基于幸运成像的衍射极限天文成像技术研究
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摘要
由于大气湍流的影响,以及各国深空探测脚步的加快,地基光学望远镜获得衍射极限图像的技术受到国内外天文研究人员的高度重视。幸运成像技术是通过对目标序列短曝光图像数据进行获取、像质评价、图像帧选取、图像配准与叠加、图像增强几个步骤,最终得到一幅清晰度显著提高、视觉效果大大改善的图像。该方法能够有效降低了噪声和大气湍流导致的图像模糊,提高非等晕条件下地基天文望远镜的成像分辨率。本文首先介绍了幸运成像技术的相关基础理论,阐述了大气湍流的特性和非等晕条件下幸运短曝光图像出现的概率,以及EMCCD的相关性能指标,从而为幸运成像技术的研究提供理论基础；然后介绍了幸运成像技术的数据处理流程,讨论了该处理方法的关键技术和需要研究的几个主要问题,并给出了相应的解决方法；最后应用该项技术,设计进行了双星观测成像的实验,并对实验数据进行了事后处理。通过分析处理结果表明,幸运成像技术能够提高目标通过湍流大气的成像分辨率,此项研究为幸运成像技术在深空探测中广泛应用打下了基础。
With the effects of the atmospheric turbulence and the faster steps of the deep-space exploration, obtaining diffraction limited images of astronomical optical telescope becomes more and more fashionable. Lucy imaging technology appeared under this background. Lucy imaging technology finally gains a image that is clearer, more comfortable for vision, passing through the following steps—image acquisition, image quality evaluation, frame selection, image match and adding, image enhancement. This technique has a few advantages:not only effectively reducing the noise and image penumbra arosed by the atmosphere, but also improve the image resolution of ground-based telescope. This thesis introduces a series of problems. Firstly, some basic theory related to the Lucy imaging. Secondly, the data processing flow chart of Lucy imaging. Third, key problems and the corresponding resolution are showed. At last, explain the whole process of binary stars observing, and the significative analysis. Lucy imaging technology has laid a basis for further extending objects in the field of deep-space and other fields.
With the effects of the atmospheric turbulence and the faster steps of the deep-space exploration, obtaining diffraction limited images of astronomical optical telescope becomes more and more fashionable. Lucy imaging technology appeared under this background. Lucy imaging technology finally gains a image that is clearer, more comfortable for vision, passing through the following steps—image acquisition, image quality evaluation, frame selection, image match and adding, image enhancement. This technique has a few advantages:not only effectively reducing the noise and image penumbra arosed by the atmosphere, but also improve the image resolution of ground-based telescope. This thesis introduces a series of problems. Firstly, some basic theory related to the Lucy imaging. Secondly, the data processing flow chart of Lucy imaging. Third, key problems and the corresponding resolution are showed. At last, explain the whole process of binary stars observing, and the significative analysis. Lucy imaging technology has laid a basis for further extending objects in the field of deep-space and other fields.
引文
[1]Law N M 2006 Lucky Imaging:Diffraction-Limited Astronomy from the Ground in the Visible Ph.D. thesis,Cambridge University.
[2]周丹,近地面大气湍流特性的研究,硕十论文,2002
[3]Tubbs R N 2003 Lucky Exposures:Diffraction Limited Astronomical Imaging Through the Atmosphere Ph.D.thesis, Cambridge University.
[4]刘忠,天文图像高分辨重建及空域性质研究,博十论文,2003
[5]王淑平.大口径望远镜专题文集.中科院长春光机所,1998
[6]Law, N. M.,"Lucky imaging:diffraction-limited astronomy from the ground in the visible." The Observatory 127, 71-71 (Feb.2007).
[7]周昶宁等,自适应光学系统中大气湍流的模型分析与计算机仿真,光学技术,2005.2：249-251
[8]严谊健,符养,洪振杰.现代大气折射引论.上海科技教育出版社,2006
[9]苏定强-2.16米天文望远镜工程文集.中国科学技术出版社,2000
[10]程景全.天文望远镜原理和设计.中国科学技术出版社,2003
[11]Baldwin, J. E., Warner, P. J., and Mackay. C. D., "The point spread function in Lucky Imaging and variations in seeing on short timescales." A&A 480,589-597 (Mar.2008).
[12]刘忠,邱耀辉,大气像质衰减参数,云南天文台台刊,1997.3：75-81
[13]Troy,M., Dekany, R. G., Brack, G., Oppenheimer, B. R., Bloemhof, E. E., Trinh, T., Dekens, F. G., Shi, F., Hayward, T. L., and Brandl. B.. "Palomar adaptive optics project:status and performance." in [Proc. SPIE Vol.4007, p. 31-40,Adaptive Optical Systems Technology, Peter L. Wizinowich; Ed.], Wizinowich, P. L., ed., Presented at the Society of Photo-Optical Instrumentation Engineers (SPIE) Conference 4007,31-40 (July 2000).
