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Accurate atmospheric wind field measurements are critical for understanding global climate dynamics and facilitating space exploration. Doppler asymmetric spatial heterodyne interferometer (DASH) is used to measure atmospheric wind speed through detecting the phase changes in interferograms induced by Doppler shifts of airglow emission lines. However, environmental temperature fluctuations and mechanical vibrations often cause imaging plane to shift, thereby introducing phase deviations, and degrading the measurement accuracy. In this study, a novel method of monitoring global fitting-based imaging shift is proposed. By etching periodic notches on the diffraction grating surface, the method models and fits the notch patterns formed on the detector plane to achieve precise imaging shift detection and correction. The optimization of notch signal modeling significantly reduces the number of fitting parameters, thus improving computational efficiency and detection precision. Through extensive simulations, the influences of signal-to-noise ratio (SNR) and model parameter variation on detection accuracy are analyzed. The results indicate that when the SNR exceeds 11, the detection uncertainty is still below 6.5 nm. Sensitivity analysis reveals that the detection error stays within acceptable limits when the variations of notch number and notch width are controlled within 40% and 0.7%, respectively, while the influence of edge smoothness parameter of notch pattern is negligible. To validate the performance of the method, the thermal stability is tested by using a near-infrared DASH prototype. The experimental results demonstrate a strong correlation between interferogram phase shifts, imaging plane shifts, and environmental temperature variations. After applying the proposed correction method, local phase fluctuations in the interferogram are significantly reduced, thus the phase stability is improved. Further, artificially applied imaging shifts are accurately detected with errors consistently below 9.96 nm, thereby confirming the reliability and precision of this method. All in all, the proposed method effectively detects and corrects the imaging plane shifts caused by temperature variations, enhancing interferogram phase stability and ensuring high-precision wind speed measurements. This method provides a robust and computationally efficient solution for reducing imaging shifts in DASH systems, and has great potential applications in atmospheric wind field measurement and space-based observation.
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Keywords:
- atmospheric wind field measurement /
- Doppler asymmetric spatial heterodyne interferometer /
- image plane shift /
- global fitting
[1] Shepherd G G 2015 Acta Astronaut. 115 206
Google Scholar
[2] Dhadly M, Sassi F, Emmert J, Drob D, Conde M, Wu Q, Makela J, Budzien S Nicholas A 2023 Astron. Space Sci. 9 1050586
Google Scholar
[3] 唐远河, 崔进, 郜海阳, 屈欧阳, 段晓东, 李存霞, 刘丽娜 2017 物理学报 66 130601
Google Scholar
Tang Y H, Cui J, Gao H Y, Qu O Y, Duan X D, Li C X, Liu L N 2017 Acta Phys. Sin. 66 130601
Google Scholar
[4] 冯玉涛, 傅頔, 赵增亮, 宗位国, 余涛, 盛峥, 朱亚军 2023 光学学报 43 0601011
Feng Y T, Fu D, Zhao Z L, Zong W G, Yu T, Sheng Z, Zhu Y J 2023 Acta Opt. Sin. 43 0601011
[5] Zhang S P, Thayer J P, Roble R G 2004 J. Atmos Sol-terr. Phys. 66 105
Google Scholar
[6] Englert C R, Harlander J M, Babcock D D, Stevens M H, Siskind D E 2006 Proc. SPIE 6303 63030T
Google Scholar
[7] Englert C R, Babcock D D, Harlander J M 2006 Appl. Opt. 46 7297
[8] Harlander J M, Englert C R, Emmert J T, Babcock D D, Roesler F 2010 Opt. Express 18 26430
Google Scholar
[9] 肖旸, 冯玉涛, 文镇清 2022 光子学报 51 16
Xiao Y, Feng Y T, Wen Z Q 2022 Acta Photon. Sin. 51 16
[10] Harding B J, Chau J L, He M, Englert C R, Harlander J M, Marr K D, Makela J J, Clahsen M, Li G, Ratnam M V, Rao S V B, Wu Y J J, England S L, Immel T J 2021 J. Geophys. Res. Space Phys. 126 e2020JA028947
