Abstract
We implement imaging spectroscopy of the optical clock transition of lattice-trapped degenerate fermionic Sr in the Mott-insulating regime, combining micron spatial resolution with submillihertz spectral precision. We use these tools to demonstrate atomic coherence for up to 15 s on the clock transition and reach a record frequency precision of 2.5×10-19. We perform the most rapid evaluation of trapping light shifts and record a 150 mHz linewidth, the narrowest Rabi line shape observed on a coherent optical transition. The important emerging capability of combining high-resolution imaging and spectroscopy will improve the clock precision, and provide a path towards measuring many-body interactions and testing fundamental physics.
| Original language | English |
|---|---|
| Article number | 103201 |
| Journal | Physical Review Letters |
| Volume | 120 |
| Issue number | 10 |
| DOIs | |
| Publication status | Published - 2018 Mar 5 |
| Externally published | Yes |
ASJC Scopus subject areas
- Physics and Astronomy(all)
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Imaging Optical Frequencies with 100 μhz Precision and 1.1 μ m Resolution. / Marti, G. Edward; Hutson, Ross B.; Goban, Akihisa; Campbell, Sara L.; Poli, Nicola; Ye, Jun.
In: Physical Review Letters, Vol. 120, No. 10, 103201, 05.03.2018.Research output: Contribution to journal › Article › peer-review
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TY - JOUR
T1 - Imaging Optical Frequencies with 100 μhz Precision and 1.1 μ m Resolution
AU - Marti, G. Edward
AU - Hutson, Ross B.
AU - Goban, Akihisa
AU - Campbell, Sara L.
AU - Poli, Nicola
AU - Ye, Jun
N1 - Funding Information: 100 μ Hz Precision and 1.1 μ m Resolution Marti G. Edward 1,2 ,* Hutson Ross B. 1,2 Goban Akihisa 1,2 Campbell Sara L. 1,2 Poli Nicola 3,4 Ye Jun 1,2 JILA, 1 National Institute of Standards and Technology and University of Colorado , 440 UCB, Boulder, Colorado 80309, USA Department of Physics, 2 University of Colorado , 390 UCB, Boulder, Colorado 80309, USA 3 Dipartimento di Fisica e Astronomia and LENS—Università di Firenze , INFN—Sezione di Firenze, Via Sansone 1, 50019 Sesto Fiorentino, Italy Istituto Nazionale di Ottica, 4 Consiglio Nazionale delle Ricerche (INO-CNR) , Largo Enrico Fermi, 6, 50125 Firenze, Italy * edward.marti@jila.colorado.edu 5 March 2018 9 March 2018 120 10 103201 22 November 2017 © 2018 American Physical Society 2018 us American Physical Society We implement imaging spectroscopy of the optical clock transition of lattice-trapped degenerate fermionic Sr in the Mott-insulating regime, combining micron spatial resolution with submillihertz spectral precision. We use these tools to demonstrate atomic coherence for up to 15 s on the clock transition and reach a record frequency precision of 2.5 × 10 - 19 . We perform the most rapid evaluation of trapping light shifts and record a 150 mHz linewidth, the narrowest Rabi line shape observed on a coherent optical transition. The important emerging capability of combining high-resolution imaging and spectroscopy will improve the clock precision, and provide a path towards measuring many-body interactions and testing fundamental physics. National Institute of Standards and Technology 10.13039/100000161 Defense Advanced Research Projects Agency 10.13039/100000185 Air Force Office of Scientific Research 10.13039/100000181 National Science Foundation 10.13039/100000001 PHY-1734006 marker VIEWPOINT marker L_SUGG Alkaline-earth (AE) atoms possess ultranarrow optical (“clock”) transitions that realize the best atomic clocks [1–5] . AE atoms become sensitive probes of their external environment, of interactions, and of fundamental physics through highly precise measurements of the optical clock frequency. Recently, frequency shifts that arise from atomic interactions in ultracold samples have been used to study magnetism and spin-orbit coupling in nondegenerate ensembles of AE atoms [6–8] , as well as spin-exchange processes, Feshbach resonances, and synthetic dimensions in degenerate samples [9–12] . Combining in situ imaging with state-of-the-art