Auxiliary functions of the
                    <b>LISA</b>
                    laser link: ranging, clock noise transfer and data communication

Heinzel, Gerhard; Esteban, Juan José; Barke, Simon; Otto, Markus; Wang, Yan; Díaz, Antonio; Danzmann, K.

doi:10.1088/0264-9381/28/9/094008

Cited by 59 publications

(40 citation statements)

References 17 publications

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“…Except the AR-coating of the crystal, a similar design should also work out at 532 nm. EOMs at a wavelength of 1064 nm are investigated in the context of the LISA mission, also addressing space relevant criteria [26], [27].…”

Section: Laser System At 532 Nmmentioning

confidence: 99%

A high-performance iodine-based frequency reference for space applications

Schuldt

Döringshoff

Reggentin

et al. 2017

International Conference on Space Optics — ICSO 2012

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Abstract-We present the development of a compact optical frequency reference with a stability in the 10 −15 domain at longer integration times utilizing Doppler-free spectroscopy based on molecular iodine. With respect to its future application in space, a setup on elegant breadboard (EBB) level was realized and successfully implemented and tested. A frequency stability of 5 · 10 −15 at an integration time of 200 s was verified in a beat measurement with a ULE cavity setup. For ensuring high thermal and mechanical stability, the EBB utilizes a baseplate made of ultra-low CTE glass ceramics. The optical components are fixed to the baseplate using an adhesive bonding technology. In a current activity, a setup on engineering model (EM) level will be realized with increased compactness and stability compared to the EBB setup utilizing a very compact multipass gas cell.

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Section: Laser System At 532 Nmmentioning

confidence: 99%

A high-performance iodine-based frequency reference for space applications

Schuldt

Döringshoff

Reggentin

et al. 2017

International Conference on Space Optics — ICSO 2012

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“…Armlength accuracies at the centimeters level have already been demonstrated in the laboratory [16, 50, 64, 26], making us confident that the required level of time-delays accuracy will be available.…”

Section: Experimental Aspects Of Tdimentioning

confidence: 99%

“…As a final note, a required clock synchronizations of about 40 ns derived in this section translates into a ranging accuracy of 12 meters, which has been experimentally shown to be easily achievable [16, 50, 64, 26]. …”

Section: Experimental Aspects Of Tdimentioning

confidence: 99%

Time-Delay Interferometry

Tinto

Dhurandhar

2014

Living Rev. Relativ.

121

113

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Equal-arm detectors of gravitational radiation allow phase measurements many orders of magnitude below the intrinsic phase stability of the laser injecting light into their arms. This is because the noise in the laser light is common to both arms, experiencing exactly the same delay, and thus cancels when it is differenced at the photo detector. In this situation, much lower level secondary noises then set the overall performance. If, however, the two arms have different lengths (as will necessarily be the case with space-borne interferometers), the laser noise experiences different delays in the two arms and will hence not directly cancel at the detector. In order to solve this problem, a technique involving heterodyne interferometry with unequal arm lengths and independent phase-difference readouts has been proposed. It relies on properly time-shifting and linearly combining independent Doppler measurements, and for this reason it has been called time-delay interferometry (TDI).This article provides an overview of the theory, mathematical foundations, and experimental aspects associated with the implementation of TDI. Although emphasis on the application of TDI to the Laser Interferometer Space Antenna (LISA) mission appears throughout this article, TDI can be incorporated into the design of any future space-based mission aiming to search for gravitational waves via interferometric measurements. We have purposely left out all theoretical aspects that data analysts will need to account for when analyzing the TDI data combinations.

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“…The clock noise is another essential element, because the space-qualified ultra-stable oscillator (USO) cannot meet LISA's requirement [34,35]. The relationship between the clock noise and the stability of the USO is [33,36]:…”

Section: Clock Jitter Noisementioning

confidence: 99%

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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Auxiliary functions of the LISA laser link: ranging, clock noise transfer and data communication

Cited by 59 publications

References 17 publications

A high-performance iodine-based frequency reference for space applications

A high-performance iodine-based frequency reference for space applications

Time-Delay Interferometry

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

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