The molecular beam electric resonance technique has been used to examine the hyperfine spectrum of CsF to determine the nuclear quadrupole interaction of the cesium nucleus. A total of 95 transitions in vibrational states vϭ0Ϫ5 and rotational states Jϭ1Ϫ8 have been included in a fit to determine the cesium nuclear quadrupole and spin-rotation interactions, the fluorine spin-rotation interaction, and the tensor and scalar parts of the spin-spin interaction. Vibration and rotation dependencies of these constants have been determined, allowing correction for zero point vibration effects. This experimental Cs nuclear quadrupole coupling constant when combined with the electric field gradient calculated using a relativistic coupled cluster method yields a nuclear quadrupole moment of the Cs nucleus equal to eQϭϪ3.43098 mbarn. The vibrational dependence of the coupling constant is smaller than the theoretical estimate. The coupling constants we have determined are the following: eQ Cs q Cs ϭ1245.598(10)Ϫ14.322(25)(vϩ1/2)ϩ0.080(14) ϫ(vϩ1/2) 2 ϩ0.0040(22)(vϩ1/2) 3 Ϫ0.00209(59)J(Jϩ1)ϩ0.00048(40)(vϩ1/2)J(Jϩ1), c Cs ϭ0.66177(14)Ϫ0.01509(28)(vϩ1/2)ϩ0.000550(94)(vϩ1/2) 2 , c F ϭ15.08163(84)Ϫ0.1744(14) ϫ(vϩ1/2)ϩ0.00234(41)(vϩ1/2) 2 Ϫ0.000093(13)J(Jϩ1), c 3 ϭ0.92713(53)Ϫ0.00917(93)(v ϩ1/2)ϩ0.00097(29)(vϩ1/2) 2 , c 4 ϭ0.62745(30)Ϫ0.00903(22)(vϩ1/2). All values are in kHz units, with one standard deviation uncertainty estimates in the last two digits shown in ().
A high-precision examination of the hyperfine spectrum of 6LiI in comparison with 7LiI shows a shift in the iodine nuclear electric quadrupole moment that cannot be accounted for by a model in which the electric field gradient at the iodine site is assumed to depend only upon the internuclear distance between Li and I. The other hyperfine interactions are consistent between the two isotopomers, including the previously reported electric hexadecapole interaction of the iodine nucleus.
This work presents 97 remeasured Fe V wavelengths (1200Å to 1600Å) and 123 remeasured Ni V wavelengths (1200Å to 1400Å) with uncertainties of approximately 2 mÅ. An additional 67 remeasured Fe V wavelengths and 72 remeasured Ni V wavelengths with uncertainties greater than 2 mÅ are also reported. A systematic calibration error is also identified in the previous Ni V wavelengths and is corrected in this work. Furthermore, a new energy level optimization of Ni V is presented that includes level values as well as Ritz wavelengths. This work improves upon the available data used for observations of quadruply ionized nickel (Ni V) in white dwarf stars. This compilation is specifically targeted towards observations of the G191-B2B white dwarf spectrum that has been used to test for variations in the fine structure constant, α, in the presence of strong gravitational fields (Berengut et al. 2013). The laboratory wavelengths for these ions were thought to be the cause of inconsistent conclusions regarding the variation limit of α as observed through the white dwarf spectrum. These inconsistencies can now be addressed with the improved laboratory data presented here.
An extensive analysis of the Mn spectrum was carried out using high-resolution Fourier transform (FT) and grating spectroscopy of Mn–Ne and Mn–Ar hollow cathode discharge sources, over the range 82–5500 nm (1820–121,728 cm−1). Spectral wavelengths for a total of 6019 Mn ii lines have been measured, of which 1345 are obtained through FT spectroscopy. These wavelengths are given to at least an order of magnitude lower uncertainty than previous measurements. These lines were used to identify 6256 Mn ii transitions and improve the values of 505 previously published energy levels with typical uncertainties of a few thousandths of a cm−1, representing an order-of-magnitude reduction in uncertainty. We have verified and improved an additional 57 Mn ii energy levels, previously established through observation of stellar spectra alone, using our FT spectra. In addition, 52 new energy level values have been established. The number of classified lines reported is approximately 50% more than previously published. The new accurate data for 614 energy levels and 6019 lines will allow a more reliable analysis of Mn ii spectral lines in astrophysical spectra.
We summarize measurements of improved wavelengths of Fe V and Ni V in the vacuum ultraviolet.
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