optical spectroscopy provides a new route to improve the precision of atomic clocks, study both few- and many-body phenomena, and test fundamental physics. Imaging the relative clock frequency between atoms in different regions of the optical lattice, called imaging spectroscopy, allows for synchronous frequency comparisons that improve precision by rejecting laser frequency noise and common-mode clock shifts. In particular, frequency differences can be measured at the quantum-projection-noise (QPN) limit by comparing the Ramsey spectroscopy excitation fraction of one atomic ensemble against another, even when the free-evolution time exceeds the laser coherence time. In addition to determining single-particle effects such as lattice light shifts that impact optical clock accuracy, maps of the local frequencies can elucidate few-body physics of atoms interacting within a lattice site, and many-body interactions between lattice sites. Thus, imaging spectroscopy gives information analogous to scanning tunneling microscopy, and will enable the exploration of long-range electric dipole-dipole interactions [13,14] and new phenomena, such as the Kondo effect [15,16] , SU( N ) quantum magnetism [17–19] , and unconventional superconductivity [20–22] . Since synchronous comparisons improve precision and hence allow for more rapid measurements than conventional techniques, they bring new tests of gravitational and other fundamental physics within the range of tabletop experiments. At 10 - 19 fractional frequency precision, gravitational redshifts can be measured within a single vacuum chamber, opening the door to exploring the interplay of quantum mechanics and general relativity [23,24] . In this Letter, we perform imaging spectroscopy on a two-state spin mixture of Fermi-degenerate Sr 87 prepared in the Mott-insulating regime of a three-dimensional (3D) optical lattice with submillihertz-precision optical spectroscopy and micron-resolution spatial imaging. This work builds on the long coherence time demonstrated in Ref. [5] and leverages high-resolution imaging for the interrogation of strontium atoms in a 3D optical lattice clock. First, we characterize the resolution of the imaging system. We then demonstrate a QPN-limited frequency difference measurement between two regions of the lattice. Using thousands of atoms that remain coherent for up to 15 s, we reach a record in frequency precision of 2.5 × 10 - 19 , or 100 μ Hz on an optical frequency. This excellent precision allows us to measure the shift of the clock transition by the optical lattice with a spatially dependent frequency map. Imaging spectroscopy provides a clear path towards reducing the uncertainty of the optical lattice light shift by more than an order of magnitude. Finally, we use imaging spectroscopy as a multiplexed measurement of the frequency noise of an ultrastable laser. This is accomplished with a magnetic field gradient such that different regions of the lattice simultaneously probe different components of the laser frequency. The lattice then acts as a highly multiplexed optical spectrum analyzer. Similarly, the lattice can be employed as a multiaxis sensor of electromagnetic, gravitational, or other field gradients. Atomic preparation follows Ref. [5] . In summary, nearly 1 0 7 Sr 87 atoms are laser-cooled to 3 μ K in a crossed optical dipole trap. Atoms are optically pumped to an incoherent mixture of the two | S 1 0 , m F = ± 1 / 2 ⟩ states. Forced evaporative cooling lowers the temperature to 15 nK = 0.1 T F , where T F is the Fermi temperature, with 1 0 4 atoms per spin state. The two-spin-state mixture is then adiabatically loaded into a deep 3D optical lattice with typical trap frequencies of 2 π × 50 kHz and negligible tunneling. A homogenous magnetic field of 4.9 G, oriented vertically, allows for spectroscopic addressing of either m F state while on-site interactions enable spectroscopic addressing of either singly or multiply occupied states. Atoms in singly occupied sites of a particular spin state, | g ⟩ = | S 1 0 , m F ⟩ for m F = + 1 / 2 or - 1 / 2 , are transferred