Laser spectroscopy and cooling of Yb{}^{+} ions on a deep-UV transition

Laser spectroscopy and cooling of Yb ions on a deep-UV transition

Hendrik M. Meyer    Matthias Steiner    Lothar Ratschbacher    Christoph Zipkes    Michael Köhl Cavendish Laboratory, University of Cambridge, JJ Thomson Avenue, Cambridge CB30HE, United Kingdom
August 6, 2019
Abstract

We perform laser spectroscopy of Yb ions on the 4f6s S - 4f5d6s D transition at 297 nm. The frequency measurements for Yb, Yb, Yb, and Yb reveal the specific mass shift as well as the field shifts. In addition, we demonstrate laser cooling of Yb ions using this transition and show that light at 297 nm can be used as the second step in the photoionization of neutral Yb atoms.

pacs:
32.30.-r, 37.10.Ty, 37.10.Rs

I Introduction

In the last decade trapped Yb+ ions have been a workhorse in the fields of quantum information processing Moehring et al. (2007); Kim et al. (2010); Timoney et al. (2011), precision measurements Schneider et al. (2005); Roberts et al. (2000) and hybrid systems Zipkes et al. (2010). Yb has a rich energy level structure because besides pure valence-electron excitations, also electrons from a closed f-shell can be excited. This leads to unusual features such as the electric octupole transition S-F, which is currently explored for the prospect of an ion based atomic clock, as it has a natural lifetime of several years Roberts et al. (2000, 1997).

Since the work of Bell et al. (1991), a common feature of most trapped Yb+ experiments is the continuous excitation of the ion within a four level system (Figure 1). The ion is cooled and detected on the S-P transition near 369 nm. A second decay channel to the metastable D state necessitates a second laser to avoid interruptions of the fluorescence. Light near 935 nm repopulates the ground state via the D state.

In this paper, we extend the available laser manipulation toolbox for trapped Yb+ ions by exciting the 4f6s S - 4f5d6s D transition at 297 nm. We perform laser spectroscopy and present frequency measurements for four isotopes. The isotope shifts contain information about the change of the charge distribution within the nucleus and about the correlations of electrons, which are intricate because of a partially filled f-shell in Yb+. Therefore they can be used to test ab-initio calculations. In addition, we show that the 297 nm light can be used as second the step in the photoionization process of neutral Yb as well as for laser cooling of single Yb+ ions. The relatively narrow line width could potentially allow to reach lower laser cooling temperatures.

Figure 1: (color online) Relevant energy levels and transitions of Yb (branching ratios given in percentages). , and branching ratio out of the P state are taken from Ref. Olmschenk et al. (2007), from Ref. Berends et al. (1993) and the D branching ratio from Ref. Bièmont et al. (1998).

Ii Experimental Setup

We trap single Yb+ ions in a RF Paul trap, which consists of two opposing endcap electrodes Schrama et al. (1993) separated by 150 m. The electrodes are formed from tungsten wire of 250 m diameter and are etched to a needle-like geometry Deslauriers et al. (2006). By applying a radio frequency signal of 20 MHz and a few hundred Volts amplitude, the ion is trapped with secular trap frequencies of  MHz and  MHz. Single ions are loaded into the trap by two-step photoionization from a thermal atomic beam Balzer et al. (2006). A stainless steel tube filled with Yb is resistively heated by a short current pulse (typically 60-80 ms, 60 A) and emits neutral Yb atoms into the trap. The atoms are resonantly excited on the S-P transition with laser light at 398 nm and subsequently ionized by a laser at 369 nm. The first excitation step is isotope selective. After ionization, the ion is continuously laser cooled on the S-P transition and the resulting fluorescence is collected by an in-vacuum objective and detected by a photomultiplier tube.

The laser system for exciting the S-D transition at 297 nm is based on sum frequency generation (SFG) of light at 532 nm and 672 nm. The sketch of the optical setup is shown in Figure 2. The green 532 nm laser is a commercial system (Coherent Verdi V6), whereas the red 672 nm diode laser with subsequent amplification stage is homebuilt. In order to supply an atomic frequency reference, the green laser is stabilized to the R(56)32-0 transition in molecular Iodine Jungner et al. (1995). As the study of isotope shifts in Yb+ requires a large frequency scan range, we use the Doppler broadened absorption line (at room temperature: line width  GHz) and generate an error signal by FM spectroscopy Bjorklund et al. (1983). We measured the rms frequency fluctuations of the green laser to be about 20 MHz.

