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Three-dimensional (3D) wavefront sensing of atmosphere turbulence is a key step to realize multi-conjugate adaptive optics technology. In this article, model tomography, which is one of the most important algorithms for 3D wavefront sensing, is analyzed in theory, the principle limitation of model tomography is proposed. Based on this view the reason for tomography error is discussed, and the simulation results for different errors are produced finally. The analysis shows that part Zernike model basis is used as a new basis of polynomial decomposition in model tomography, which leads to modal coupling error and aliasing error. The un-correlation of part Zernike model basis is the prerequisite to avoid modal aliasing error, but modal coupling error cannot be removed and we can only restrain its influence. Combined with simulation result a method with large field of view (FOV) sensing and small FOV reconstruction is proposed and gives a good performance to control modal coupling error.
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Keywords:
- 3D wavefront sensing /
- atmosphere tomography /
- modal method /
- error analysis
[1] Beckers J M 1988 In ESO Conference on Very Large Telescopes and Their Implementation European Southern Observatory Garching, Germany, March 21-24, 1988 p693
[2] Beckers J M 1989 Proc. SPIE 1114 215
[3] Tallom M, Foy R 1990 Astron. Astrophys. 235 549
[4] Ragazzoni R, Marchetti E, Rigaut F 1999 Astron. Astrophys. 342 L53
[5] Ragazzoni R, Marchetti E, Valente G 2000 Nature 403 54
[6] Fusco T, Conan J M, Michau V, Rousset G, Assemat F 2001 Proc. SPIE 4167 168
[7] Tokovinin A, Louarn M L, Viard E, Hubin N, Conan R 2001 Astron. Astrophys. 378 710
[8] Tokovinin A, Viard E 2001 J. Opt. Soc. Am. A 18 873
[9] Li C H, Xian H, Jiang W H, Rao C H 2007 Acta Phys. Sin. 56 4289 (in Chinese) [李超宏, 鲜浩, 姜文汉, 饶长辉 2007 物理学报 56 4289]
[10] Fusco T, Conan J M, Rousset M, Mugnier L M, Michau V 2001 J. Opt. Soc. Am. A 18 2527
[11] Yang H F, Jiang Z F 2005 Laser Technol. 29 484 (in Chinese) [杨华峰, 姜宗福 2005 激光技术 29 484]
[12] Duan H F, Li E D, Wang H Y, Yang Z P, Zhang Y D 2003 Acta Opt. Sin. 23 1143 (in Chinese) [段海峰, 李恩得, 王海英, 杨泽平, 张雨东 2003 光学学报 23 1143]
[13] Roddier N 1990 Opt. Eng. 29 1174
[14] Zhang L Q, Rao C H 2012 Proc. SPIE 8415 84150W
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[1] Beckers J M 1988 In ESO Conference on Very Large Telescopes and Their Implementation European Southern Observatory Garching, Germany, March 21-24, 1988 p693
[2] Beckers J M 1989 Proc. SPIE 1114 215
[3] Tallom M, Foy R 1990 Astron. Astrophys. 235 549
[4] Ragazzoni R, Marchetti E, Rigaut F 1999 Astron. Astrophys. 342 L53
[5] Ragazzoni R, Marchetti E, Valente G 2000 Nature 403 54
[6] Fusco T, Conan J M, Michau V, Rousset G, Assemat F 2001 Proc. SPIE 4167 168
[7] Tokovinin A, Louarn M L, Viard E, Hubin N, Conan R 2001 Astron. Astrophys. 378 710
[8] Tokovinin A, Viard E 2001 J. Opt. Soc. Am. A 18 873
[9] Li C H, Xian H, Jiang W H, Rao C H 2007 Acta Phys. Sin. 56 4289 (in Chinese) [李超宏, 鲜浩, 姜文汉, 饶长辉 2007 物理学报 56 4289]
[10] Fusco T, Conan J M, Rousset M, Mugnier L M, Michau V 2001 J. Opt. Soc. Am. A 18 2527
[11] Yang H F, Jiang Z F 2005 Laser Technol. 29 484 (in Chinese) [杨华峰, 姜宗福 2005 激光技术 29 484]
[12] Duan H F, Li E D, Wang H Y, Yang Z P, Zhang Y D 2003 Acta Opt. Sin. 23 1143 (in Chinese) [段海峰, 李恩得, 王海英, 杨泽平, 张雨东 2003 光学学报 23 1143]
[13] Roddier N 1990 Opt. Eng. 29 1174
[14] Zhang L Q, Rao C H 2012 Proc. SPIE 8415 84150W
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