to the long-lived excited state | e ⟩ = | P 3 0 , m F ⟩ using a π pulse from an ultrastable clock laser (26 mHz linewidth) [25] . We remove any remaining atoms in other spin states or in multiply occupied sites. We then interrogate the e atoms using Ramsey spectroscopy [26] , first by placing atoms in a superposition state | g ⟩ + | e ⟩ with a π / 2 pulse, then waiting several seconds as the two states acquire a relative phase shift ϕ , with a state | g ⟩ + e - i ϕ | e ⟩ . A final π / 2 pulse converts this phase difference into a population difference, i sin ϕ | g ⟩ + cos ϕ | e ⟩ . We use state-dependent absorption imaging to measure the spatial distribution of the | g ⟩ and | e ⟩ state populations in the horizontal plane, from which we infer the atomic clock frequency distribution [27] . The g atoms are imaged with a 5 or 10 μ s pulse of resonant 461 nm light and subsequently removed. The e atoms are then repumped to g and imaged with a second pulse of resonant light [28] . A final pulse without atoms is used to acquire a reference image. The data are processed to generate column densities of the ground state n ˜ g [Fig. 1(b) ], excited state n ˜ e [Fig. 1(c) ], and normalized excitation fraction p ˜ e = n ˜ e / ( n ˜ e + n ˜ g ) [Fig. 1(d) ]. Imaging is done at saturation intensity for the best signal-to-noise ratio [32–35] . 1 10.1103/PhysRevLett.120.103201.f1 FIG. 1. Imaging spectroscopy experimental sequence. (a) A spin mixture of | S 1 0 , m F = ± 1 / 2 ⟩ atoms is loaded into a 3D optical lattice. A π pulse drives singly occupied sites of one spin state to the excited state, after which all other atoms are removed. The remaining atoms are placed in a superposition state and then read out with absorption imaging. Images are processed to yield the column density of (b) the ground state n ˜ g , (c) the excited state n ˜ e , and (d) the excitation fraction p ˜ e . Small spatial frequency shifts can be measured through changes in p ˜ e . (e) The normalized autocorrelation function of the central 15 μ m × 10 μ m region of p ˜ e (black points) demonstrates correlations induced by the imaging system that correspond to a 1.1 μ m imaging resolution (red line). Spatial correlations of the density characterize an imaging system’s resolution [36] . Here, we measure correlations in the excitation fraction by placing atoms in the state | g ⟩ + | e ⟩ . An imaging sequence projects the atomic wave function on each lattice site onto either | g ⟩ or | e ⟩ . This projection produces well-calibrated binomial noise with zero correlation length. The finite imaging resolution creates spatial correlations in the images (but not in the actual sample). The measured spatial autocorrelation function (black points, Fig. 1 ), ⟨ ( p ˜ e i - p ¯ e ) ( p ˜ e i + j - p ¯ e ) ⟩ / var p ˜ e , corresponds to a 1 / e 2 radius imaging resolution of 1.1 μ m for a 5 μ s imaging pulse time (red line). Here, p ¯ e is the average excitation fraction taken over all pixels i . Longer pulse times have a slightly worse imaging resolution as atoms are accelerated out of the depth of field [28] . We use a series of images similar to Fig. 1(d) to determine small differences in the clock frequency across the lattice. Frequency shifts are measured by comparing the excitation fractions in one region against another, with a frequency uncertainty set by QPN, removing the laser frequency (or phase) noise. Magnetic fields, interactions, or the lattice light can shift the local clock frequency. A spatially varying clock transition frequency creates a spatially inhomogeneous excitation fraction, p ˜ e ( r ) = 1 2 + C 2 cos [ 2 π f ( r ) T + ϕ 0 ] , (1) where C is the contrast, f ( r ) is the local clock frequency, T is the Ramsey free-evolution time, and ϕ 0 is a common-mode phase offset. Small misalignments in the lattice beams and birefringence of the vacuum chamber windows induce a small gradient of the vector ac Stark shift. A typical value is approximately m F × 20 mHz across the 50 μ m sample size, corresponding to a fictitious magnetic field gradient of 0.04 G / cm . Ordinarily, such a small