listed545
Frequency / GHz< 22047
Max. J21
log STR0-15.0
log STR1-15.0
Isotope Corr.-0.022
Egy / (cm–1)2598.03
 µa / D0.764
 µb / D 
 µc / D 
 A / MHz 
 B / MHz275268.4
 C / MHz 
 Q(2000.)1272.5449
 Q(1000.)495.0662
 Q(500.0)209.7702
 Q(300.0)113.4351
 Q(225.0)81.9762
 Q(150.0)54.3914
 Q(75.00)30.9152
 Q(37.50)20.5682
 Q(18.75)16.7001
 Q(9.375)16.0151
 Q(5.000)15.9904
 Q(2.725)15.9823
detected in ISM/CSMno


Database maintained by Holger S. P. Müller and Sven Thorwirth, programming by D. Roth and F. Schloeder