Hartmann-Shack wavefront sensors (Hartmann WFS) are widely used for optical wavefront measurement in adaptive optics. They are especially useful in the conjunction with laser guide stars that provide a quasi-point-source reference with continuous and pulse operating patterns. The principle of the sensor is that an array of lenslets is used to divide the coming wavefront into subaperatures and form images at their focal planes where the detector is placed. If the wavefront is plane, each lenslet forms an image of the source at its focus. If the wavefront is disturbed, each lenslet receives a tilted wavefront and forms an image out of axis in its focal plane. The measure of the image position gives the angle of arrival of the wave for each lenslet. The Hartmann WFS generally consists of a lenslet array, a detector which is a CCD or an intensified CCD, and an image processing system. For both natural and guide stars, a very low-light photo-counting level characterisation of the sensor is needed. And the knowledge on the low-light performance of the sensor for the both operating patterns is useful for the AO system design.
{"title":"Test and analysis of low-light characterisation of the ICCD Hartmann-Shack wavefront sensor","authors":"Qiang Zhang, Binghuo Xu, Li Chen","doi":"10.1364/adop.1995.tua21","DOIUrl":"https://doi.org/10.1364/adop.1995.tua21","url":null,"abstract":"Hartmann-Shack wavefront sensors (Hartmann WFS) are widely used for optical wavefront measurement in adaptive optics. They are especially useful in the conjunction with laser guide stars that provide a quasi-point-source reference with continuous and pulse operating patterns. The principle of the sensor is that an array of lenslets is used to divide the coming wavefront into subaperatures and form images at their focal planes where the detector is placed. If the wavefront is plane, each lenslet forms an image of the source at its focus. If the wavefront is disturbed, each lenslet receives a tilted wavefront and forms an image out of axis in its focal plane. The measure of the image position gives the angle of arrival of the wave for each lenslet. The Hartmann WFS generally consists of a lenslet array, a detector which is a CCD or an intensified CCD, and an image processing system. For both natural and guide stars, a very low-light photo-counting level characterisation of the sensor is needed. And the knowledge on the low-light performance of the sensor for the both operating patterns is useful for the AO system design.","PeriodicalId":256393,"journal":{"name":"Adaptive Optics","volume":"56 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":"126642616","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}
{"title":"Review of Industrial Applications","authors":"F. Merkle","doi":"10.1364/adop.1996.awb.1","DOIUrl":"https://doi.org/10.1364/adop.1996.awb.1","url":null,"abstract":"Summary not available.","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":"126013511","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}
Phased telescope arrays can be used to coherently receive or transmit optical radiation [1], even in the presence of wavefront distortion due to turbulent media [2]. In addition, phased telescope arrays operating in receive mode allow to obtain images with high angular resolution [3] and to implement wide field-of-view imaging systems [4].
{"title":"Adaptive Telescope Array for Laser Communications and Astronomy","authors":"K. Kudielka, W. Leeb","doi":"10.1364/adop.1995.thb5","DOIUrl":"https://doi.org/10.1364/adop.1995.thb5","url":null,"abstract":"Phased telescope arrays can be used to coherently receive or transmit optical radiation [1], even in the presence of wavefront distortion due to turbulent media [2]. In addition, phased telescope arrays operating in receive mode allow to obtain images with high angular resolution [3] and to implement wide field-of-view imaging systems [4].","PeriodicalId":256393,"journal":{"name":"Adaptive Optics","volume":"125 44","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"1900-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"132845709","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.16
T. Berkefeld, A. Glindemann
Investigating the tilt correlation as a function of separation angle, exposure time and aperture, the maximum angular distance between the object and the tip-tilt guide star is determined. This distance can be increased by multiple guide stars.