gradient would be negligible in state-of-the-art optical lattice clocks, as this frequency shift is sufficiently small and can be averaged away using opposite m F states. We apply an additional (real) magnetic field gradient, enabling us to either cancel or increase the overall spatial frequency shifts. A parametric plot of the excitation fraction P 1 of region 1 against P 2 of region 2 [regions marked in Fig. 2(a) ] shows a clear ellipse [Fig. 2(b) ]. The eccentricity of the ellipse increases as the phase difference 2 π ( f 1 - f 2 ) T increases with longer interrogation times, where f i is the average frequency in region i . For short times, T = 0.1 s , we observe nearly perfect contrast in the excitation fraction with a small phase difference. At longer times, the frequency difference becomes more apparent as an increasing eccentricity of the ellipse [Fig. 2(b) ]. The contrast decreases with a time constant of 8 s, likely due to Raman scattering of lattice photons by e atoms [37] . 2 10.1103/PhysRevLett.120.103201.f2 FIG. 2. Imaging the local excitation fraction allows for the determination of small frequency shifts within the lattice-trapped sample. (a) A map of the excitation fraction of atoms after a Ramsey sequence ( T = 5 s ) is split into two separate regions. (b) Parametric plots of P 1 against P 2 (black points) show ellipses, created by a reproducible phase shift between the two regions. A maximum likelihood estimator determines the ellipse properties (red line). The phase shift increases with T for a fixed frequency difference f 1 - f 2 , while the contrast decays. (c) The measured uncertainty δ ( f 1 - f 2 ) for 900 s averaging time (blue points) closely follows the expected QPN limit for ellipse fitting (blue line). The measurements remain QPN-limited for 1000 experimental repetitions (red square and line), reaching a fractional uncertainty of 2.5 × 10 - 19 , with (inset) a total Allan deviation that averages with a slope of 3.6 × 10 - 17 / Hz . This uncertainty would correspond to a 2.3 mm gravitational redshift on the Earth. The frequencies are normalized to the clock frequency f 0 ≈ 429 THz of Sr 87 . The competition between a linearly increasing phase shift and an exponentially decreasing contrast creates a maximum signal-to-noise ratio at 4 s [Fig. 2(c) ] [28] . The fractional uncertainty δ ( f 1 - f 2 ) / f 0 is measured from T = 0.1 to 20 s [Fig. 2(c) , blue circles] and matches well with the calculated QPN limit of the 3000 atoms in each rectangle (blue curve) for a fixed per cycle dead time of 16 s and total measurement time of 900 s. This synchronous measurement technique can reach record-breaking performance for extended measurement times. The fractional uncertainty from averaging 1000 experimental repetitions over six hours [red square, Fig. 2(c) ] is set by the QPN limit (red curve) and has an Allan deviation consistent with white noise [Fig. 2(c) , inset]. The uncertainty of 2.5 × 10 - 19 , the best measured in any system, corresponds to a 100 μ Hz frequency uncertainty, or a 2.7 × 10 - 3 rad uncertainty of a 1.08 × 10 16 rad total phase shift over a 4 s coherent evolution time. We use the spatial mapping of the clock frequency to rapidly determine the differential ac Stark shift induced by the optical trap. The uncertainty in this shift remains the second largest systematic effect in state-of-the-art clocks [3] . As measurement precision improves, the higher-order effects in the 10 - 19 region will be investigated [39] . In previous work, measurements of the differential ac Stark shift were performed by asynchronously comparing the clock frequency in different lattice depths against an ultrastable cavity acting as a frequency flywheel. These measurements are typically dominated by laser noise, yielding a precision worse than what could be achieved in a QPN-limited system [3] . Imaging spectroscopy allows for a measurement of the differential ac Stark shift within a single image. In previous work, combining imaging with spectroscopy or interferometry has been used to measure the spatial distribution of scalar [40] and