Weak-light phase tracking with a low cycle slip rate

Francis, Samuel P.; Lam, Thanh; McKenzie, Kirk; Sutton, Andrew J.; Ward, R. L.; McClelland, D. E.; Shaddock, D. A.

doi:10.1364/ol.39.005251

Cited by 31 publications

(21 citation statements)

References 12 publications

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“…signal' is given based on the references [41][42][43] that the strain amplitude of major LISA G.W. sources, after one year integration, could reach to a level from 21 10 Hz  to 18 10 Hz  strongly depends on the distances and types. In the following sections, the effects of the frequency noise and the clock noise on the performance of WLPL for LISA will be emphasized.…”

Section: Simulation Results and Discussionmentioning

confidence: 99%

“…It has been mentioned that Laser Interferometer Space Antenna (LISA) phasemeter looked at reducing the probability of cycle slipping when tracking a 3.5 pW signal [18]. Indeed, the received power for LISA will be more than 100 pW, the phase lock loop will operate far outside any cycle slip region and therefore in the linear region [45].…”

Section: Discussionmentioning

confidence: 99%

“…Although WLPL is unnecessary in the ground based laser interferometric gravitational wave observers, it has been researched along with the increasing interest in weak light detection and the thriving scheme of extremely long laser ranging in space by scientists since the end of the last century. In previous experimental demonstration of WLPL for LISA, the laser measurement instrument noises, however, have not been considered [13][14][15][16][17][18][19][20]. Since the phase-locking at pico-watt region is very stringent due to the low signal to noise ratio (SNR), the systematic complicity and the technical difficulty will make the situation even worse in debt of the introduction of such the instrument noises as shot noise, pointing jitter noise, laser frequency noise, clock jitter noise, phase readout noise, proof mass acceleration noise, etc..…”

Section: Introductionmentioning

confidence: 99%

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A comprehensive simulation of weak-light phase-locking for space-borne gravitational wave antenna

Dong

Liu

Luo

et al. 2016

Sci. China Technol. Sci.

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A comprehensive simulation was performed to better understand the impacts and effects of the additional technical noises on weak-light phase-locking for LISA. The result showed that the phase of the slave laser tracked well with the received transmitting light under different noise level, and the locking precision was limited by the phase readout noise when the laser frequency noise and clock jitter noise were removed. This result was then confirmed by a benchtop experimental test. The required LISA noise floor was recovered from the simulation which proved the validity of the simulation program. In order to convert the noise function into real time data with random characteristics, an algorism based on Fourier transform was also invented.

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Section: Simulation Results and Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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A comprehensive simulation of weak-light phase-locking for space-borne gravitational wave antenna

Dong

Liu

Luo

et al. 2016

Sci. China Technol. Sci.

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“…In JPL (Jet Propulsion Laboratory), Dick et al [29] have achieved offset phase locking of local oscillator to 40 fW incoming laser light. More recently, Gerberding et al [30] and Francis et al [31] have phase-locked and tracked a 3.5 pW weak light signal and a 30 fW weak light signal respectively at reduced cycle slipping rate. For LISA, 85 pW weaklight phase locking is required.…”

Section: Sensitivitymentioning

confidence: 99%

Astrodynamical middle-frequency interferometric gravitational wave observatory AMIGO: Mission concept and orbit design

Wang

2020

Int. J. Mod. Phys. D

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AMIGO is a first-generation Astrodynamical Middle-frequency Interferometric GW Observatory. The scientific goals of AMIGO are: to bridge the spectra gap between first-generation high-frequency and low-frequency GW sensitivities; to detect intermediate mass BH coalescence; to detect inspiral phase and predict time of binary black hole coalescence together with neutron star coalescence for ground interferometers; to detect compact binary inspirals for studying stellar evolution and galactic population. The mission concept is to use time delay interferometry for a nearly triangular formation of 3 drag-free spacecraft with nominal arm length 10,000 km, emitting laser power 2-10 W and telescope diameter 300-360 mm. The design GW sensitivity in the middle frequency band is 3 × 10 −21 Hz -1 . Four options of orbits are under study: (i) Earth-like solar orbits (2-20 degrees behind the Earth); (ii) 600,000 km high orbit formation around the Earth; (iii) 50,000 km-250,000 high orbit formation around the Earth; (iv) near Earth-Moon L4 (or L5) halo orbit formation. All four options have LISAlike formations, that is the triangular formation is 60º inclined to the orbit plane. For AMIGO, the first-generation time delay interferometry is good enough for the laser frequency noise suppression. We also investigate for each options of orbits under study, whether constant equal-arm implementation is feasible. For the solar-orbit option, the acceleration to maintain the formation can be designed to be less than 15 nm/s 2 with the thruster requirement in the 15 μN range. AMIGO would be a good place to implement the constant equal-arm option. Fuel requirement, thruster noise requirement and test mass acceleration actuation requirement are briefly considered. From the orbit study, the solar orbit option is the first mission orbit choice. We study the deployment for this orbit option. A last-stage launch from 300 km LEO (Low Earth Orbit) to an appropriate 2-degree-behindthe-Earth AMIGO formation in 95 days requires only a v of 75 m/s.

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“…These methods can provide exquisitely high accuracy but require a beat note with high signal-to-noise ratio. Too low a signal-to-noise ratio will lead to cycle slips and improper counting or phase locking [1,3,8,9]. This limits the range of conditions over which these methods apply.…”

Section: Introductionmentioning

confidence: 99%

Accurate laser frequency locking to optical frequency combs under low-signal-to-noise-ratio conditions

Guo

Favier

Galland

et al. 2020

Review of Scientific Instruments

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We demonstrate a method for accurately locking the frequency of a continuous-wave laser to an optical frequency comb in conditions where the signal-to-noise ratio is low, too low to accommodate other methods. Our method is typically orders of magnitude more accurate than conventional wavemeters and can considerably extend the usable wavelength range of a given optical frequency comb. We illustrate our method by applying it to the frequency control of a dipole lattice trap for an optical lattice clock, a representative case where our method provides significantly better accuracy than other methods.

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Weak-light phase tracking with a low cycle slip rate

Cited by 31 publications

References 12 publications

A comprehensive simulation of weak-light phase-locking for space-borne gravitational wave antenna

A comprehensive simulation of weak-light phase-locking for space-borne gravitational wave antenna

Astrodynamical middle-frequency interferometric gravitational wave observatory AMIGO: Mission concept and orbit design

Accurate laser frequency locking to optical frequency combs under low-signal-to-noise-ratio conditions

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