We achieve type-I (ooe) SFG in a doubly resonant bow-tie cavity (finesse: 75, free spectral range:  GHz). The cavity length is locked to the 532 nm laser using the Hänsch-Couillaud stabilization technique Hänsch and Couillaud (1980), whereas the 672 nm laser follows the SFG cavity by the Pound-Drever-Hall locking technique Drever et al. (1983). By sweeping the green 532 nm laser we can scan the generated UV light continuously about 1 GHz. Input light intensities of 1 W (532 nm) and 300 mW (672 nm) yield about 10 mW of 297 nm light.

Figure 2: (color online) Laser system to generate 297 nm light. Abbreviations: EOM: Electro-optic modulator, FP: Fast piezo-transducer, LP: Low pass, Mod: Laser current modulation, PBS: Polarizing beam splitter, PD: Photodiode, PID: Feedback controller, SFG: Sum frequency generation, SP: Slow piezo-transducer, TA: Tapered Amplifier

Iii Isotope Shifts

Spectroscopy on the S-D transition is performed in a double-resonance scheme. The laser at 369 nm cools the ion continuously on the S-P transition and yields fluorescence, which is detected. Simultaneously, the 297 nm probe laser excites the S-D transition. Additional 935 nm light is necessary to deplete the population of the D state. By sweeping the frequency of the 297 nm light, the S-D resonance is observed as a drop in the 369 nm fluorescence (Figure 3).

The ratio of the saturation parameters, and (, with the (saturation) intensity ()) is important for the strength of the observed signal. For the excitation into the D is much slower than the probing of the S state due to the 369 nm laser, which effectively suppresses the transition to D in a quantum zeno like manner. In contrast, the signal of the 369 nm S-P fluorescence shows a significant drop for similar saturation parameters . The steady state fluorescence is proportional to the population of the P state, which is given by

(1)

assuming fast repumping out of the D state and neglecting coherences. Here is the detuning of the 369 nm laser and the natural line width of the P state. The term describes the coupling to the D state

(2)

where is the detuning of the 297 nm laser and the natural line width of the D state. For typical experimental parameters of and , this results in a 20-30% drop of the fluorescence, which is consistent with our measured spectra. We typically scan the 297 nm light 400 MHz in 10 s and record the 369 nm fluorescence. The line width of the 297 nm laser, residual micromotion and the continuous driving of the S-P transition broaden the linewidth, which is measured to be 40 MHz. The absolute frequency is determined by measuring the frequency of the 532 nm and the 672 nm laser with a wave meter (HighFinesse WS/07). The wave meter is calibrated to the D (F, F’) crossover line in Rb and has a specified 3- accuracy of 60 MHz. In this manner we measured the S-D frequencies for the isotopes Yb, Yb, Yb+ and Yb+ (Table 1).

Isotope Frequency (THz)
170Yb 1008.91619(3)
172Yb 1008.91759(3)
174Yb 1008.91855(3)
176Yb 1008.91958(3)
Table 1: Measured frequencies of the S-D transition in Yb (1- error).
Figure 3: (color online) Double-resonance spectrum of the S-D transition in Yb+. Yellow line: Gauss fit. Transition frequencies have been determined by averaging 10 spectra.

The isotope shift of a spectral line consists of two contributions, the field and the mass shift King (1984). The field shift (FS) is caused by the change of the charge distribution within the nucleus and is very sensitive to the electron charge density at the nucleus . The mass shift itself has two contributions: The change in the reduced mass is taken into account by the normal mass shift (NMS) whereas the specific mass shift (SMS) describes the change in the correlations between electrons. In total, the isotope shift of a spectral line between isotopes a and b reads

(3)

with and () being the isotope masses and the mass of the electron. The parameter depends only on the transition frequency of the lighter isotope and is given by . A common technique to identify the field shift and the specific mass shift from measured isotope shifts is via a King plot King (1984). After eliminating the normal mass shift from the measured isotope shift, the residual shift is multiplied by and the reduced mass of a reference pair (we choose Yb,Yb) to obtain the modified isotope shift :

(4)

The modified isotope shift is plotted against that of another transition and the slope of the resulting linear fit relates the field shifts:

(5)

We use the data from Clark et al. (1979) on the 555.6 nm S-P transition in neutral Yb as the reference for the King plot. These data are very precise and allow to calculate the field shift Zinkstok et al. (2002). For the King plot and the determination of the transition characteristic parameter, and , Yb was chosen as reference isotope. From Figure 4 we extract the slope and calculate and (Table 2).

4.16 (66) GHz
2.92 (47) GHz
1.65 (26) GHz
-4.5 (4.0) GHz amu
Table 2: Experimentally determined contributions to the isotope shift.
Figure 4: (color online) King plot of our data vs the data of Clark et al. (1979). The slope of the linear fit is used to determine the field shift.