vector [41] ac Stark shifts, dipolar magnetic fields [27] , and microwave field strength [42,43] . Here, we apply imaging spectroscopy to evaluate the differential ac Stark shift in a record short time. The vertical lattice beam, which propagates along the imaging axis, is used to create a spatially inhomogeneous clock frequency because the optical lattice intensity varies with the Gaussian profile of the trapping laser beam [Fig. 3(a) ]. The local clock frequency f ( r ) then varies spatially, depending on the local lattice intensity I ( r ) . We measure the position-dependent excitation fraction as described in Eq. (1) and shown schematically in Fig. 3(b) . A sample image [Fig. 3(c) ] of the excitation fraction changes radially from the center of the trap as the optical lattice intensity decreases. We exaggerate the effect by detuning the frequency of the vertical lattice beam by 1 GHz from the magic frequency, the frequency of the laser at which the differential ac Stark shift vanishes. This large detuning creates an overall 1 Hz mismatch of the | g ⟩ and | e ⟩ state potentials, out of a total ac Stark shift of 300 kHz [Fig. 3(a) ]. We choose T = 4 s , such that in each realization, atoms on the edge of the trap wrap greater than a 2 π rad phase shift as compared to the center [Fig. 3(b) ], leading to clear rings in the local excitation fraction [Fig. 3(c) ]. 3 10.1103/PhysRevLett.120.103201.f3 FIG. 3. Determining the lattice magic frequency through imaging spectroscopy. (a) When the lattice frequency is higher than the magic frequency, e atoms (red line) experience a deeper potential than g atoms (blue line, not to scale). (b) The mismatch in lattice potentials results in a spatially dependent clock frequency that we measure via p ˜ e after a Ramsey sequence, with a population that varies from 1 2 + C to 1 2 - C , where C is the contrast. An image of p ˜ e from a single cycle of the experiment is shown in (c). (d) A fit of the distance between the imaged rings gives a single-shot estimate of the differential ac Stark shift, which we determine separately for the m F = 1 / 2 (purple circles) and - 1 / 2 (orange squares) states. Detuning of the lattice light is from the scalar magic frequency 368.554 725 THz [38] . (e) The uncertainty in the differential ac Stark shift averages down rapidly (black circles, fit is black line), with a QPN limit (dashed black line) 10 times better than the state-of-the-art Ref. [3] . Each image is fit to a model including a local frequency shift proportional to the local intensity f ( r ) = f 0 + a ( f lattice ) I ( r ) , where I ( r ) is local intensity of the vertical lattice beam and a ( f lattice ) is our fit determining the differential ac Stark shift. The intensity of the vertical optical lattice beam is measured with motional sideband spectroscopy [44] , while the beam waist is determined independently. We measure the coefficient a ( f lattice ) at three trapping light frequencies for both m F = ± 1 / 2 spin states [Fig. 3(d) ]. Averaging the coefficient for the two spin states removes the vector ac Stark shift and allows us to determine the combined scalar plus tensor differential ac Stark shift [black line, Fig. 3(d) ] [5] . Synchronous interrogation removes laser noise that limited previous asynchronous measurements. The differential ac Stark shift uncertainty is limited by the statistical noise of the measured coefficient, with a standard error of the mean δ a ( f lattice ) . The peak differential ac Stark shift uncertainty while operating the lattice at the measured magic frequency is then U op δ a ( f lattice ) , where U op = 30 E rec is the operational lattice depth, E rec = h × 3.47 kHz is the lattice photon recoil energy, and h is the Planck constant. In Ref. [3] , laser noise dominated the measurement imprecision, requiring ∼ 13 hours of averaging to reach an uncertainty of 1.1 × 10 - 18 . Our measurement (black points) rejects laser noise and requires only 1 hour to reproduce this uncertainty. We have not yet reached the ultimate limit of this technique, the QPN limit, which would require only 6 minutes