{"title":"Measurements of the Isoplanatic Angle of the Wavefront Tilt","authors":"T. Berkefeld, A. Glindemann","doi":"10.1364/adop.1996.awd.16","DOIUrl":"https://doi.org/10.1364/adop.1996.awd.16","url":null,"abstract":"Investigating the tilt correlation as a function of separation angle, exposure time and aperture, the maximum angular distance between the object and the tip-tilt guide star is determined. This distance can be increased by multiple guide stars.","PeriodicalId":256393,"journal":{"name":"Adaptive Optics","volume":"27 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":"133551730","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.amb.18
J. Kenemuth, J. McNally, James R. Passaro, P. Berger, Carlo La Fiandra, Rene Abreu
The Advanced Electro-Optical System (AEOS) is being developed as an upgrade to the Air Force Maui Space Surveillance Site (MSSS) on Haleakala, Maui, Hawaii. It consists of a new 3.6-m diameter telescope in an azimuth-elevation configuration mounted atop a pier approximately 60 ft above the local ground level. A bent-Cassegrain configuration provides for selection between three (3) sensor locations on the telescope trunnion and access to a coudé path through the elevation and azimuth axes to ground level. The coudé optics in the telescope provide a ± 150 μrad field of view over a 0.5 to 5.0 μm spectral band to a 941-actuator adaptive optics system located in the coudé path directly beneath the telescope at ground level (coudé room) which will provide dynamic compensation for atmospheric turbulence effects so that a significantly improved image quality may be achieved. A switching mirror located at the output of the adaptive optics system will provide a capability to direct either a compensated beam, or a beam which bypasses the adaptive optics system, to any of seven (7) optics laboratories concentrically located around the room which contains the adaptive optics system.
{"title":"Status of the Advanced Electro-Optical System (AEOS) Adaptive Optics","authors":"J. Kenemuth, J. McNally, James R. Passaro, P. Berger, Carlo La Fiandra, Rene Abreu","doi":"10.1364/adop.1996.amb.18","DOIUrl":"https://doi.org/10.1364/adop.1996.amb.18","url":null,"abstract":"The Advanced Electro-Optical System (AEOS) is being developed as an upgrade to the Air Force Maui Space Surveillance Site (MSSS) on Haleakala, Maui, Hawaii. It consists of a new 3.6-m diameter telescope in an azimuth-elevation configuration mounted atop a pier approximately 60 ft above the local ground level. A bent-Cassegrain configuration provides for selection between three (3) sensor locations on the telescope trunnion and access to a coudé path through the elevation and azimuth axes to ground level. The coudé optics in the telescope provide a ± 150 μrad field of view over a 0.5 to 5.0 μm spectral band to a 941-actuator adaptive optics system located in the coudé path directly beneath the telescope at ground level (coudé room) which will provide dynamic compensation for atmospheric turbulence effects so that a significantly improved image quality may be achieved. A switching mirror located at the output of the adaptive optics system will provide a capability to direct either a compensated beam, or a beam which bypasses the adaptive optics system, to any of seven (7) optics laboratories concentrically located around the room which contains the adaptive optics system.","PeriodicalId":256393,"journal":{"name":"Adaptive Optics","volume":"57 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":"130518786","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}
Application of the well-known principle of heterodyning was first described in Ref. 1 as the Fourier transform method for phase restoration from interferogram and in Ref. 2 as the analytic signal method for designing an interference wave-front sensor. Here we discuss a development of the latter, and go into unknown essential details of it.
{"title":"Interferogram Evaluation by 4D Analytic Signal Theory","authors":"V. A. Tartakowski","doi":"10.1364/adop.1995.tua16","DOIUrl":"https://doi.org/10.1364/adop.1995.tua16","url":null,"abstract":"Application of the well-known principle of heterodyning was first described in Ref. 1 as the Fourier transform method for phase restoration from interferogram and in Ref. 2 as the analytic signal method for designing an interference wave-front sensor. Here we discuss a development of the latter, and go into unknown essential details of it.","PeriodicalId":256393,"journal":{"name":"Adaptive Optics","volume":"3 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":"130822406","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}
D. Bruns, T. Barrett, G. Brusa, R. Biasi, D. Gallieni
The MMT will be converted to a single 6.5 m primary mirror in 1997. The new telescope will be equipped with adaptive optics for high-resolution infrared astronomy at wavelengths between 1.6 microns and 5 microns. Atmospheric distortions will be corrected using an adaptive secondary mirror which directly feeds a high-resolution infrared detector. The use of an adaptive secondary maximizes emissivity, which provides high throughput to the imaging detector and efficient wavefront sensing by eliminating many optical elements normally needed in Coudé systems.
