Nuclear moments and optical isotope shift of radioactive 133Ba

Hohle, Christoph; Hühnermann, H.; Meier, Th.; Ihle, H.R.; Wagner, R.

doi:10.1016/0370-2693(76)90664-x

Cited by 12 publications

(7 citation statements)

References 7 publications

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“…We measure the previously unknown 133 Ba + isotope shift of the 6 2 P 1/2 ↔ 5 2 D 3/2 transition and the hyperfine constant of the 5 2 D 3/2 state. Our measurements of the other spectroscopic features of 133 Ba + are in agreement with earlier measurements [23][24][25]. In addition, using the same techniques, we measure and report the isotope shifts of the 6 2 P 1/2 ↔ 5 2 D 3/2 transition in the rare 130 Ba + and 132 Ba + species.…”

supporting

confidence: 87%

“…3, summarizes spectroscopic data for barium atomic ions along with our measurements of δν r 130,138 , δν r 132,138 , and δν r 133,138 . Using previous spectroscopic data [24,31,33], the fitted slope of -0.26 is close to a theoretical calculation of the slope -0.288 [39]. The fitted slope, field and specific mass shifts of 988 MHz/fm 2 and 360 MHz respectively [33,40], and the new measurement of δν r 133,138 are combined to determine δ r 2 133,138 = −0.104 fm 2 .…”

supporting

confidence: 66%

“…The bolded values are spectroscopic measurements from this work and have a systematic uncertainty of ±20 MHz. All other isotope shifts are reported from references [24,25,[30][31][32][33]. Columns 3-8 are in MHz.…”

mentioning

confidence: 99%

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Spectroscopy of a Synthetic Trapped Ion Qubit

et al. 2017

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133 Ba + has been identified as an attractive ion for quantum information processing due to the unique combination of its spin-1/2 nucleus and visible wavelength electronic transitions. Using a microgram source of radioactive material, we trap and laser-cool the synthetic A = 133 radioisotope of barium II in a radio-frequency ion trap. Using the same, single trapped atom, we measure the isotope shifts and hyperfine structure of the 6 2 P 1/2 ↔ 6 2 S 1/2 and 6 2 P 1/2 ↔ 5 2 D 3/2 electronic transitions that are needed for laser cooling, state preparation, and state detection of the clockstate hyperfine and optical qubits. We also report the 6 2 P 1/2 ↔ 5 2 D 3/2 electronic transition isotope shift for the rare A = 130 and 132 barium nuclides, completing the spectroscopic characterization necessary for laser cooling all long-lived barium II isotopes.Since the demonstration of the first CNOT gate over 20 years ago [1], trapped ion quantum information processing (QIP), including quantum simulation, has developed considerably [2], recently demonstrating fullyprogrammable quantum processors [3,4]. To date, qubits have been demonstrated in trapped ion hosts of all nonradioactive, alkaline-earth-like elements [1,[5][6][7][8][9][10][11][12]. These ions possess a simple electronic structure that facilitates straightforward laser cooling as well as quantum state preparation, manipulation, and readout via electromagnetic fields.For the coherent manipulation of qubits, the phase of this applied electromagnetic field must remain stable with respect to the qubit phase evolution. Thus, atomic hyperfine structure is a natural choice for the definition of a qubit, as these extremely long-lived states can be manipulated with easily-generated, phase-coherent microwave radiation. In particular, qubits defined on the hyperfine structure of ions with half-integer nuclear spin possess a pair of states with no projection of the total angular momentum (F ) along the magnetic field (m F = 0). These so-called "clock-state" qubits are well-protected from magnetic field noise and can yield coherence times exceeding 10 minutes [13,14]. Further, for these species, F = 0 ground and excited states only occur when the nuclear spin I = 1/2. This is desirable because the F = 0 ↔ F = 0 selection rule can be leveraged to produce fast, robust qubit state preparation and readout that relies solely on frequency selectivity [10,12].Among the alkaline-earth-like elements, only three (Cd, Hg, Yb) have naturally occurring I = 1/2 isotopes. Mercury and cadmium ions require lasers in the deep ultraviolet portion of the electromagnetic spectrum, making it difficult to integrate them into a large-scale QIP architecture. Since 171 Yb + has the longest laser-cooling wavelength at 370 nm, it has been used in a wide variety of groundbreaking QIP experiments [4,[15][16][17][18][19]. However, even at this ultraviolet wavelength, the use of photonics infrastructure developed for visible and infrared light is limited. For example, significant fiber attenuation limits t...

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supporting

confidence: 87%

supporting

confidence: 66%

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Spectroscopy of a Synthetic Trapped Ion Qubit

et al. 2017

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“…More to the point, although we have had to make undesirable assumptions in order to make progress, the inclusion of lower level splittings means that our calculations are at least expected to be closer to reality than if we had neglected hyperfine splitting completely. A values were taken from Höhle, Hühnermann & Wagner (1982). No values were available for the 4619 Å transition.…”

Section: A1 Lanthanum: Pure Hyperfine Splittingmentioning

confidence: 99%

Neutron Capture Elements ins‐Process–Rich, Very Metal‐Poor Stars

Aoki

Ryan

Norris

et al. 2001

ApJ

149

166

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We report abundance estimates for neutron-capture elements, including lead (Pb), and nucleosynthesis models for their origin, in two carbon-rich, very metal-poor stars, LP 625-44 and LP 706-7. These stars are subgiants whose surface abundances are likely to have been strongly affected by mass transfer from companion AGB stars that have since evolved to white dwarfs. The detections of Pb, which forms the final abundance peak of the s-process, enable a comparison of the abundance patterns from Sr (Z = 38) to Pb (Z = 82) with predictions of AGB models. The derived chemical compositions provide strong constraints on the AGB stellar models, as well as on s-process nucleosynthesis at low metallicity. The present paper reports details of the abundance analysis for 16 neutron-capture elements in LP 625-44, including the effects of hyperfine splitting and isotope shifts of spectral lines for some elements. A Pb abundance is also derived for LP 706-7 by a re-analysis of a previously observed spectrum. We investigate the characteristics of the nucleosynthesis pathway that produces the abundance ratios of these objects using a parametric model of the s-process without adopting any specific stellar model. The neutron exposure τ is estimated to be about 0.7mb −1 , significantly larger than that which best fits solar-system material, but consistent with the values predicted by models of moderately metal-poor AGB stars. This value is strictly limited by the Pb abundance, in addition to those of Sr and Ba. We also find that the observed abundance pattern can be explained by a few recurrent neutron exposures, and that the overlap of the material that is processed in two subsequent exposures is small (the overlap factor r ∼ 0.1).

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“…Theoretical and experimental hyperfine A and B values from the 5d 6s b 1 D 2 level of 139 La + have been reported from calculations [14] and collinear laser spectroscopic methods [9,15]. A typical FIBLAS hyperfine spectrum is shown in figure 5.…”

Section: Measurementmentioning

confidence: 99%