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}
Pub Date : 1900-01-01DOI: 10.1364/adop.1996.atub.1
L. Close, F. Roddier, C. Roddier, M. Northcott, J. E. (. Graves
The Adaptive Optics system, built at the Institute for Astronomy (University of Hawai’i), has been making unique scientific observations since 1993. During that period this versatile AO system has been mounted at both Cassegrain and coude feeds at the 3.6m CFH telescope and the bent Cassegrain at the 3.8m UKIRT telescope. The instrument is now permanently a Cassegrain instrument which has enjoyed 24 nights of 4m class observing at Manua Kea.
{"title":"Bubbles, Disks, and Planets: Science with the University of Hawai’i AO System","authors":"L. Close, F. Roddier, C. Roddier, M. Northcott, J. E. (. Graves","doi":"10.1364/adop.1996.atub.1","DOIUrl":"https://doi.org/10.1364/adop.1996.atub.1","url":null,"abstract":"The Adaptive Optics system, built at the Institute for Astronomy (University of Hawai’i), has been making unique scientific observations since 1993. During that period this versatile AO system has been mounted at both Cassegrain and coude feeds at the 3.6m CFH telescope and the bent Cassegrain at the 3.8m UKIRT telescope. The instrument is now permanently a Cassegrain instrument which has enjoyed 24 nights of 4m class observing at Manua Kea.","PeriodicalId":256393,"journal":{"name":"Adaptive Optics","volume":"59 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":"124496038","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 (AO) has the capability of providing diffraction-limited images from ground-based astronomical telescopes through the turbulent atmosphere. Because of limitations in the AO system, the point spread functions (PSF’s) of the AO system suffers from incomplete compensation and variability. Depending on the observation wavelength (λ), the spatial coherence length of the atmosphere (r0), the sub-aperture size (d), the correlation time of the atmosphere (τ0), the sample time of the wavefront sensing (t s ), and the signal strength of the source, the Strehl ratios of the compensated images can vary considerably (between 2% – 90%). In addition, residual errors in tilt compensation due to the source signal strength can further degrade the image quality. Thus, AO compensated imaging genearally requires some post-processing to extract the maximum possible information. As long as the PSF for the imaging process is stationary, then standard deconvolution algorithms can be applied. These algorithms have been recently developed and applied to Hubble Space Telescope imaging and include maximum-likelihood, maximum-entropy and pixon-based algorithms, etc.[1].
{"title":"Post-Processing of Adaptive Optics Images: Blind Deconvolution Analysis","authors":"J. Christou, E. Hege, S. Jefferies","doi":"10.1364/adop.1996.awa.1","DOIUrl":"https://doi.org/10.1364/adop.1996.awa.1","url":null,"abstract":"Adaptive Optics (AO) has the capability of providing diffraction-limited images from ground-based astronomical telescopes through the turbulent atmosphere. Because of limitations in the AO system, the point spread functions (PSF’s) of the AO system suffers from incomplete compensation and variability. Depending on the observation wavelength (λ), the spatial coherence length of the atmosphere (r0), the sub-aperture size (d), the correlation time of the atmosphere (τ0), the sample time of the wavefront sensing (t\u0000 s\u0000 ), and the signal strength of the source, the Strehl ratios of the compensated images can vary considerably (between 2% – 90%). In addition, residual errors in tilt compensation due to the source signal strength can further degrade the image quality. Thus, AO compensated imaging genearally requires some post-processing to extract the maximum possible information. As long as the PSF for the imaging process is stationary, then standard deconvolution algorithms can be applied. These algorithms have been recently developed and applied to Hubble Space Telescope imaging and include maximum-likelihood, maximum-entropy and pixon-based algorithms, etc.[1].","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":"125265698","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}
The past decade has seen the development of new devices to reliably monitor atmospheric seeing and several observatories are now routinely proposing to the observers new services including online visualization of the site seeing as in addition to standard meteorological parameters.
{"title":"Site Atmospheric Characterization","authors":"M. Sarazin","doi":"10.1364/adop.1995.thc1","DOIUrl":"https://doi.org/10.1364/adop.1995.thc1","url":null,"abstract":"The past decade has seen the development of new devices to reliably monitor atmospheric seeing and several observatories are now routinely proposing to the observers new services including online visualization of the site seeing as in addition to standard meteorological parameters.","PeriodicalId":256393,"journal":{"name":"Adaptive Optics","volume":"13 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":"122446629","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}
We present an exhaustive review of adaptive optics systems with a vocation for astronomy. After a brief historical introduction, we review the different technological approaches and the results.
{"title":"Review of astronomical adaptive optics systems on medium size (1.5-5m) telescopes","authors":"F. Rigaut","doi":"10.1364/adop.1996.ama.2","DOIUrl":"https://doi.org/10.1364/adop.1996.ama.2","url":null,"abstract":"We present an exhaustive review of adaptive optics systems with a vocation for astronomy. After a brief historical introduction, we review the different technological approaches and the results.","PeriodicalId":256393,"journal":{"name":"Adaptive Optics","volume":"14 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":"122607036","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}
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}
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}
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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