The laser guide star concept was proposed for the application of adaptive optics in astronomy in order to overcome the problem of natural star requisite brightness which significantly limits the sky coverage [1, 2]. Recently, the adaptive optics compensation of turbulent wavefront using laser guide star has been demonstrated [3,4].
{"title":"Laser and Natural Guide Star Measured Turbulent Wavefront Correlation","authors":"R. Deron, Sylvain Laurent, M. Séchaud, G. Rousset","doi":"10.1364/adop.1995.fa1","DOIUrl":"https://doi.org/10.1364/adop.1995.fa1","url":null,"abstract":"The laser guide star concept was proposed for the application of adaptive optics in astronomy in order to overcome the problem of natural star requisite brightness which significantly limits the sky coverage [1, 2]. Recently, the adaptive optics compensation of turbulent wavefront using laser guide star has been demonstrated [3,4].","PeriodicalId":256393,"journal":{"name":"Adaptive Optics","volume":"38 ","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"1900-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"120973616","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 1900-01-01DOI: 10.1364/adop.1996.athc.13
M. Otsubo, H. Takami, M. Iye
NAOJ has been developing an adaptive optics(AO) system for SUBARU 8.2m telescope. The AO system is composed of a curvature wavefront sensor and a bimorph mirror with 36 elements.
{"title":"Optimization of Bimorph Mirror Electrode Pattern for SUBARU AO System","authors":"M. Otsubo, H. Takami, M. Iye","doi":"10.1364/adop.1996.athc.13","DOIUrl":"https://doi.org/10.1364/adop.1996.athc.13","url":null,"abstract":"NAOJ has been developing an adaptive optics(AO) system for SUBARU 8.2m telescope. The AO system is composed of a curvature wavefront sensor and a bimorph mirror with 36 elements.","PeriodicalId":256393,"journal":{"name":"Adaptive Optics","volume":"34 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"1900-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"122686949","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Current astronomical adaptive optics (AO) systems are not able to fully correct the atmospheric turbulence. As a result, the quality of the AO long exposure images is degraded by a residual blur which significantly reduces the contrast of the fine details [1]. Removing this residual blur is the field of image restoration (deconvolution) and since this problem is general to many imaging applications, many different methods have already been developed. To achieve an accurate restoration however, an accurate estimation of the system Point Spread Function (PSF) is usually required. For adaptive optics imaging, the shape of the PSF depends on how well the deformable mirror is able to compensate for the wavefront distortions. This “degree of correction” in turn depends on the size and magnitude of the object used as a reference for wavefront sensing, but also on the characteristics of the turbulence, which is known to be a non-stationary process. As a results, the AO PSF is highly variable [2]. The usual way around this problem involves dedicating of significant portion of the observing time to the sole acquisition of a point source, from which the current PSF is estimated.
{"title":"ADAPTIVE OPTICS LONG EXPOSURE POINT SPREAD FUNCTION RETRIEVAL FROM WAVEFRONT SENSOR MEASUREMENTS: TESTS ON REAL DATA","authors":"J. Véran, F. Rigault, H. Maître","doi":"10.1364/adop.1996.awd.3","DOIUrl":"https://doi.org/10.1364/adop.1996.awd.3","url":null,"abstract":"Current astronomical adaptive optics (AO) systems are not able to fully correct the atmospheric turbulence. As a result, the quality of the AO long exposure images is degraded by a residual blur which significantly reduces the contrast of the fine details [1]. Removing this residual blur is the field of image restoration (deconvolution) and since this problem is general to many imaging applications, many different methods have already been developed. To achieve an accurate restoration however, an accurate estimation of the system Point Spread Function (PSF) is usually required. For adaptive optics imaging, the shape of the PSF depends on how well the deformable mirror is able to compensate for the wavefront distortions. This “degree of correction” in turn depends on the size and magnitude of the object used as a reference for wavefront sensing, but also on the characteristics of the turbulence, which is known to be a non-stationary process. As a results, the AO PSF is highly variable [2]. The usual way around this problem involves dedicating of significant portion of the observing time to the sole acquisition of a point source, from which the current PSF is estimated.","PeriodicalId":256393,"journal":{"name":"Adaptive Optics","volume":"1 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"1900-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"127011081","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 1900-01-01DOI: 10.1364/adop.1996.awd.11
I. Lukin
At registration of astronomical objects through the turbulent atmosphere for large telescopes conditions will be usually realized, when the astronomical image represents from self a chaotic picture interleaved light and dark spots (speckle-strusture). In this connection, it is represented interesting to give an estimation of size of characteristic parameters of these areas. In given message the similar analysis will be carried out on the basis of treatment light spots of speckle-structure as the random spikes of intensity of the astronomical image.