Our results can be interpreted in comparison with the data of Zinkstok et al. Zinkstok et al. (2002), who investigated a similar line in neutral Yb, namely the 4f6s S to 4f5d6s P transition. They found a similarly large negative specific mass shift, which is explained by the strong coupling of d- and f-electrons King (1984). In contrast, our measured field shift is about 50% higher. This may reflect the fact that, in general the electron charge density at the nucleus is higher in ionic systems than in their neutral counterparts and thereby more sensitive to changes of the charge distribution within the nucleus.

Iv Photoionization and laser cooling

Photoionization of Yb can be achieved by a photon at 398 nm (S-P transition) and a second photon with a wavelength smaller than 394 nm. Here we demonstrate that light at 297 nm can be used for the second step. At the beginning of the loading sequence the Yb oven is heated for 75 ms and simultaneously the 398 nm, the 297 nm and the 935 nm laser lights are switched on. After three seconds the light at 398 nm is turned off and one second later the 369 nm laser illuminates the ion and the resulting fluorescence is recorded (Figure 5). We note that for reliable loading the oven heating time needs to be slightly longer compared to the standard loading with 369 nm light.

Figure 5: (color online) Recorded 369 nm fluorescence while loading a single Yb+ with 297 nm light. Inset: Zoom into the onset of the fluorescence (each curve is the average of 10 loadings). Yellow curve: Large detuning,  MHz. Blue line: Expected fluorescence of an 100 K hot ion Wesenberg et al. (2007). Black curve: Sweep of from -200 MHz to -60 MHz in 3 s after heating the oven leads to a high initial level of 369 nm fluorescence indicating a cold ion. In both cases .

The fluorescence curve after switching on the 369 nm light depends strongly on the kinetic energy of the ion due to the Doppler shift and can be used to determine its temperature Wesenberg et al. (2007); Epstein et al. (2007). In order to measure the onset of the fluorescence, we interrupt the 935 nm light 10 ms before the 369 nm light is switched on. This allows the 369 nm intensity controller to adjust without affecting the ion. We switch the 935 nm light back on 100 ms later. Only with both lights, 935 nm and 369 nm, the excitation cycle is closed and the ion continuously scatters photons. The inset in Figure 5 shows the onset of the fluorescence for two different loading sequences. In the first the 297 nm laser is set 400 MHz below the resonance frequency during the loading (yellow curve). Because of the large detuning the ion scatters only few photons on the S-D transition and the cooling of the ion is very inefficient. Thus, the 369 nm fluorescence starts low due to Doppler broadening and increases as the 369 nm laser cools the ion. In the second loading sequence, a smooth shifting of the 297 nm laser frequency towards the resonance (from  MHz to  MHz) in the first three seconds after photoionization yields a photon scatter rate, which starts immediately at its saturation value and hence indicates a cold ion (black curve).

V Conclusion

In conclusion, we have demonstrated laser spectroscopy, photoionization and laser cooling of a single Yb ion on the 4f6s S - 4f5d6s D transition. We measure the isotope shifts and determine the specific mass shift as well as the field shifts. The results on loading-and-cooling show that this transition complements the existing manipulation capabilities of Yb ions and potentially could replace the S-P transition. In the future, we plan to make use of the relatively narrow line width of this transition to facilitate Doppler cooling to very low temperatures, potentially directly into the vibrational ground state. Moreover, the new availability of a -system in Yb will allow for new ways of quantum state manipulation and, for example, EIT cooling Morigi et al. (2000); Roos et al. (2000).

Vi Acknowledgments

We would like to thank Sebastien Garcia, Neil McDonald, Ben Metcalf, Christopher Overstreet and the workshop of the Cavendish Laboratory. This work has been supported by EPSRC (EP/H005679/1) and ERC (Grant No. 240335).

