Pub Date : 1900-01-01DOI: 10.1364/adop.1996.amb.15
J. Graves
The highly successful AO program at the UH is now planning to expand the curvature technology into higher order correction systems with a unique Vis/IR WFS concept.. Computer simulation have been carried out scaling the current 13 element system now being used at the CFHT on Mauna Kea to a 36 element design. The Vis-IR WFS sensor is expected to increase the performance overall, all as it is used to study young stellar objects that are at many times deeply reddened. An example is HL Tau, in the visible it is around magnitude 14 and at the H band it magnitude 9 or 100 times brighter!
{"title":"Future Directions for the University of Hawaii Adaptive Optics Program","authors":"J. Graves","doi":"10.1364/adop.1996.amb.15","DOIUrl":"https://doi.org/10.1364/adop.1996.amb.15","url":null,"abstract":"The highly successful AO program at the UH is now planning to expand the curvature technology into higher order correction systems with a unique Vis/IR WFS concept.. Computer simulation have been carried out scaling the current 13 element system now being used at the CFHT on Mauna Kea to a 36 element design. The Vis-IR WFS sensor is expected to increase the performance overall, all as it is used to study young stellar objects that are at many times deeply reddened. An example is HL Tau, in the visible it is around magnitude 14 and at the H band it magnitude 9 or 100 times brighter!","PeriodicalId":256393,"journal":{"name":"Adaptive Optics","volume":"31 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":"116252726","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) works in many cases in the partial correction regime, i.e. with a Strehl ratio lower than 0.8. In this regime, seeing variations induce some variations in the correction (see Tessier 95), as shown on Fig. 1 which plots the Strehl ratio for continuous frames taken with the Come-On Plus instrument (see Beuzit et al. 94 for a description of this instrument).
自适应光学(AO)工作在许多情况下，在部分校正制度，即与斯特雷特比低于0.8。在这种情况下，看到变化会导致校正的一些变化(见Tessier 95)，如图1所示，图1绘制了用Come-On Plus仪器拍摄的连续帧的Strehl比率(见Beuzit et al. 94对该仪器的描述)。
{"title":"Speckle techniques for adaptive optics in the partial correction regime","authors":"E. Tessier, C. Perrier","doi":"10.1364/adop.1996.awa.4","DOIUrl":"https://doi.org/10.1364/adop.1996.awa.4","url":null,"abstract":"Adaptive optics (AO) works in many cases in the partial correction regime, i.e. with a Strehl ratio lower than 0.8. In this regime, seeing variations induce some variations in the correction (see Tessier 95), as shown on Fig. 1 which plots the Strehl ratio for continuous frames taken with the Come-On Plus instrument (see Beuzit et al. 94 for a description of this instrument).","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":"123152237","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. N. Yeskov, B. É. Bonshtedt, S. N. Koreshev, G. I. Lebedeva, V. Parfenov, V. Podoba, V. V. Reznichenko, A. G. Seregin, V. Sidorov, V. N. Smirnov, L. G. Fedina, N. T. Firsov, V. K. Khakunov, I. S. Etsin
At present, some large-scale programs are carried out in various countries that are aimed towards development of a new class of ground and space telescopes for both civil and military use. Being now at different stages of implementation, these programs have been initiated by both scientific and military and political causes and, to a large extent, owing to emerging technologies coupled mainly with active and adaptive optics.
