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Liu Y, Hua Z Y, Peng S J, et al. Research on optical field calculation methods in the space gravitational wave telescope[J]. Opto-Electron Eng, 2023, 50(11): 230186. doi: 10.12086/oee.2023.230186
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Research on optical field calculation methods in the space gravitational wave telescope
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Abstract
In the space gravitational wave detection system, the accuracy of the complex amplitude field distribution simulation at the telescope exit pupil closely affects the accuracy of the interferometric measurement and impacts the effectiveness of TTL noise control analysis. Therefore, it is necessary to carry out the high-precision diffraction calculation for the field propagation. This paper demonstrates the necessity of the vectorial ray-based diffraction integral algorithm for simulation and illustrates the algorithm flow combining the telescope model. A computational model was established based on the algorithm. The telescope system parameters were substituted to verify the wavefront calculation accuracy, and the vectorial field simulation results were presented. Based on the system model, the effects of the input Gaussian field parameters and the complex refractive index on the output vectorial optical field characteristics are simulated. -
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References
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Overview
The space gravitational wave detection program breaks through the limitation of the detection frequency band of the ground-based gravitational wave program and opens a new era of gravitational wave detection. The gravitational wave telescope is an important part of the laser heterodyne interferometry system, which plays a role in receiving and transmitting the laser signals, relaying and transforming the beam size. The complex amplitude field distribution at the telescope exit pupil closely affects the far-field phase and the amplitude distribution coupled into the receiving laser interferometer system, in turn, affects the accuracy of interferometric measurement. Meanwhile, the accuracy of the phase distribution simulation of the receiving telescope affects the effectiveness of TTL noise control analysis. Therefore, it is necessary to carry out the high-precision diffraction calculation for optical field propagation simulation. Due to the vector characteristics of the polarized light field and the non-paraxial propagation characteristics of the off-axis optical system, the phase distribution of the optical field at the telescope exit pupil will show different characteristics from the wavefront distribution of geometric optics. Therefore, the effects of the true boundary conditions on the field should be considered, and the strict vectorial diffraction calculation should be adopted. This paper explains the necessity of the strict vectorial diffraction field calculation based on polarization ray tracing in the space gravitational wave telescope, demonstrates the feasibility of VRBDI algorithm, and illustrates the algorithm flow combining the off-axis four-mirror afocal telescope model. A computational model was established based on the algorithm, and a set of telescope design parameters were substituted. The exit pupil wavefront was simulated in comparison with the result of ZEMAX, a commercial optical simulation software, verifying the ray tracing calculation accuracy of the simulation program reaching 10−6 pm level, and the results of optical field simulation were presented. Aiming at the two factors that may lead to the simulation deviation of the output vectorail field, the input Gaussian field parameters and the complex refractive index of the component surface, a series of simulation discussions were carried out. It is shown that the output vectorial field characteristics will vary with the input Gaussian beam waist radius and the waist distance. The variation of the phase distribution is analyzed by low order Zernike decomposition, and the Z5 term has the most positive correlation. The phase distributions of the output X polarization and Y polarization components when the elements are aluminum mirrors were simulated and were compared with the ideal reflection condition, and the phase difference of the two polarizations has some similarity in low-order aberration distributions.
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Liu Y, Hua Z Y, Peng S J, et al. Research on optical field calculation methods in the space gravitational wave telescope[J]. Opto-Electron Eng, 2023, 50(11): 230186. doi: 10.12086/oee.2023.230186
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Figure 1.
Schematic diagram of the space gravitational wave detector[4]
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Figure 2.
Schematic diagram of the optical structure of the gravitational wave telescope[9]
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Figure 3.
Schematic diagram of the algorithm flow of the gravitational wave telescope system model
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Figure 4.
Schematic diagram of the telescope system structure
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Figure 5.
Optical path data at the exit pupil of the transmitting telescope at the 0 degree field angle. (a) Calculation results of the optical field simulation model; (b) Calculation results of the simulation software ZEMAX; (c) The difference between (a) and (b)
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Figure 6.
Intensity distribution map on the input surface
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Figure 7.
Vectorial optical field distributions on the output surface of simulation calculation. (a) Intensity distribution map; (b) X polarization component amplitude distribution map; (c) X polarization component phase distribution map
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Figure 8.
The amplitude distributions of the output field change with the waist distance (unit: V/m)
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Figure 9.
The phase distributions of the output field change with the waist distance (unit: rad)
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Figure 10.
The amplitude distributions of the output field change with the waist radius (unit: V/m)
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Figure 11.
The phase distributions of the output field change with the waist radius (unit: rad)
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Figure 12.
The changes of Z5 coefficient. (a) Z5 coefficient in the phase distribution changes with the waist distance; (b) Z5 coefficient in the phase distribution changes with the waist radius. (c) Z5 (defocus) term distribution form
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Figure 13.
Phase distributions of the output X polarization field. (a) X polarization phase distribution under the ideal reflection; (b) X polarization phase distribution under the aluminum mirror reflection. (c) The difference in X polarization phase distribution between the aluminum mirror reflection case and the ideal reflection case
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Figure 14.
Phase distributions of the output Y polarization field. (a) Y polarization phase distribution under the ideal reflection; (b) Y polarization phase distribution under the aluminum mirror reflection; (c) The difference in Y polarization phase distribution between the aluminum mirror reflection case and the ideal reflection case
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Figure 15.
Comparison of Z2-Z15 coefficients of the X and Y polarizations phase difference distribution
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