Efficiency analysis of polarizing filter enhanced signal to noise ratio for daytime star measurement

doi:10.11947/j.AGCS.2024.20230416

Abstract

Abstract:

Now, astronomical geodesy can only observe the celestial bodies in the visible band at night, and has not yet achieved all-time measurement. Therefore, studying daytime star measurement technology is very meaningful. In order to enhance the signal-to-noise ratio(SNR) of star measurement in daytime, this paper constructs a polarization filtering SNR enhancement model and analyzes the effectiveness of using polarization filtering method for star measurement SNR enhancement. Firstly, the characterization model of atmospheric polarization state is analyzed, and then a polarization filtering model is put forward based on the Rayleigh scattering model. Then, an enhancement model for improving the SNR is derived, and the SNR enhancement efficiency and influencing factors are analyzed. Finally, two outdoor experimental platforms were built to verify the effectiveness of the model. The experimental results show that in the band of 900~1700 nm, the filtering model constructed based on the Rayleigh scattering model has high accuracy, with 77% of the point polarization angle errors being smaller than 5° and 100% smaller than 12°, which can meet the accuracy requirements for the practical polarization filter model. Through observations of 6 stars, including Arcturus and Kochab, it was shown that the SNR of stars with different observation orientations can be improved by 22%~109%, which is consistent with the SNR enhancement model. The use of polarization filtering method for daytime star measurement in the entire sky has important application value. When the maximum polarization degree of the entire sky is 0.65, the average polarization degree can reach 0.34, and the corresponding star measurement SNR can be improved by about 51.5%.

Key words: astronomical geodesy, all-day measurement, daytime star measurement, atmospheric polarization, polarization filtering

CLC Number:

P228.7

Wanxiang GOU, Chonghui LI, Yinhu ZHAN, Yuan YANG, Yong ZHENG. Efficiency analysis of polarizing filter enhanced signal to noise ratio for daytime star measurement[J]. Acta Geodaetica et Cartographica Sinica, 2024, 53(8): 1574-1585.