of averaging. We believe the measurement noise is in excess of QPN noise because this measurement is made with the entire sample, including the relatively low-density edge of the sample. These rapid measurement times open the possibility of reaching an uncertainty at the 10 - 19 level and studying hyperpolarizability shifts [39,45] . Finally, we use the atomic sample in a highly dispersive, multiplexed measurement of the frequency noise of an ultrastable laser. A magnetic field gradient 0.26 G / cm shifts the clock frequency by approximately 1 Hz across the sample. This, in combination with our 1.1 μ m imaging resolution, yields a 14 mHz frequency resolution. In this experiment, we use the m F = + 9 / 2 state for increased frequency sensitivity and calibrate the magnetic field gradient with Ramsey spectroscopy. The magnetic field gradient converts Ramsey fringes, the sinusoidal response of atoms to a laser frequency, into a sinusoidal spatial response [Fig. 4(a) ]. The range of the magnetic fields is sufficiently small, such that all atoms respond to the short laser pulses used in Ramsey spectroscopy. Laser noise manifests itself as a shot-to-shot variation in the location of the spatial nodes, but it cannot be observed from a single image. To measure the laser noise, we perform Rabi spectroscopy for 8 s, such that only atoms in a narrow spatial region, 8 μ m width for the 100 mHz Fourier limit, can be excited by this laser. Frequency excursions excite a spatially broadened region. In this way, imaging spectroscopy serves as a multiplexed measurement of laser frequency noise [25] , and as a dispersive element that converts frequency shifts into position variations of the atomic excitation. The observed linewidth of 150 mHz (Fig. 4 ), the narrowest Rabi line shape measured on an optical transition, is limited mainly by the 8 s | e ⟩ state lifetime in the lattice. 4 10.1103/PhysRevLett.120.103201.f4 FIG. 4. Synchronous Rabi and Ramsey spectroscopy of an ultrastable laser. An applied magnetic field gradient creates a spatially dependent clock frequency. This effectively “disperses” the signal by converting the frequency response into a spatial pattern, a multiplexed measurement of the laser noise and atomic response. (a) In Ramsey spectroscopy, nearly all laser noise is common mode. “Ramsey fringes” are imaged as a spatially sinusoidal excitation fraction that measures the linearly increasing frequency shift across the sample, with T = 6 s . (b) In Rabi spectroscopy, the entire lattice is illuminated by a clock pulse for 8 s. Only atoms in a narrow spatial region can be excited. Here, the measured linewidth is 150 mHz. In conclusion, imaging spectroscopy on the clock transition of lattice-trapped degenerate AE fermions combines the use of micron-resolution spatial imaging with submillihertz frequency resolution for advancing the measurement capabilities of atomic clocks. Comparing the frequency shifts of separated regions within a 3D lattice allows for rapid and precise measurements, reaching a record frequency precision of 2.5 × 10 - 19 in 6 hours, limited by the QPN of 3000 atoms interrogated coherently for 4 s. We apply these techniques to determine the differential ac Stark shift more rapidly than all previous work. We also observe the narrowest atomic linewidth on an optical transition. High spatial and frequency resolution imaging spectroscopy will be used to explore many-body physics through maps of local position and frequency density of states, and test the interplay of quantum mechanics and general relativity on the millimeter scale. We acknowledge technical contributions from W. Milner, E. Oelker, J. Robinson, L. Sonderhouse, W. Zhang, and useful discussions with T. Bothwell, S. Bromley, C. Kennedy, D. Kedar, S. Kolkowitz. This work is supported by NIST, DARPA, AFOSR-MURI, and the NSF JILA Physics Frontier Center (NSF PHY-1734006). G. E. M. is supported by a postdoctoral fellowship from the National Research Council and A. G. is supported by a postdoctoral fellowship from the Japan Society for the Promotion of Science. N. P. is partially supported by the JILA Visiting Fellowship. [1] 1 B. J. Bloom , T. L. Nicholson , J. R. Williams , S. L. Campbell , M. Bishof , X. Zhang , W. Zhang , S. L. Bromley , and J. Ye , Nature (London) 506 , 71 ( 2014 ). NATUAS 0028-0836 10.1038/nature12941 [2] 2 I. Ushijima , M. Takamoto , M. Das , T. Ohkubo , and H. Katori , Nat. Photonics 9 , 185 ( 2015 ). NPAHBY 1749-4885 10.1038/nphoton.2015.5 [3] 3 T. L. Nicholson , S. L. Campbell , R. B. Hutson , G. E. Marti , B. J. Bloom , R. L. McNally , W. Zhang , M. D. Barrett , M. S. Safronova , G. F. Strouse , W. L. Tew , and J. Ye , Nat. Commun. 