{"title":"Adaptive Secondary Development","authors":"D. Bruns, T. Barrett, G. Brusa, R. Biasi, D. Gallieni","doi":"10.1364/adop.1996.afa.1","DOIUrl":"https://doi.org/10.1364/adop.1996.afa.1","url":null,"abstract":"The MMT will be converted to a single 6.5 m primary mirror in 1997. The new telescope will be equipped with adaptive optics for high-resolution infrared astronomy at wavelengths between 1.6 microns and 5 microns. Atmospheric distortions will be corrected using an adaptive secondary mirror which directly feeds a high-resolution infrared detector. The use of an adaptive secondary maximizes emissivity, which provides high throughput to the imaging detector and efficient wavefront sensing by eliminating many optical elements normally needed in Coudé systems.","PeriodicalId":256393,"journal":{"name":"Adaptive Optics","volume":"33 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":"133126946","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}
Astronomers have long known that the resolution in ground-based astronomy is almost always limited by aberrations introduced by the atmosphere. Over the years, researchers have developed a variety of clever pre- and post-detection approaches for correcting these effects. A strong argument can be made for pre-detection correction. It can be shown that the Modulation Transfer Function (MTF) will achieve a maximum at each spatial frequency when the system is unaberrated [1]. Aberrations can only modulate object spatial-frequency information to reduced levels. This modulation could be perfectly inverted in the absence of noise. However, detection of the imagery always introduces noise and inversion schemes result in noise amplification. Therefore, when it can be successfully accomplished, pre-detection correction is preferable to post-detection correction with regard to signal-to-noise ratio.
天文学家早就知道，地面天文学的分辨率几乎总是受到大气引入的像差的限制。多年来，研究人员开发了各种巧妙的检测前和检测后方法来纠正这些影响。可以提出一个强有力的理由来支持检测前校正。可以看出，当系统无像差时，调制传递函数(Modulation Transfer Function, MTF)在每个空间频率处都达到最大值[1]。像差只能将物体的空间频率信息调制到较低的水平。这种调制可以在没有噪声的情况下完全反转。然而，图像的检测总是会引入噪声，而反演方案会导致噪声放大。因此，当能够成功完成时，就信噪比而言，检测前校正优于检测后校正。
{"title":"Roles for Phase Diversity in Compensated Imaging","authors":"R. Paxman","doi":"10.1364/adop.1996.awa.3","DOIUrl":"https://doi.org/10.1364/adop.1996.awa.3","url":null,"abstract":"Astronomers have long known that the resolution in ground-based astronomy is almost always limited by aberrations introduced by the atmosphere. Over the years, researchers have developed a variety of clever pre- and post-detection approaches for correcting these effects. A strong argument can be made for pre-detection correction. It can be shown that the Modulation Transfer Function (MTF) will achieve a maximum at each spatial frequency when the system is unaberrated [1]. Aberrations can only modulate object spatial-frequency information to reduced levels. This modulation could be perfectly inverted in the absence of noise. However, detection of the imagery always introduces noise and inversion schemes result in noise amplification. Therefore, when it can be successfully accomplished, pre-detection correction is preferable to post-detection correction with regard to signal-to-noise ratio.","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":"133278710","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.2
V. A. Tartakovski, Vladimir P. ukin
Lomonosov and Descartes had known about the first principles of the Hartmann measurements. There are many references1 to a classical version of this method concerning testing the telescope optics. At the modern stage the Shack–Hartmann sensor is used.
{"title":"Scan–Hartmann Wavefront Sensor","authors":"V. A. Tartakovski, Vladimir P. ukin","doi":"10.1364/adop.1996.athc.2","DOIUrl":"https://doi.org/10.1364/adop.1996.athc.2","url":null,"abstract":"Lomonosov and Descartes had known about the first principles of the Hartmann measurements. There are many references1 to a classical version of this method concerning testing the telescope optics. At the modern stage the Shack–Hartmann sensor is used.","PeriodicalId":256393,"journal":{"name":"Adaptive Optics","volume":"63 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":"133903678","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}
V. V. Reznichenko, Victor V. Kotov, Y. Leonov, V. N. Smirnov, M. E. Zvezdina
The majority of wavefront disturbances of space reflector and space telescopes are due to external thermal fields variations and the optical surface deformations.
空间反射镜和空间望远镜的波前扰动主要是由于外热场的变化和光学表面的变形引起的。
{"title":"Numerical Simulation and Test Of A Model Thermo-Adaptive Mirror","authors":"V. V. Reznichenko, Victor V. Kotov, Y. Leonov, V. N. Smirnov, M. E. Zvezdina","doi":"10.1364/adop.1995.tua26","DOIUrl":"https://doi.org/10.1364/adop.1995.tua26","url":null,"abstract":"The majority of wavefront disturbances of space reflector and space telescopes are due to external thermal fields variations and the optical surface deformations.","PeriodicalId":256393,"journal":{"name":"Adaptive Optics","volume":"18 6 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":"122378472","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}
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