[14]Dekany. R. G.. Brack, G., Palmer. D.. Oppenheimer, B. R., Hayward. T. L.. and Brandl, B.. "First tip-tilt correction with the Palomar 200-in. adaptive optics system," in [Proc. SPIE Vol.3353. p.56-59, Adaptive Optical System Technologies, Domenico Bonaccini; Robert K. Tyson; Eds.], Bonaccini, D. and Tyson, R. K., eds., Presented at the Society of Photo-Optical Instrumentation Engineers (SPIE) Conference 3353,56-59 (Sept.1998).
[15]Mackay. C. D., Baldwin. J., Law. N.. andWarner. P., "High-resolution imaging in the visible from the ground without adaptive optics:new techniques and results," in [Proceedings of the SPIE, Volume 5492, pp.128-135 (2004).], 128-135 (Sept.2004).
[16]Racine. R.. Salmon. D.. Cowley,D., and Sovka. J., "Mirror, dome, and natural seeing at CFHT." PASP 103. 1020-1032 (Sept.1991).
[17]Gladysz, S., Christou, J. C., Bradford, L. W., and Roberts. Jr, L. C., "Temporal variability and statistics of the Strehl ratio in adaptive-optics images," ArXiv e-prints 801 (Jan.2008).
[18]Law. N. M.. Mackay. C. D.. and Baldwin,J. E.. "Lucky imaging:high angular resolution imaging in the visible from the ground." A&A 446,739-745 (Feb.2006).
[19](美)古德曼,曹其智,陈家璧.光学中的散斑现象：理论与应用.科学出版社,2009
[20](美)约德,周海宪,程云芳.光机系统设计.机械工业出版社,2008
[21]Law, N. M., Mackay, C. D., Dekany, R. G, Ireland, M., Lloyd, J. P., Moore, A. M., Robertson, J. G., Tuthill, P., and Woodruff. H., "Getting Lucky with Adaptive Optics:Fast AO Image Selection in the Visible with a Large Telescope," ArXiv e-prints, submitted to ApJ 805 (May 2008).
[22]Coude du Foresto, V., Faucherre.M.. Hubin. N.. and Gitton, P.. "Using single-mode fibers to monitor fast Strehl ratio fluctuations. Application to a 3.6 m telescope corrected by adaptive optics." AAPS 145.305-310 (Aug.2000).
[23]冒蔚,季凯帆,CCD天体测量学,第1版,云南科技出版社,2003
[24]杨志文.光学测量.北京理工大学出版社,1995
[25]张广军.视觉测量.科学出版社,2008
[26]Mackay, C., Basden, A., and Bridgeland.M.. "Astronomical imaging with L3CCDs:detector performance and highspeed controller design," in [Proceedings of the SPIE. Volume 5499. pp.203-209 (2004).],203-209 (Sept.2004).
[27]章毓晋, 图象处理和分析,清华大学出版社
[28]李象霖.数字图像处理.中国科学院研究生院教材,2004
[29]王庆有.图像传感器应用技术.电子工业出版社,2003
[30]罗林等,空间扩展目标对准误差图像的高分辨复原,红外与毫米波学报,2007.5：372-376
[31]于万波.基于Matlab的图像处理.清华大学出版社,2008
[32]Fruchter, A. S. and Hook, R. N., "Drizzle:A Method for the Linear Reconstruction of Undersampled Images," PASP 114,144-152 (Feb.2002).
[33]邱耀辉,刘忠,楼柯等。斑点全息术天文高分辨像复原实验闭光学学报,1999,19(2)：151154.
[34]卢汝为,王峰,娄柯等,云南天文台新型斑点像探测系统云南天文台刊,1998,总72期(1)：5964
[2]周丹,近地面大气湍流特性的研究,硕十论文,2002
[3]Tubbs R N 2003 Lucky Exposures:Diffraction Limited Astronomical Imaging Through the Atmosphere Ph.D.thesis, Cambridge University.
[4]刘忠,天文图像高分辨重建及空域性质研究,博十论文,2003
[5]王淑平.大口径望远镜专题文集.中科院长春光机所,1998
[6]Law, N. M.,"Lucky imaging:diffraction-limited astronomy from the ground in the visible." The Observatory 127, 71-71 (Feb.2007).