{"title":"Spatial Spikes of Intensity of the Atmospherically–distorted Images","authors":"I. Lukin","doi":"10.1364/adop.1996.awd.11","DOIUrl":"https://doi.org/10.1364/adop.1996.awd.11","url":null,"abstract":"At registration of astronomical objects through the turbulent atmosphere for large telescopes conditions will be usually realized, when the astronomical image represents from self a chaotic picture interleaved light and dark spots (speckle-strusture). In this connection, it is represented interesting to give an estimation of size of characteristic parameters of these areas. In given message the similar analysis will be carried out on the basis of treatment light spots of speckle-structure as the random spikes of intensity of the astronomical image.","PeriodicalId":256393,"journal":{"name":"Adaptive Optics","volume":"4 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"1900-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"121772508","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
J. Gonglewski, D. Dayton, S. Sandven, D. Laughlin, S. Rogers, S. McDermott, S. Browne, Robert D. Babnick, Joe Rae, J. Gallegos, R. Highland
An experiment with a nasmyth adaptive optics system mounted on the SOR 3.5m telescope is described. The 183 actuator mirror allows only partial compensation in the near IR, and the imagery is enhanced by postprocessing methods. We describe the system design, and evaluate the performance based on long-to-short exposure SNR ratio metrics.
{"title":"Experimental Results of a Low-Order Adaptive Optics Experiment on the Starfire 3.5m Telescope","authors":"J. Gonglewski, D. Dayton, S. Sandven, D. Laughlin, S. Rogers, S. McDermott, S. Browne, Robert D. Babnick, Joe Rae, J. Gallegos, R. Highland","doi":"10.1364/adop.1995.fa5","DOIUrl":"https://doi.org/10.1364/adop.1995.fa5","url":null,"abstract":"An experiment with a nasmyth adaptive optics system mounted on the SOR 3.5m telescope is described. The 183 actuator mirror allows only partial compensation in the near IR, and the imagery is enhanced by postprocessing methods. We describe the system design, and evaluate the performance based on long-to-short exposure SNR ratio metrics.","PeriodicalId":256393,"journal":{"name":"Adaptive Optics","volume":"180 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"1900-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"132932897","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 1900-01-01DOI: 10.1364/adop.1996.athc.21
V. V. Reznichenko, Vladislav V. Nicitin, A. Onokhov, Michail V. Isaev, Natalia L.Ivanova, L. Beresnev, W. Haase
We have developed efficient optically controlled liquid-crystal optically addressed spatial light modulators that possess modulation parameters for reflected light.
我们开发了具有反射光调制参数的高效光控液晶光寻址空间光调制器。
{"title":"Liquid Crystal Spatial Modulators with Segmented Mirror for Adaptive Optics.","authors":"V. V. Reznichenko, Vladislav V. Nicitin, A. Onokhov, Michail V. Isaev, Natalia L.Ivanova, L. Beresnev, W. Haase","doi":"10.1364/adop.1996.athc.21","DOIUrl":"https://doi.org/10.1364/adop.1996.athc.21","url":null,"abstract":"We have developed efficient optically controlled liquid-crystal optically addressed spatial light modulators that possess modulation parameters for reflected light.","PeriodicalId":256393,"journal":{"name":"Adaptive Optics","volume":"285 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"1900-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"133534243","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 1900-01-01DOI: 10.1364/adop.1996.athc.28
É. Prieto, D. Bonaccini, H. Geoffray, P. Prado, L. Demailly
The evaluation of the quality parameters of the adaptive correction and their evolution with time is important while your adaptive optics system is running. It allows to give an observer a precise feeling of what he will get in the integrated image, it allows the operator to keep an eye on the system performance, and it allows the implementation of adaptive filtering techniques to the servo control laws. These reason have driven us to implement such a tool on the ESO Adonis system. To know the image quality parameters the only possibilities are to directly look at the science image or from the wavefront sensor residuals. Our purpose is to report on our attempts to evaluate the long exposure Strehl ratio and FWHM of the corrected PSF, by using the residual slopes given by the Wave Front Sensor (for us a Shark-Hartmann). We have used the following relation to compute the long exposure strehl1:
{"title":"Adaptive Optics Servo-system Performance Estimator: practical implementation","authors":"É. Prieto, D. Bonaccini, H. Geoffray, P. Prado, L. Demailly","doi":"10.1364/adop.1996.athc.28","DOIUrl":"https://doi.org/10.1364/adop.1996.athc.28","url":null,"abstract":"The evaluation of the quality parameters of the adaptive correction and their evolution with time is important while your adaptive optics system is running. It allows to give an observer a precise feeling of what he will get in the integrated image, it allows the operator to keep an eye on the system performance, and it allows the implementation of adaptive filtering techniques to the servo control laws. These reason have driven us to implement such a tool on the ESO Adonis system. To know the image quality parameters the only possibilities are to directly look at the science image or from the wavefront sensor residuals. Our purpose is to report on our attempts to evaluate the long exposure Strehl ratio and FWHM of the corrected PSF, by using the residual slopes given by the Wave Front Sensor (for us a Shark-Hartmann). We have used the following relation to compute the long exposure strehl1:","PeriodicalId":256393,"journal":{"name":"Adaptive Optics","volume":"90 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"1900-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"131797423","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
J. Bryant, J. O'Byrne, R. Minard, P. Fekete, L. Cram
The first stage of the AAT adaptive optics program, allowing tip-tilt correction for images and spectroscopy in the near infrared has recently been implemented.
