Far-field optical path noise coupled with the pointing jitter in the space measurement of gravitational waves

Zhao, Ya; Shen, Jia; Fang, Chao; Wang, Zhi; Gao, Ruihong; Sha, Wei E. I.

doi:10.1364/ao.405467

Cited by 15 publications

(15 citation statements)

References 15 publications

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“…The measuring beam with a wavefront residual ΔW can be expressed as: E meas (x, y, z) = A meas e −ik(x sin α+z cos α)+2πiΔW (18) where α is the angle of jitter. Zhao et al provided a complete derivation and code for this interference model [33]. Then we can get the TTL noise change rate caused by design residual wavefront error.…”

Section: Design Results and Performancementioning

confidence: 99%

High performance telescope system design for the TianQin project

Fan¹,

ZHAO²,

PENG³

et al. 2022

Class. Quantum Grav.

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China is planning to construct a new space-borne gravitational-wave (GW) observatory, the TianQin project, in which the spaceborne telescope is an important component in laser interferometry. The telescope is aimed to transmit laser beams between the spacecrafts for the measurement of the displacements between proof-masses in long arms. The telescope should have ultra-small wavefront deviation to minimize noise caused by pointing error, ultra-stable structure to minimize optical path noise caused by temperature jitter, ultra-high stray light suppression ability to eliminate background noise. In this paper, we realize a telescope system design with ultra-stable structure as well as ultra-low wavefront distortion for the space-based GW detection mission. The design requirements demand extreme control of high image quality and extraordinary stray light suppression ability. Based on the primary aberration theory, the initial structure design of the mentioned four-mirror optical system is explored. After optimization, the maximum RMS wavefront error is less than λ/300 over the full field of view (FOV), which meets the noise budget on the telescope design. The stray light noise caused by the back reflection of the telescope is also analyzed. The noise at the position of optical bench is less than 10-10 of the transmitted power, satisfying the requirements of space gravitational-wave detection. We believe that our design can be a good candidate for TianQin project, and can also be a good guide for the space telescope design in any other similar science project.

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Section: Design Results and Performancementioning

confidence: 99%

High performance telescope system design for the TianQin project

Fan¹,

ZHAO²,

PENG³

et al. 2022

Class. Quantum Grav.

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show abstract

“…In a previous work, we studied the principal prototype of the 200-mm-aperture space GW telescope. [14][15][16][17][18] In the current Taiji project mission, we have developed a 400-mm-aperture telescope to detect GWs in the frequency band 10 −4 to 1 Hz. In this study, according to the Taiji telescope requirements and based on the primary aberration theory, we have established a coaxial four-mirror initial structure with an aperture of 400 mm, which eliminates the central occlusion through the off-axis aperture.…”

Section: Introductionmentioning

confidence: 99%

“…Although, it is difficult to quantitatively analyze the contribution of a single factor to TTL coupling noise, the noise source can be suppressed. Thus far, 8 – 13 Zhao presented a comprehensive theoretical analysis of the influence of telescope aberration on TTL coupling noise, proposed that the coupling coefficient should be suppressed at ±25 pm/μrad, analyzed the contribution of TTL coupling noise of the prototype of the Taiji project telescope principle, and determined whether the final optical path stability has exceeded 3 pm/√Hz 14 …”

Section: Introductionmentioning

confidence: 99%

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Optical system design of large-aperture space gravitational wave telescope

Miao

Lin

et al. 2023

Opt. Eng.

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.In the Taiji Program, the space gravitational wave (GW) telescope is an important component of the space laser interferometer, which is used to receive and transmit laser signals, and has strict requirements in terms of light intensity signals and tilt-to-length (TTL) noise. Therefore, the telescope has a particular design; it should have a large aperture to meet the demand for light intensity signals, and the TTL coupling noise should be suppressed in the design process. Based on the primary aberration theory, the solution of the four-mirror off-axis initial structure is described. According to the interference model of flat-topped and Gaussian beams, the coupling coefficient of wavefront error and TTL noise at the exit pupil of the telescope are analytically calculated using the average phase signal. The optimization method and design flow are established, considering the special requirements of the space GW telescope. The results indicate that the diameter of the telescope entrance pupil is 400 mm, and the system magnification is 80 × . The root mean square (RMS) value of wavefront errors is better than 0.00504 λ (λ = 1064 nm) within ±8 μrad of the scientific field of view, and the coupling coefficient is not more than 1.7 pm / μrad within ±600 μrad of jitter angle. The tolerance analysis of the design results shows that the RMS value and coupling coefficient meet the requirements of space GW detection. Therefore, the proposed design is a good candidate for the Taiji Program.

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“…Kenny analyzed the wavefront distortion composed of the first 11 terms of Zernike polynomials, and obtained that only those terms with even noll index are relevant to the measured phase error coupling to the beam alignment [13]. Zhao et al built a wavefront distortion model with the first 25 terms of Zernike polynomials and investigated the far-field optical-path-length noise of one telescope prototype [14]. Previous works have already analyzed the measurement noise induced by the coupling of wavefront distortion and beam pointing misalignment by means of numerical and ray-tracing methods.…”

Section: Introductionmentioning

confidence: 99%

Analysis on the coupling effect of wavefront distortion and pointing misalignment in space laser interferometry

Min¹,

Jiang²,

Zhang³

et al. 2021

Class. Quantum Grav.

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Space-based gravitational wave detection aims to measure gravitational waves with strains of down to 10−20 in 10−4 Hz ∼ 1 Hz frequency band. In order to achieve this measurement sensitivity, inter-satellite laser interferometry with picometer precision for an armlength of 108 ∼ 109 m is required. However, the coupling of the transmitting-beam misalignment and the wavefront distortion results in a non-negligible measurement error of intersatellite laser interferometry. Considering a wavefront distortion model composed of the first 55 terms of Zernike polynomials, we analyze the coupling effect of beam misalignment and wavefront distortion in both analytical and numerical methods. Calculation results show that the position of the stationary point is mainly determined by defocus, astigmatism and coma of the wavefront distortion of the transmitting beam. Moreover, a large defocus and small coma are preferred to achieve a better alignment of the stationary pointing direction with the inter-satellite line-of-sight, such that the coupling noise and received laser power can be optimized.

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Far-field optical path noise coupled with the pointing jitter in the space measurement of gravitational waves

Cited by 15 publications

References 15 publications

High performance telescope system design for the TianQin project

High performance telescope system design for the TianQin project

Optical system design of large-aperture space gravitational wave telescope

Analysis on the coupling effect of wavefront distortion and pointing misalignment in space laser interferometry

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