[7]周昶宁等,自适应光学系统中大气湍流的模型分析与计算机仿真,光学技术,2005.2：249-251
[8]严谊健,符养,洪振杰.现代大气折射引论.上海科技教育出版社,2006
[9]苏定强-2.16米天文望远镜工程文集.中国科学技术出版社,2000
[10]程景全.天文望远镜原理和设计.中国科学技术出版社,2003
[11]Baldwin, J. E., Warner, P. J., and Mackay. C. D., "The point spread function in Lucky Imaging and variations in seeing on short timescales." A&A 480,589-597 (Mar.2008).
[12]刘忠,邱耀辉,大气像质衰减参数,云南天文台台刊,1997.3：75-81
[13]Troy,M., Dekany, R. G., Brack, G., Oppenheimer, B. R., Bloemhof, E. E., Trinh, T., Dekens, F. G., Shi, F., Hayward, T. L., and Brandl. B.. "Palomar adaptive optics project:status and performance." in [Proc. SPIE Vol.4007, p. 31-40,Adaptive Optical Systems Technology, Peter L. Wizinowich; Ed.], Wizinowich, P. L., ed., Presented at the Society of Photo-Optical Instrumentation Engineers (SPIE) Conference 4007,31-40 (July 2000).
[14]Dekany. R. G.. Brack, G., Palmer. D.. Oppenheimer, B. R., Hayward. T. L.. and Brandl, B.. "First tip-tilt correction with the Palomar 200-in. adaptive optics system," in [Proc. SPIE Vol.3353. p.56-59, Adaptive Optical System Technologies, Domenico Bonaccini; Robert K. Tyson; Eds.], Bonaccini, D. and Tyson, R. K., eds., Presented at the Society of Photo-Optical Instrumentation Engineers (SPIE) Conference 3353,56-59 (Sept.1998).
[15]Mackay. C. D., Baldwin. J., Law. N.. andWarner. P., "High-resolution imaging in the visible from the ground without adaptive optics:new techniques and results," in [Proceedings of the SPIE, Volume 5492, pp.128-135 (2004).], 128-135 (Sept.2004).
[16]Racine. R.. Salmon. D.. Cowley,D., and Sovka. J., "Mirror, dome, and natural seeing at CFHT." PASP 103. 1020-1032 (Sept.1991).
[17]Gladysz, S., Christou, J. C., Bradford, L. W., and Roberts. Jr, L. C., "Temporal variability and statistics of the Strehl ratio in adaptive-optics images," ArXiv e-prints 801 (Jan.2008).
[18]Law. N. M.. Mackay. C. D.. and Baldwin,J. E.. "Lucky imaging:high angular resolution imaging in the visible from the ground." A&A 446,739-745 (Feb.2006).
[19](美)古德曼,曹其智,陈家璧.光学中的散斑现象：理论与应用.科学出版社,2009
[20](美)约德,周海宪,程云芳.光机系统设计.机械工业出版社,2008
[21]Law, N. M., Mackay, C. D., Dekany, R. G, Ireland, M., Lloyd, J. P., Moore, A. M., Robertson, J. G., Tuthill, P., and Woodruff. H., "Getting Lucky with Adaptive Optics:Fast AO Image Selection in the Visible with a Large Telescope," ArXiv e-prints, submitted to ApJ 805 (May 2008).
[22]Coude du Foresto, V., Faucherre.M.. Hubin. N.. and Gitton, P.. "Using single-mode fibers to monitor fast Strehl ratio fluctuations. Application to a 3.6 m telescope corrected by adaptive optics." AAPS 145.305-310 (Aug.2000).
[23]冒蔚,季凯帆,CCD天体测量学,第1版,云南科技出版社,2003
[24]杨志文.光学测量.北京理工大学出版社,1995
[25]张广军.视觉测量.科学出版社,2008
[26]Mackay, C., Basden, A., and Bridgeland.M.. "Astronomical imaging with L3CCDs:detector performance and highspeed controller design," in [Proceedings of the SPIE. Volume 5499. pp.203-209 (2004).],203-209 (Sept.2004).
[27]章毓晋, 图象处理和分析,清华大学出版社
[28]李象霖.数字图像处理.中国科学院研究生院教材,2004
[29]王庆有.图像传感器应用技术.电子工业出版社,2003
[30]罗林等,空间扩展目标对准误差图像的高分辨复原,红外与毫米波学报,2007.5：372-376
[31]于万波.基于Matlab的图像处理.清华大学出版社,2008
[32]Fruchter, A. S. and Hook, R. N., "Drizzle:A Method for the Linear Reconstruction of Undersampled Images," PASP 114,144-152 (Feb.2002).
[33]邱耀辉,刘忠,楼柯等。斑点全息术天文高分辨像复原实验闭光学学报,1999,19(2)：151154.
[34]卢汝为,王峰,娄柯等,云南天文台新型斑点像探测系统云南天文台刊,1998,总72期(1)：5964