Google Scholar
[11] Englert C R, Harlander J M, Brown C M, Makela J J, Marr K D, Immel T J In Fourier Transform Spectroscopy Lake Arrowhead, California, United States, March 1–4, 2015 pFM4A-1
[12] Stevens M H, Englert C R, Harlander J M, England S L, Marr K D, Brown C M, Immel T J 2018 Space Sci. Rev. 214 4
Google Scholar
[13] Harlander J M, Englert C R, Brown C M, Marr K D, Miller I J, Zastera V, Bach B W, Mende S B 2017 Space Sci. Rev. 212 601
Google Scholar
[14] Englert C R, Brown C M, Bach B, Bach E, Bach K, Harlander J M, Seely J F, Marr K D, Miller I 2017 Appl. Opt. 56 2090
Google Scholar
[15] Marr K D, Thayer A S, Englert C R, Harlander J M 2020 Opt. Eng. 59 013102
[16] Englert C R, Harlander J M, Marr K D, Harding B J, Makela J J, Fae T, Brown C M, Venkat Ratnam M, Vijaya Bhaskara Rao S , Immel T J 2023 Space Sci. Rev. 219 27
[17] 张亚飞, 冯玉涛, 傅頔, 畅晨光, 李娟, 白清兰, 胡炳樑 2022 物理学报 71 084201
Google Scholar
Zhang Y F, Feng Y T, Fu D, Chang C G, Li J, Bai Q L, Hu B L 2022 Acta Phys. Sin. 71 084201
Google Scholar
[18] Zhang Y F, Feng Y T, Fu D, Wang P C, Sun J, Bai Q L 2020 Chin. Phys. B 29 104204
Google Scholar
[19] 傅頔, 畅晨光, 孙剑, 李娟, 武魁军, 冯玉涛, 刘学斌 2022 光学学报 42 18
Fu D, Chang C G, Sun J, Li J, Wu K J, Feng Y T, Liu X B 2022 Acta Opt. Sin. 42 18
[20] Wei D K, Zhu Y J, Liu J L, Gong Q C, Kaufmann M, Olschewski F, Knieling P, Xu J Y, Koppmann R, Riese M 2020 Opt Express 28 19887
Google Scholar
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图 1 DASH原理图, 右下角为干涉图(顶部为刻槽图像)
Figure 1. Schematic of a DASH interferometer. The interferogram is located at the lower right (The top area is notch pattern).
图 2 (a)梳状函数; (b)梳状函数卷积矩形函数后的方波函数; (c)方波函数卷积高斯核后的刻槽形状
Figure 2. (a) The comb function; (b) the square wave function after the comb function convolved with the rectangle function; (c) the notch signal after the square wave function convolved with Gaussian kernel.
图 3 实测刻槽信号及模拟刻槽信号
Figure 3. Measured notch signal and simulated notch signal.
图 4 检测漂移量及检测误差
Figure 4. Measured imaging shift and measurement error.
图 5 不同信噪比、不同成像漂移量下的成像漂移检测不确定度
Figure 5. Uncertainty of imaging shift measurement under different SNR and different imaging shift.
图 6 SNR = 100时, 高斯函数标准差σ的拟合误差对测量精度的影响
Figure 6. Influence of fitting error of standard deviation σ of Gaussian function on measurement accuracy when SNR = 100
图 7 SNR = 100下, 矩形函数宽度Wnotches的拟合误差对测量精度的影响
Figure 7. Influence of fitting error of rectangle function width Wnotches on measurement accuracy when SNR = 100.
图 8 SNR = 100下, 脉冲数目Nnotches的拟合误差对测量精度的影响
Figure 8. Influence of fitting of pulse number Nnotches on measurement accuracy when SNR = 100.
图 9 近红外多普勒差分干涉仪样机示意图
Figure 9. Schematic diagram of the near infrared DASH prototype.
图 10 (a)实验中所测刻槽图像的成像漂移量(蓝色虚线), 对所测图像人为给定成像漂移量后对应的检测结果(绿色实线); (b)对实验中所测每一帧刻槽图像叠加固定的成像漂移量
Figure 10. (a) The imaging shift of the notch image measured in the experiment (blue dashed line), and the corresponding detection result of the notch image measured in the experiment after artificially superimposing the imaging shift amount (green solid line); (b) the fixed imaging shift is superimposed on each frame of notch image measured in the experiment.
图 11 蓝线为图10(a)中两信号的差值, 即对人为给定漂移量的检测值, 红线为检测误差, 即检测成像漂移量与人为给定成像漂移量间的差值
Figure 11. The blue line is the difference between the two signals in Fig.10 (a), that is, the measurement of the artificially given amount of shift. The red line is the measurement error, that is, the difference between the measured image shift and the input image shift.
图 12 近红外多普勒差分干涉仪样机的连续热稳定性测试数据, 灰色线为温度数据, 蓝色虚线为干涉条纹相位, 绿色线为成像漂移引起的相位变化, 蓝色实线为成像漂移校正后的干涉条纹相位
Figure 12. Thermal stability test data of the near infrared DASH prototype, the gray line is temperature data, the blue dashed line is fringe phase, the green line is phase change caused by imaging shift, and the blue solid line is fringe phase after imaging shift correction.