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References 36

[1]	HIRT C, BURKI B. Status of geodetic astronomy at the beginning of the 21st century[J]. Geodäsie und Geoinformatik der Universität Hannover, 2006, 258: 81-99.
[2]	张超, 詹银虎, 王若璞, 等. 光学天文大地测量技术发展评述[J]. 测绘科学技术学报, 2021, 38(4): 331-336, 342.
	ZHANG Chao, ZHAN Yinhu, WANG Ruopu, et al. Review of the development of optical astro-geodetic technology[J]. Journal of Geomatics Science and Technology, 2021, 38(4): 331-336, 342.
[3]	詹银虎, 张超, 李飞战, 等. 基于图像全站仪的天文大地垂线偏差测量及其精度分析[J]. 测绘学报, 2023, 52(2): 175-182. DOI: 10.11947/j.AGCS.2023.20210486.
	ZHAN Yinhu, ZHANG Chao, LI Feizhan, et al. Astro-geodetic vertical deflection measurement and accuracy analysis based on image total station[J]. Acta Geodaetica et Cartographica Sinica, 2023, 52(2): 175-182. DOI: 10.11947/j.AGCS.2023.20210486.
[4]	张旭, 张超, 詹银虎, 等. 基于星点位置预测的线阵全站仪天文测量异常数据剔除方法[J]. 测绘学报, 2023, 52(4): 571-578. DOI: 10.11947/J.AGCS.2023.20210675.
	ZHANG Xu, ZHANG Chao, ZHAN Yinhu, et al. A method of removing abnormal data from linear array total station astronomical measurement based on star position prediction[J]. Acta Geodaetica et Cartographica Sinica, 2023, 52(4): 571-578. DOI: 10.11947/J.AGCS.2023.20210675.
[5]	刘宇宸, 赵春晖, 徐卿. 基于神经网络的全天时天文导航图像去噪方法[J]. 光学学报, 2019, 39(6): 0610003.
	LIU Yuchen, ZHAO Chunhui, XU Qing. Neural network-based noise suppression algorithm for star images captured during daylight hours[J]. Acta Optica Sinica, 2019, 39(6): 0610003.
[6]	戴东凯, 吴州平, 谭文锋, 等. 基于姿态关联帧叠加的星图信噪比增强方法[J]. 中国惯性技术学报, 2020, 28(1): 82-88.
	DAI Dongkai, WU Zhouping, TAN Wenfeng, et al. An image signal-to-noise ratio enhancement method based on attitude correlated frames adding[J]. Journal of Chinese Inertial Technology, 2020, 28(1): 82-88.
[7]	BARBOT L, FERRARI M, MONTEL J, et al. Towards a daytime and low-altitude stellar positioning system: challenges and first results[C]//Proceedings of 2022 International Technical Meeting of The Institute of Navigation. Long Beach: IEEE, 2022: 1371-1379.
[8]	WANG Wenjie, WEI Xinguo, LI Jian, et al. Optical parameters optimization for all-time star sensor[J]. Sensors (Basel, Switzerland), 2019, 19(13): 2960.
[9]	张凯胜, 苏秀琴, 叶志龙. 大相对孔径全天时星敏感器光学系统[J]. 光子学报, 2022, 51(11): 1111003.
	ZHANG Kaisheng, SU Xiuqin, YE Zhilong. Large relative aperture optical system design for all day star sensor [J]. Acta Photonica Sinica, 2022, 51(11): 1111003.
[10]	张路青. 短波红外白天测星技术研究[J]. 光学与光电技术, 2015, 13(4): 61.
	ZHANG Luqing. Research on SWIR star detection technology in daytime[J]. Optics & Optoelectronic Technology, 2015, 13(4): 61.
[11]	LU Rui, WU Yanpeng. Estimation of stellar instrument magnitudes using synthetic photometry[C]//Proceedings of 2019 IEEE Aerospace Conference. Big Sky: IEEE, 2019: 1-7.
[12]	BUCHOLTZ A. Rayleigh-scattering calculations for the terrestrial atmosphere[J]. Applied Optics, 1995, 34(15): 2765-2773.
[13]	CUI Yan, ZHANG Xiguang, ZHOU Xinchang, et al. Effect of aerosol on polarization distribution of sky light[J]. Acta Optica Sinica, 2019, 39(6): 0601001.
[14]	ESHELMAN L M, SMITH A M, SMITH K M, et al. Unique navigation solution utilizing sky polarization signatures[C]//Proceedings of 2022 Conference on Polarization: Measurement, Analysis, and Remote Sensing XV. Orlando: SPIE, 2022.
[15]	LIU Jun, ZHAO Donghua, WANG Chenguang, et al. Attitude calculation method based on full-sky atmospheric polarization mode[J]. Review of Scientific Instruments, 2019, 90(1): 015009.
[16]	叶松, 方勇华, 孙晓兵, 等. 一种基于偏振信息的恒星白天观测方法[J]. 大气与环境光学学报, 2007, 2(3): 222-226.
	YE Song, FANG Yonghua, SUN Xiaobing, et al. Star observation based on polarization information in daytime[J]. Journal of Atmospheric and Environmental Optics, 2007, 2(3): 222-226.