{"title":"Adaptive Astronomical Telescope with Two-Stage Wavefront Correction: current status of a project","authors":"D. N. Yeskov, B. É. Bonshtedt, S. N. Koreshev, G. I. Lebedeva, V. Parfenov, V. Podoba, V. V. Reznichenko, A. G. Seregin, V. Sidorov, V. N. Smirnov, L. G. Fedina, N. T. Firsov, V. K. Khakunov, I. S. Etsin","doi":"10.1364/adop.1995.wc4","DOIUrl":"https://doi.org/10.1364/adop.1995.wc4","url":null,"abstract":"At present, some large-scale programs are carried out in various countries that are aimed towards development of a new class of ground and space telescopes for both civil and military use. Being now at different stages of implementation, these programs have been initiated by both scientific and military and political causes and, to a large extent, owing to emerging technologies coupled mainly with active and adaptive optics.","PeriodicalId":256393,"journal":{"name":"Adaptive Optics","volume":"36 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":"123691724","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}
Pub Date : 1900-01-01DOI: 10.1364/adop.1996.athc.11
L. Fini, S. Esposito
We address problems of control loop parameters optimization for tip-tilt correction system based on the approach followed for the T.N.G. tracking system.
本文在T.N.G.跟踪系统的基础上，研究了倾斜校正系统的控制回路参数优化问题。
{"title":"Tip-Tilt Control Loop Optimization","authors":"L. Fini, S. Esposito","doi":"10.1364/adop.1996.athc.11","DOIUrl":"https://doi.org/10.1364/adop.1996.athc.11","url":null,"abstract":"We address problems of control loop parameters optimization for tip-tilt correction system based on the approach followed for the T.N.G. tracking system.","PeriodicalId":256393,"journal":{"name":"Adaptive Optics","volume":"96 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":"124667405","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}
Deconvolution from Wave-Front Sensing (DWFS) has been investigated both through laboratory and field experiments as a method to produce high resolution images from ground based telescopes.1,2,3 This technique has sometimes been referred to as Speclde Holography. With this technique a short exposure focal plane image is recorded simultaneously with an estimate of the atmospheric wave-front. The wave-front estimate is used to calculate an optical transfer function (OTF) for the atmosphere. This OTF estimate is then used in a deconvolution algorithm to correct the focal plane image. A synoptic sketch of a DWFS instrument is shown in figure 1.
{"title":"Comparison of Speckle Image Reconstruction Techniques: Experimental Measurements of Estimator Bias and Signal to Noise Ratio","authors":"D. Dayton, S. Sandven, J. Gonglewski","doi":"10.1364/adop.1995.wb1","DOIUrl":"https://doi.org/10.1364/adop.1995.wb1","url":null,"abstract":"Deconvolution from Wave-Front Sensing (DWFS) has been investigated both through laboratory and field experiments as a method to produce high resolution images from ground based telescopes.1,2,3 This technique has sometimes been referred to as Speclde Holography. With this technique a short exposure focal plane image is recorded simultaneously with an estimate of the atmospheric wave-front. The wave-front estimate is used to calculate an optical transfer function (OTF) for the atmosphere. This OTF estimate is then used in a deconvolution algorithm to correct the focal plane image. A synoptic sketch of a DWFS instrument is shown in figure 1.","PeriodicalId":256393,"journal":{"name":"Adaptive Optics","volume":"25 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":"121675049","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. Currie, P. Avizonis, D. M. Dowling, D. O’Leary, J. Nagy, R. Fugate
Image processing methods, highlighting specific hardware systems, will be demonstrated. Correcting spatial dependence and instrumental artifacts of the Point-Spread-Function significantly improves image guality.
图像处理方法，突出具体的硬件系统，将演示。校正空间依赖性和点扩散函数的仪器伪影显著提高图像质量。
{"title":"Approaches for Image Processing Supporting Adaptive Optics","authors":"D. Currie, P. Avizonis, D. M. Dowling, D. O’Leary, J. Nagy, R. Fugate","doi":"10.1364/adop.1995.tua50","DOIUrl":"https://doi.org/10.1364/adop.1995.tua50","url":null,"abstract":"Image processing methods, highlighting specific hardware systems, will be demonstrated. Correcting spatial dependence and instrumental artifacts of the Point-Spread-Function significantly improves image guality.","PeriodicalId":256393,"journal":{"name":"Adaptive Optics","volume":"30 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":"122014411","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}
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