6 , 6896 ( 2015 ). NCAOBW 2041-1723 10.1038/ncomms7896 [4] 4 M. Schioppo , R. C. Brown , W. F. McGrew , N. Hinkley , R. J. Fasano , K. Beloy , T. H. Yoon , G. Milani , D. Nicolodi , J. A. Sherman , N. B. Phillips , C. W. Oates , and A. D. Ludlow , Nat. Photonics 11 , 48 ( 2017 ). NPAHBY 1749-4885 10.1038/nphoton.2016.231 [5] 5 S. L. Campbell , R. B. Hutson , G. E. Marti , A. Goban , N. Darkwah Oppong , R. L. McNally , L. Sonderhouse , J. M. Robinson , W. Zhang , B. J. Bloom , and J. Ye , Science 358 , 90 ( 2017 ). SCIEAS 0036-8075 10.1126/science.aam5538 [6] 6 M. J. Martin , M. Bishof , M. D. Swallows , X. Zhang , C. Benko , J. von-Stecher , A. V. Gorshkov , A. M. Rey , and J. Ye , Science 341 , 632 ( 2013 ). SCIEAS 0036-8075 10.1126/science.1236929 [7] 7 X. Zhang , M. Bishof , S. L. Bromley , C. V. Kraus , M. S. Safronova , P. Zoller , A. M. Rey , and J. Ye , Science 345 , 1467 ( 2014 ). SCIEAS 0036-8075 10.1126/science.1254978 [8] 8 S. Kolkowitz , S. L. Bromley , T. Bothwell , M. L. Wall , G. E. Marti , A. P. Koller , X. Zhang , A. M. Rey , and J. Ye , Nature (London) 542 , 66 ( 2017 ). NATUAS 0028-0836 10.1038/nature20811 [9] 9 F. Scazza , C. Hofrichter , M. Höfer , P. C. De Groot , I. Bloch , and S. Fölling , Nat. Phys. 10 , 779 ( 2014 ). NPAHAX 1745-2473 10.1038/nphys3061 [10] 10 G. Cappellini , M. Mancini , G. Pagano , P. Lombardi , L. Livi , M. Siciliani de Cumis , P. Cancio , M. Pizzocaro , D. Calonico , F. Levi , C. Sias , J. Catani , M. Inguscio , and L. Fallani , Phys. Rev. Lett. 113 , 120402 ( 2014 ). PRLTAO 0031-9007 10.1103/PhysRevLett.113.120402 [11] 11 M. Höfer , L. Riegger , F. Scazza , C. Hofrichter , D. R. Fernandes , M. M. Parish , J. Levinsen , I. Bloch , and S. Folling , Phys. Rev. Lett. 115 , 265302 ( 2015 ). PRLTAO 0031-9007 10.1103/PhysRevLett.115.265302 [12] 12 M. Mancini , G. Pagano , G. Cappellini , L. Livi , M. Rider , J. Catani , C. Sias , P. Zoller , M. Inguscio , M. Dalmonte , and L. Fallani , Science 349 , 1510 ( 2015 ). SCIEAS 0036-8075 10.1126/science.aaa8736 [13] 13 D. E. Chang , J. Ye , and M. D. Lukin , Phys. Rev. A 69 , 023810 ( 2004 ). PLRAAN 1050-2947 10.1103/PhysRevA.69.023810 [14] 14 S. Krämer , L. Ostermann , and H. Ritsch , Europhys. Lett. 114 , 14003 ( 2016 ). EULEEJ 0295-5075 10.1209/0295-5075/114/14003 [15] 15 M. Foss-Feig , M. Hermele , and A. M. Rey , Phys. Rev. A 81 , 051603 ( 2010 ). PLRAAN 1050-2947 10.1103/PhysRevA.81.051603 [16] 16 L. Riegger , N. D. Oppong , M. Höfer , D. Rio Fernandes , I. Bloch , and S. Fölling , arXiv:1708.03810 . [17] 17 C. Honerkamp and W. Hofstetter , Phys. Rev. Lett. 92 , 170403 ( 2004 ). PRLTAO 0031-9007 10.1103/PhysRevLett.92.170403 [18] 18 M. Hermele , V. Gurarie , and A. M. Rey , Phys. Rev. Lett. 103 , 135301 ( 2009 ). PRLTAO 0031-9007 10.1103/PhysRevLett.103.135301 [19] 19 A. V. Gorshkov , M. Hermele , V. Gurarie , C. Xu , P. S. Julienne , J. Ye , P. Zoller , E. Demler , M. D. Lukin , and A. M. Rey , Nat. Phys. 6 , 289 ( 2010 ). NPAHAX 1745-2473 10.1038/nphys1535 [20] 20 W. Hofstetter , J. I. Cirac , P. Zoller , E. Demler , and M. D. Lukin , Phys. Rev. Lett. 89 , 220407 ( 2002 ). PRLTAO 0031-9007 10.1103/PhysRevLett.89.220407 [21] 21 S. Trebst , U. Schollwöck , M. Troyer , and P. Zoller , Phys. Rev. Lett. 96 , 250402 ( 2006 ). PRLTAO 0031-9007 10.1103/PhysRevLett.96.250402 [22] 22 A. M. Rey , R. Sensarma , S. Fölling , M. Greiner , E. Demler , and M. D. Lukin , Europhys. Lett. 87 , 60001 ( 2009 ). EULEEJ 0295-5075 10.1209/0295-5075/87/60001 [23] 23 C. W. Chou , D. B. Hume , T. Rosenband , and D. J. Wineland , Science 329 , 1630 ( 2010 ). SCIEAS 0036-8075 10.1126/science.1192720 [24] 24 M. Zych , F. Costa , I. Pikovski , and C̆. Brukner , Nat. Commun. 