[17]	LAN Gongpu, MA Wenli, CHENG Feng. Daytime star detection device using polarization and spectral filtering method[C]//Proceedings of the 5th International Symposium on Advanced Optical Manufacturing and Testing Technologies. Dalian: SPIE, 2010.
[18]	REN Jianbin, LIU Jun, TANG Jun, et al. Attitude determination based on location of astronomical markers with skylight polarization pattern[J]. IEEE Sensors Journal, 2015, 15(12): 7312-7320.
[19]	张锐进, 鲜浩, 饶长辉, 等. 偏振滤波白天抑制天光背景作用分析[J]. 光学学报, 2012, 32(5): 0501003.
	ZHANG Ruijin, XIAN Hao, RAO Changhui, et al. Study on effect of polarization filter for suppressing sky background light in daytime[J]. Acta Optica Sinica, 2012, 32(5): 0501003.
[20]	冯斌, 史泽林, 艾锐, 等. 偏振滤波抑制大气背景光的性能计算模型[J]. 光学学报, 2011, 31(4): 0401003.
	FENG Bin, SHI Zelin, AI Rui, et al. A new computational model for performance of airlight rejection utilizing polarization filtering[J]. Acta Optica Sinica, 2011, 31(4): 0401003.
[21]	FU Qiang, ZHAO Feng, CHEN Hongyi, et al. Space object and background polarization models and detectability analysis[J]. Applied Sciences, 2022, 12(21): 10714.
[22]	WANG Bingwen, WANG Hongyuan, YAN Zhiqiang, et al. A daytime sky analytical model of the degree of polarization for JHKs bands[J]. Infrared Physics & Technology, 2021, 119: 103960.
[23]	陶志炜, 戴聪明, 武鹏飞, 等. 星光成像的大气影响研究(Ⅰ)：天空偏振[J]. 光子学报, 2023, 52(5): 0552209.
	TAO Zhiwei, DAI Congming, WU Pengfei, et al. Atmospheric effects of star imaging(Ⅰ): sky polarization[J]. Acta Photonica Sinica, 2023, 52(5): 0552209.
[24]	KONG F, GUO Y, ZHANG J, et al. Review on bio-inspired polarized skylight navigation[J]. Chinese Journal of Aeronautics, 2023, 36(9): 14-37.
[25]	BERRY M V, DENNIS M R, LEE R L. Polarization singularities in the clear sky[J]. New Journal of Physics, 2004, 6: 162.
[26]	HANNAY J H. Polarization of sky light from a canopy atmosphere[J]. New Journal of Physics, 2004, 6: 197.
[27]	SUHAI Bence, HORVÁTH G. How well does the Rayleigh model describe the E-vector distribution of skylight in clear and cloudy conditions? A full-sky polarimetric study[J]. Journal of the Optical Society of America A, Optics, Image Science, and Vision, 2004, 21(9): 1669-1676.
[28]	BOURGES B. Improvement in solar declination computation[J]. Solar Energy, 1985, 35(4): 367-369.
[29]	ESHELMAN L M, SHAW J A. The VIS-SWIR spectrum of skylight polarization[J]. Applied Optics, 2018, 57(27): 7974-7986.
[30]	梁铨廷. 物理光学[M]. 3版. 北京: 电子工业出版社, 2008.
	LIANG Quanting. Physical optics[M]. 3rd ed. Beijing: Publishing House of Electronics Industry, 2008.
[31]	NOVAK G, JARRETT T. Technique for accurate stellar polarimetry using CCD cameras[J]. Applied Optics, 1995, 34(10): 1672-1677.
[32]	张辉, 周向东, 汪新梅, 等. 近地空间全天时星敏感器技术现状及发展综述[J]. 航空学报, 2020, 41(8): 13-25.
	ZHANG Hui, ZHOU Xiangdong, WANG Xinmei, et al. Survey of technology status and development of all-time star sensors in near-earth space[J]. Acta Aeronautica et Astronautica Sinica, 2020, 41(8): 13-25.
[33]	TRUESDALEN A, DINKEL K J, DISCHNER Z J B, et al. DayStar: modeling and test results of a balloon-borne daytime star tracker[C]//Proceedings of 2013 IEEE Aerospace Conference. Big Sky: IEEE, 2013: 1-12.
[34]	韩礼, 蔡洪. 白天大气层内星敏感器观星能力分析[J]. 飞行器测控学报, 2015, 34(3): 291-297.
	HAN Li, CAI Hong. Analysis of stargazing capability of star sensors from the atmosphere in daytime[J]. Journal of Spacecraft TT&C Technology, 2015, 34(3): 291-297.
[35]	胡睿. 大气偏振中性点便携式测量方法研究[D]. 桂林: 桂林电子科技大学, 2020.
	HU Rui. Study on portable measurement method of atmospheric polarization neutral point[D]. Guilin: Guilin University of Electronic Technology, 2020.
[36]	MIYAZAKI D, AMMAR M, KAWAKAMI R, et al. Estimating sunlight polarization using a fish-eye lens[J]. IPSJ Transactions on Computer Vision and Applications, 2009, 1: 288-300.