References

  • Moehring et al. (2007) D. L. Moehring, P. Maunz, S. Olmschenk, K. C. Younge, D. N. Matsukevich, L.-M. Duan,  and C. Monroe, Nature 449, 68 (2007).
  • Kim et al. (2010) K. Kim, M.-S. Chang, S. Korenblit, R. Islam, E. E. Edwards, J. K. Freericks, G.-D. Lin, L.-M. Duan,  and C. Monroe,  Nature 465, 590 (2010).
  • Timoney et al. (2011) N. Timoney, I. Baumgart, M. Johanning, A. F. Varon, M. B. Plenio, A. Retzker,  and C. Wunderlich, Nature 476, 185 (2011).
  • Schneider et al. (2005) T. Schneider, E. Peik,  and C. Tamm,  Phys. Rev. Lett. 94, 230801 (2005).
  • Roberts et al. (2000) M. Roberts, P. Taylor, G. P. Barwood, W. R. C. Rowley,  and P. Gill,  Phys. Rev. A 62, 020501 (2000).
  • Zipkes et al. (2010) C. Zipkes, S. Palzer, C. Sias,  and M. Köhl,  Nature 464, 388 (2010).
  • Roberts et al. (1997) M. Roberts, P. Taylor, G. P. Barwood, P. Gill, H. A. Klein,  and W. R. C. Rowley,  Phys. Rev. Lett. 78, 1876 (1997).
  • Bell et al. (1991) A. S. Bell, P. Gill, H. A. Klein, A. P. Levick, C. Tamm,  and D. Schnier,  Phys. Rev. A 44, R20 (1991).
  • Olmschenk et al. (2007) S. Olmschenk, K. C. Younge, D. L. Moehring, D. N. Matsukevich, P. Maunz,  and C. Monroe,  Phys. Rev. A 76, 052314 (2007).
  • Berends et al. (1993) R. W. Berends, E. H. Pinnington, B. Guo,  and Q. Ji,  Journal of Physics B: Atomic, Molecular and Optical Physics 26, L701 (1993).
  • Bièmont et al. (1998) E. Bièmont, J.-F. Dutrieux, I. Martin,  and P. Quinet,  Journal of Physics B: Atomic, Molecular and Optical Physics 31, 3321 (1998).
  • Schrama et al. (1993) C. Schrama, E. Peik, W. Smith,  and H. Walther,  Optics Communications 101, 32 (1993).
  • Deslauriers et al. (2006) L. Deslauriers, S. Olmschenk, D. Stick, W. K. Hensinger, J. Sterk,  and C. Monroe,  Phys. Rev. Lett. 97, 103007 (2006).
  • Balzer et al. (2006) C. Balzer, A. Braun, T. Hannemann, C. Paape, M. Ettler, W. Neuhauser,  and C. Wunderlich, Phys. Rev. A 73, 041407 (2006).
  • Jungner et al. (1995) P. Jungner, S. Swartz, M. Eickhoff, J. Ye, J. Hall,  and S. Waltman, IEEE Transactions on Instrumentation and Measurement 44, 151 (1995).
  • Bjorklund et al. (1983) G. C. Bjorklund, M. D. Levenson, W. Lenth,  and C. Ortiz, Applied Physics B: Lasers and Optics 32, 145 (1983).
  • Hänsch and Couillaud (1980) T. Hänsch and B. Couillaud, Optics Communications 35, 441 (1980).
  • Drever et al. (1983) R. W. P. Drever, J. L. Hall, F. V. Kowalski, J. Hough, G. M. Ford, A. J. Munley,  and H. Ward,  Applied Physics B: Lasers and Optics 31, 97 (1983).
  • King (1984) W. H. King,  Isotope Shifts in Atomic Spectra (Plenum Press, 1984).
  • Clark et al. (1979) D. L. Clark, M. E. Cage, D. A. Lewis,  and G. W. Greenlees, Phys. Rev. A 20, 239 (1979).
  • Zinkstok et al. (2002) R. Zinkstok, E. J. van Duijn, S. Witte,  and W. Hogervorst,  Journal of Physics B: Atomic, Molecular and Optical Physics 35, 2693 (2002).
  • Wesenberg et al. (2007) J. H. Wesenberg, R. J. Epstein, D. Leibfried, R. B. Blakestad, J. Britton, J. P. Home, W. M. Itano, J. D. Jost, E. Knill, C. Langer, R. Ozeri, S. Seidelin,  and D. J. Wineland,  Phys. Rev. A 76, 053416 (2007).
  • Epstein et al. (2007) R. J. Epstein, S. Seidelin, D. Leibfried, J. H. Wesenberg, J. J. Bollinger, J. M. Amini, R. B. Blakestad, J. Britton, J. P. Home, W. M. Itano, J. D. Jost, E. Knill, C. Langer, R. Ozeri, N. Shiga,  and D. J. Wineland, Phys. Rev. A 76, 033411 (2007).
  • Morigi et al. (2000) G. Morigi, J. Eschner,  and C. H. Keitel, Phys. Rev. Lett. 85, 4458 (2000).
  • Roos et al. (2000) C. F. Roos, D. Leibfried, A. Mundt, F. Schmidt-Kaler, J. Eschner,  and R. Blatt, Phys. Rev. Lett. 85, 5547 (2000).
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