2 , 505 ( 2011 ). NCAOBW 2041-1723 10.1038/ncomms1498 [25] 25 M. Bishof , X. Zhang , M. J. Martin , and J. Ye , Phys. Rev. Lett. 111 , 093604 ( 2013 ). PRLTAO 0031-9007 10.1103/PhysRevLett.111.093604 [26] 26 N. F. Ramsey , Phys. Rev. 78 , 695 ( 1950 ). PHRVAO 0031-899X 10.1103/PhysRev.78.695 [27] 27 G. E. Marti , A. MacRae , R. Olf , S. Lourette , F. Fang , and D. M. Stamper-Kurn , Phys. Rev. Lett. 113 , 155302 ( 2014 ). PRLTAO 0031-9007 10.1103/PhysRevLett.113.155302 [28] 28 See Supplemental Material at http://link.aps.org/supplemental/10.1103/PhysRevLett.120.103201 for a description of imaging effects, the QPN limit of ellipse fitting, and statistical analysis, which includes Refs. [29–31]. [29] 29 G. T. Foster , J. B. Fixler , J. M. McGuirk , and M. A. Kasevich , Opt. Lett. 27 , 951 ( 2002 ). OPLEDP 0146-9592 10.1364/OL.27.000951 [30] 30 J. K. Stockton , X. Wu , and M. A. Kasevich , Phys. Rev. A 76 , 033613 ( 2007 ). PLRAAN 1050-2947 10.1103/PhysRevA.76.033613 [31] 31 R. G. Miller , Biometrika 61 , 1 ( 1974 ). BIOKAX 0006-3444 10.1093/biomet/61.1.1 [32] 32 G. Reinaudi , T. Lahaye , Z. Wang , and D. Guéry Odelin , Opt. Lett. 32 , 3143 ( 2007 ). OPLEDP 0146-9592 10.1364/OL.32.003143 [33] 33 K. Maussang , G. E. Marti , T. Schneider , P. Treutlein , Y. Li , A. Sinatra , R. Long , J. Esteve , and J. Reichel , Phys. Rev. Lett. 105 , 080403 ( 2010 ). PRLTAO 0031-9007 10.1103/PhysRevLett.105.080403 [34] 34 W. Muessel , H. Strobel , M. Joos , E. Nicklas , I. Stroescu , J. Tomkovič , D. B. Hume , and M. K. Oberthaler , Appl. Phys. B 113 , 69 ( 2013 ). APBOEM 0946-2171 10.1007/s00340-013-5553-8 [35] 35 G. E. Marti and D. M. Stamper Kurn , in Proceedings of the International School of Physics “Enrico Fermi” on Quantum Matter at Ultralow Temperatures , edited by M. Inguscio , W. Ketterle , S. Stringari , and G. Roati ( IOS Press , Amsterdam, 2016 ), Vol. 191 , p. 221 . [36] 36 C.-L. Hung , X. Zhang , L.-C. Ha , S.-K. Tung , N. Gemelke , and C. Chin , New J. Phys. 13 , 075019 ( 2011 ). NJOPFM 1367-2630 10.1088/1367-2630/13/7/075019 [37] 37 R. B. Hutson ,
PY - 2018/3/5
Y1 - 2018/3/5
N2 - We implement imaging spectroscopy of the optical clock transition of lattice-trapped degenerate fermionic Sr in the Mott-insulating regime, combining micron spatial resolution with submillihertz spectral precision. We use these tools to demonstrate atomic coherence for up to 15 s on the clock transition and reach a record frequency precision of 2.5×10-19. We perform the most rapid evaluation of trapping light shifts and record a 150 mHz linewidth, the narrowest Rabi line shape observed on a coherent optical transition. The important emerging capability of combining high-resolution imaging and spectroscopy will improve the clock precision, and provide a path towards measuring many-body interactions and testing fundamental physics.
AB - We implement imaging spectroscopy of the optical clock transition of lattice-trapped degenerate fermionic Sr in the Mott-insulating regime, combining micron spatial resolution with submillihertz spectral precision. We use these tools to demonstrate atomic coherence for up to 15 s on the clock transition and reach a record frequency precision of 2.5×10-19. We perform the most rapid evaluation of trapping light shifts and record a 150 mHz linewidth, the narrowest Rabi line shape observed on a coherent optical transition. The important emerging capability of combining high-resolution imaging and spectroscopy will improve the clock precision, and provide a path towards measuring many-body interactions and testing fundamental physics.
UR - http://www.scopus.com/inward/record.url?scp=85043698969&partnerID=8YFLogxK
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U2 - 10.1103/PhysRevLett.120.103201
DO - 10.1103/PhysRevLett.120.103201
M3 - Article
C2 - 29570334
AN - SCOPUS:85043698969
VL - 120
JO - Physical Review Letters
JF - Physical Review Letters
SN - 0031-9007
IS - 10
M1 - 103201
ER -