AAT自适应光学计划的第一阶段，允许近红外图像和光谱的倾斜校正，最近已经实施。
{"title":"Tip-Tilt Correction at the Anglo-Australian Telescope","authors":"J. Bryant, J. O'Byrne, R. Minard, P. Fekete, L. Cram","doi":"10.1364/adop.1995.tua54","DOIUrl":"https://doi.org/10.1364/adop.1995.tua54","url":null,"abstract":"The first stage of the AAT adaptive optics program, allowing tip-tilt correction for images and spectroscopy in the near infrared has recently been implemented.","PeriodicalId":256393,"journal":{"name":"Adaptive Optics","volume":"42 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"1900-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"134186444","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Adaptive optics components have been used for almost twenty years without major modifications of the basic hardware. Problems connected with cost, power consumption and reliability have pushed several groups to start, investigating the possibility of using different technologies. Of the many technologies under investigation two, in our opinion, demonstrate a high possibility of being an alternative to conventional adaptive mirrors. They are liquid crystal spatial light modulators and and micro-machined mirrors. The USAF Phillips Laboratory, is investigating both these technologies, however here we report, on the results of the liquid crystal work, which has a slightly longer history and more maturity.
{"title":"Liquid Crystals for Adaptive Optics","authors":"S. Restaino, R. Carreras, G. Love","doi":"10.1364/adop.1995.tua47","DOIUrl":"https://doi.org/10.1364/adop.1995.tua47","url":null,"abstract":"Adaptive optics components have been used for almost twenty years without major modifications of the basic hardware. Problems connected with cost, power consumption and reliability have pushed several groups to start, investigating the possibility of using different technologies. Of the many technologies under investigation two, in our opinion, demonstrate a high possibility of being an alternative to conventional adaptive mirrors. They are liquid crystal spatial light modulators and and micro-machined mirrors. The USAF Phillips Laboratory, is investigating both these technologies, however here we report, on the results of the liquid crystal work, which has a slightly longer history and more maturity.","PeriodicalId":256393,"journal":{"name":"Adaptive Optics","volume":"22 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"1900-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"114371222","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Detailed computer simulations have been performed to evaluate the potential for spatio-temporal prediction of wavefront slope data from a Shack-Hartmann sensor to improve the imaging quality of an astronomical adaptive optics system by overcoming the effect of the inherent delay between sensing and correcting the wavefront phase error. Results of the simulations show that an improvement of a factor of at least 2 in the residual mean-square phase error can be achieved by extrapolating into the future on the basis of past wavefront measurements. Experiments will be conducted very shortly with actual data gathered at a 1.6 m telescope using a Shack-Hartmann sensor with 31-cm subapertures to test the simulations. Both the simulations and the experimental arrangement have been chosen to match closely the measured operating conditions of the adaptive optics system under construction for the 6.5 m MMT (Martin & Anderson 1995).
利用Shack-Hartmann传感器的波前斜率数据进行时空预测，克服感知和校正波前相位误差之间的固有延迟，提高天文自适应光学系统的成像质量，并进行了详细的计算机模拟。仿真结果表明，在过去波前测量的基础上，通过外推到未来，可以将剩余均方相位误差提高至少2个因子。实验将很快进行，使用1.6米望远镜收集的实际数据，使用具有31厘米子孔径的Shack-Hartmann传感器来测试模拟。所选择的模拟和实验安排都与正在建造的6.5 m MMT自适应光学系统的测量工作条件密切匹配(Martin & Anderson 1995)。
{"title":"Linear Spatio-Temporal Prediction for Adaptive Optics Wavefront Reconstructors","authors":"M. Lloyd-Hart","doi":"10.1364/adop.1995.tua7","DOIUrl":"https://doi.org/10.1364/adop.1995.tua7","url":null,"abstract":"Detailed computer simulations have been performed to evaluate the potential for spatio-temporal prediction of wavefront slope data from a Shack-Hartmann sensor to improve the imaging quality of an astronomical adaptive optics system by overcoming the effect of the inherent delay between sensing and correcting the wavefront phase error. Results of the simulations show that an improvement of a factor of at least 2 in the residual mean-square phase error can be achieved by extrapolating into the future on the basis of past wavefront measurements. Experiments will be conducted very shortly with actual data gathered at a 1.6 m telescope using a Shack-Hartmann sensor with 31-cm subapertures to test the simulations. Both the simulations and the experimental arrangement have been chosen to match closely the measured operating conditions of the adaptive optics system under construction for the 6.5 m MMT (Martin & Anderson 1995).","PeriodicalId":256393,"journal":{"name":"Adaptive Optics","volume":"41 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"1900-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"115836618","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
京公网安备 11010802042870号
京ICP备2023020795号-1
扫码关注我们
求助内容：
应助结果提醒方式：