Catadioptric Optical System Design of 15-Magnitude Star Sensor with Large Entrance Pupil Diameter

Bai, Yang; Li, Jianlin; Zha, Rongwei; Wang, Ying; Lei, Guangzhi

doi:10.3390/s20195501

Cited by 6 publications

(6 citation statements)

References 27 publications

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“…As shown in equation ( 9), the limit magnitude at the tangent height h a is m l_ha by solving equation ( 8). The limit magnitude at the tangent height h b is m l_hb shown in equation (10). So, the limit magnitude difference at different tangent heights can be calculated according to equation (11).…”

Section: Fov and Limit Magnitudementioning

confidence: 99%

“…Tolerance analysis is one of the most important steps in optical design. Table 7 shows the tolerances for the designed optical system, which is obtained from a large catadioptric optical system [10,30]. Tolerance analysis is performed by the ZEMAX software with two methods, including sensitivity analysis and Monte Carlo analysis.…”

Section: Image Qualitymentioning

confidence: 99%

“…This star sensor had a 57.5% probability of observing refracted stars at night. In 2020, Bai et al [10] designed a visible catadioptric star sensor for the satellite with an aperture of 285 mm for lenses, an FOV of 2.8°, and an aperture of 257 mm for mirrors. Because the strong limb background during the day is ignored, the existing star sensors [7][8][9][10] were unable to detect enough refracted stars during the day.…”

Section: Introductionmentioning

confidence: 99%

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Optical system design method of the all-day starlight refraction navigation system

Wu,

Wang,

Yan

2023

J. Eur. Opt. Society-Rapid Publ.

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The application of starlight refraction navigation to spacecraft and space weapons is a significant development direction. Observing enough refracted stars for the star sensor in a strong limb background is an urgent problem. The all-day optical system parameters are analyzed based on the star detection requirement and navigation accuracy. Combined with primary aberration theory, the prime-focus catadioptric optical system is selected to meet the design requirements of a wide field of view (FOV) and tight structure. An H-band (1.52um-1.78um) star sensor is designed with a FOV of 6°, a focal length of 831mm, an effective aperture of 253mm, and a relative distortion of 0.03%. The energy concentration of the star point is 85% within 30um, and the maximum lateral chromatic aberration is 2.9um, which meets the imaging requirements. Furthermore, a baffle is designed to avoid the influence of direct sunlight on stellar imaging. The proposed method can provide a theoretical foundation and technical support for the optical design of the refraction star navigation.

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Section: Fov and Limit Magnitudementioning

confidence: 99%

Section: Image Qualitymentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Optical system design method of the all-day starlight refraction navigation system

Wu,

Wang,

Yan

2023

J. Eur. Opt. Society-Rapid Publ.

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“…According to the imaging model shown in Equation (1), the larger the focal length f, the smaller the impact of the deviation of the imaging position (x i ,y i ) on the position vector w i , resulting in higher precision in spacecraft attitude determination. As shown in Figure 3, for conventional optical system of star sensors, the relationship between the half angle ωmax of FOV and the focal length f is as follows [24]:…”

Section: Principlesmentioning

confidence: 99%

An Optical System of Star Sensors with Accuracy Performance Varying with the Field of View

Wang,

Chen,

et al. 2023

Sensors

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The field of view and single-star measurement accuracy are crucial metrics for assessing the performance of a star sensor. The field of view determines the spatial range of stars that can be captured by the sensor, while the single-star measurement accuracy determines the precision of attitude determination and control for the star sensor. The optical system of conventional star sensors is constrained by imaging relationships. Once the detector is determined, improving either the field of view or the single-star measurement accuracy will result in the degradation of the other. To address this issue, we propose an optical system for star sensors with accuracy performance varying with the field of view. By controlling the relationship between the field focal length of the optical system and the field of view, it is possible to simultaneously enhance both the field of view and the single-star measurement accuracy. We have designed corresponding optical systems to address the requirements for improving the single-star measurement accuracy and field of view. The design results confirm the feasibility of this star sensor. The star sensors are capable of simultaneously meeting the requirements for star pattern recognition and attitude determination, presenting broad application prospects in fields such as space navigation.

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“…MTF (modulus of the OTF) is employed in this paper to assess the optical performance of the camera after the Zernike coefficients of the deformed surface are directly imported into the ray-tracing software Zemax [ 25 ]. The MTF values described below are the average value in the tangential and sagittal planes [ 26 , 27 , 28 ]. The image size of the visible light detector is 1920 × 1080 and the pixel size is 5.5 um corresponding to the cutoff frequency of MTF is about 90 cycles per mm.…”

Section: Optimal Design Of the Primary Mirror Assemblymentioning

confidence: 99%

Design and Optimization for Mounting Primary Mirror with Reduced Sensitivity to Temperature Change in an Aerial Optoelectronic Sensor

Zhang

Qi-peng

Tian

et al. 2021

Sensors

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In order to improve the image quality of the aerial optoelectronic sensor over a wide range of temperature changes, high thermal adaptability of the primary mirror as the critical components is considered. Integrated optomechanical analysis and optimization for mounting primary mirrors are carried out. The mirror surface shape error caused by uniform temperature decrease was treated as the objective function, and the fundamental frequency of the mirror assembly and the surface shape error caused by gravity parallel or vertical to the optical axis are taken as the constraints. A detailed size optimization is conducted to optimize its dimension parameters. Sensitivities of the optical system performance with respect to the size parameters are further evaluated. The configuration of the primary mirror and the flexure are obtained. The simulated optimization results show that the size parameters differently affect the optical performance and which factors are the key. The mirror surface shape error under 30 °C uniform temperature decrease effectively decreased from 26.5 nm to 11.6 nm, despite the weight of the primary mirror assembly increases by 0.3 kg. Compared to the initial design, the value of the system’s modulation transfer function (0° field angle) is improved from 0.15 to 0.21. Namely, the optical performance of the camera under thermal load has been enhanced and thermal adaptability of the primary mirror has been obviously reinforced after optimization. Based on the optimized results, a prototype of the primary mirror assembly is manufactured and assembled. A ground thermal test was conducted to verify difference in imaging quality at room and low temperature, respectively. The image quality of the camera meets the requirements of the index despite degrading.

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Catadioptric Optical System Design of 15-Magnitude Star Sensor with Large Entrance Pupil Diameter

Cited by 6 publications

References 27 publications

Optical system design method of the all-day starlight refraction navigation system

Optical system design method of the all-day starlight refraction navigation system

An Optical System of Star Sensors with Accuracy Performance Varying with the Field of View

Design and Optimization for Mounting Primary Mirror with Reduced Sensitivity to Temperature Change in an Aerial Optoelectronic Sensor

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