表 1 仿真参数
Table 1. Simulation parameters.
参数 数值 系统参数 波长/nm 867.16 光程差/mm 49.87 光栅参数 Littrow 波数/nm 868.24 光栅阶数 1 光栅闪耀角/(°) 10 光栅衍射效率 70% 探测器参数 像元数 2048×2048 量子效率 0.75 像元尺寸/μm 6.5 刻槽信号参数 刻槽数量 111.81 刻槽宽度/μm 59.52 
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[1] Shepherd G G 2015 Acta Astronaut. 115 206
Google Scholar
[2] Dhadly M, Sassi F, Emmert J, Drob D, Conde M, Wu Q, Makela J, Budzien S Nicholas A 2023 Astron. Space Sci. 9 1050586
Google Scholar
[3] 唐远河, 崔进, 郜海阳, 屈欧阳, 段晓东, 李存霞, 刘丽娜 2017 物理学报 66 130601
Google Scholar
Tang Y H, Cui J, Gao H Y, Qu O Y, Duan X D, Li C X, Liu L N 2017 Acta Phys. Sin. 66 130601
Google Scholar
[4] 冯玉涛, 傅頔, 赵增亮, 宗位国, 余涛, 盛峥, 朱亚军 2023 光学学报 43 0601011
Feng Y T, Fu D, Zhao Z L, Zong W G, Yu T, Sheng Z, Zhu Y J 2023 Acta Opt. Sin. 43 0601011
[5] Zhang S P, Thayer J P, Roble R G 2004 J. Atmos Sol-terr. Phys. 66 105
Google Scholar
[6] Englert C R, Harlander J M, Babcock D D, Stevens M H, Siskind D E 2006 Proc. SPIE 6303 63030T
Google Scholar
[7] Englert C R, Babcock D D, Harlander J M 2006 Appl. Opt. 46 7297
[8] Harlander J M, Englert C R, Emmert J T, Babcock D D, Roesler F 2010 Opt. Express 18 26430
Google Scholar
[9] 肖旸, 冯玉涛, 文镇清 2022 光子学报 51 16
Xiao Y, Feng Y T, Wen Z Q 2022 Acta Photon. Sin. 51 16
[10] Harding B J, Chau J L, He M, Englert C R, Harlander J M, Marr K D, Makela J J, Clahsen M, Li G, Ratnam M V, Rao S V B, Wu Y J J, England S L, Immel T J 2021 J. Geophys. Res. Space Phys. 126 e2020JA028947
Google Scholar
[11] Englert C R, Harlander J M, Brown C M, Makela J J, Marr K D, Immel T J In Fourier Transform Spectroscopy Lake Arrowhead, California, United States, March 1–4, 2015 pFM4A-1
[12] Stevens M H, Englert C R, Harlander J M, England S L, Marr K D, Brown C M, Immel T J 2018 Space Sci. Rev. 214 4
Google Scholar
[13] Harlander J M, Englert C R, Brown C M, Marr K D, Miller I J, Zastera V, Bach B W, Mende S B 2017 Space Sci. Rev. 212 601
Google Scholar
[14] Englert C R, Brown C M, Bach B, Bach E, Bach K, Harlander J M, Seely J F, Marr K D, Miller I 2017 Appl. Opt. 56 2090
Google Scholar
[15] Marr K D, Thayer A S, Englert C R, Harlander J M 2020 Opt. Eng. 59 013102
[16] Englert C R, Harlander J M, Marr K D, Harding B J, Makela J J, Fae T, Brown C M, Venkat Ratnam M, Vijaya Bhaskara Rao S , Immel T J 2023 Space Sci. Rev. 219 27
[17] 张亚飞, 冯玉涛, 傅頔, 畅晨光, 李娟, 白清兰, 胡炳樑 2022 物理学报 71 084201
Google Scholar
Zhang Y F, Feng Y T, Fu D, Chang C G, Li J, Bai Q L, Hu B L 2022 Acta Phys. Sin. 71 084201
Google Scholar
[18] Zhang Y F, Feng Y T, Fu D, Wang P C, Sun J, Bai Q L 2020 Chin. Phys. B 29 104204
Google Scholar
[19] 傅頔, 畅晨光, 孙剑, 李娟, 武魁军, 冯玉涛, 刘学斌 2022 光学学报 42 18
Fu D, Chang C G, Sun J, Li J, Wu K J, Feng Y T, Liu X B 2022 Acta Opt. Sin. 42 18
[20] Wei D K, Zhu Y J, Liu J L, Gong Q C, Kaufmann M, Olschewski F, Knieling P, Xu J Y, Koppmann R, Riese M 2020 Opt Express 28 19887
Google Scholar
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