太阳高度角/(°)	信噪比增强值(SNE)
太阳高度角/(°)	≤30%	30%~60%	60%~90%	90%~120%	120%~150%	150%~180%	≥180%
0	19.6	13.6	8.9	7.7	7.7	8.6	33.9
30	23.9	17.2	16.6	9.8	7.5	6.7	18.3
60	44.6	15.0	9.0	6.6	5.5	5.1	14.2
90	49.6	13.0	8.0	6.1	5.0	4.7	13.5

滤光模型误差Δω/(°)	偏振度p
滤光模型误差Δω/(°)	0.1	0.3	0.5	0.7	0.9
0	11%	43%	100%	233%	900%
10	10%	39%	89%	192%	548%
30	5%	18%	33%	54%	82%
50	－2%	－5%	－8%	－11%	－14%
70	－7%	－19%	－28%	－35%	－41%
90	－9%	－23%	－33%	－41%	－47%

高度角		方位角
高度角		0°	30°	60°	90°	120°	150°	180°	210°	240°	270°	300°	330°
20°	AOP	－32°	－24°	－22°	－25°	20°	14°	22°	31°	47°	70°	－70°	－45°
20°	DOP	0.64	0.38	0.25	0.12	0.04	0.23	0.65	0.60	0.38	0.21	0.21	0.47
40°	AOP	－30°	－17°	5°	23°	－43°	－2°	17°	36°	57°	80°	－73°	－57°
40°	DOP	0.57	0.36	0.22	0.10	0.04	0.17	0.35	0.47	0.40	0.35	0.38	0.47
60°	AOP	－28°	－11°	15°	56°	－57°	－18°	7°	32°	54°	83°	－67°	－50°
60°	DOP	0.46	0.27	0.22	0.09	0.08	0.17	0.36	0.55	0.64	0.57	0.59	0.60
80°	AOP	－22°	2°	39°	64°	－69°	－38°	－7°	21°	55°	81°	－76°	－51°
80°	DOP	0.33	0.25	0.17	0.17	0.16	0.34	0.33	0.38	0.46	0.44	0.43	0.47

高度角		方位角
高度角		0°	30°	60°	90°	120°	150°	180°	210°	240°	270°	300°	330°
20°	AOP	－3°	－3°	－5°	4°	－5°	－3°	0°	1°	1°	－4°	0°	－1°
20°	DOP	－0.01	－0.09	0.08	0.10	0.01	0.03	0.14	－0.04	－0.04	－0.04	－0.05	0.02
40°	AOP	3°	－1°	4°	－10°	－4°	1°	2°	5°	6°	5°	4°	－5°
40°	DOP	－0.06	－0.05	0.06	0.07	0.02	0.03	－0.04	－0.15	－0.22	－0.18	－0.15	－0.15
60°	AOP	3°	－4°	－6°	－4°	11°	8°	4°	5°	3°	8°	12°	4°
60°	DOP	－0.06	－0.08	0.03	－0.01	－0.01	0.01	0.04	0.06	0.03	－0.08	－0.06	－0.02
80°	AOP	3°	－2°	4°	－4°	9°	6°	5°	4°	10°	8°	4°	2°
80°	DOP	－0.06	－0.08	－0.10	－0.06	－0.07	0.08	0.02	0.01	0.03	－0.02	－0.03	0.03

恒星	观测方位(A_S，h_S)	原灰度均值(16 bit)	滤光后灰度均值(16 bit)	曝光时间Δt/ms	曝光延长Δt_p/ms
Arcturus	(81°，22°)	45 686	44 647	15	55
Kochab	(19°，36°)	46 816	40 016	10	40
Antares	(292°，68°)	51 972	53 109	5	12
Rigil Kent	(217°，46°)	41 938	47 438	5	14
Enif	(47°，29°)	42 049	43 752	20	62
Atria	(201°，51°)	43 266	45 507	20	70