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Exploring High Altitude Beacon Concepts Other Than Sodium 探索除钠以外的高空信标概念
Adaptive Optics Pub Date : 1900-01-01 DOI: 10.1364/adop.1996.amc.4
J. Telle
{"title":"Exploring High Altitude Beacon Concepts Other Than Sodium","authors":"J. Telle","doi":"10.1364/adop.1996.amc.4","DOIUrl":"https://doi.org/10.1364/adop.1996.amc.4","url":null,"abstract":"Na and most other mesospheric species suffer from two major shortcomings, low density and low saturation intensity. The Na density in the mesosphere is typically 103 - 104 atoms per cm3. Moreover this density is spread over about 100 velocity classes with a natural width of 10 MHz giving a total Doppler width of 1 GHz for each line. The D2 line is split by 1.772 GHz into a doublet ignoring other hyperfine splittings of the order of 10 MHz. The doublet is often treated as a single line with 3 GHz FWHM. The Doppler-broadened Na cross section is about 2.7 (-12) cm2 but the low density results in only about 1.5% unsaturated absorption across the entire mesosphere (depth ≈ 10 km).","PeriodicalId":256393,"journal":{"name":"Adaptive Optics","volume":"8 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":"123941274","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}
引用次数: 1
Measurement of a Non-Kolmogorov Structure Function 非kolmogorov结构函数的测量
Adaptive Optics Pub Date : 1900-01-01 DOI: 10.1364/adop.1996.awd.15
T. Nicholls, N. Wooder, C. Dainty
{"title":"Measurement of a Non-Kolmogorov Structure Function","authors":"T. Nicholls, N. Wooder, C. Dainty","doi":"10.1364/adop.1996.awd.15","DOIUrl":"https://doi.org/10.1364/adop.1996.awd.15","url":null,"abstract":"The structure function of atmospheric phase fluctuations is defined as follows: A generalised model for the structure function of phase is: ℛ\u0000 0\u0000 is related to the size of the long-exposure image formed by a large-aperture telescope, while γ\u0000 ß\u0000 is a parameter which depends on ß and on the precise definition of ℛ\u0000 0\u0000 The widely-used Kolmogorov model of refractive index fluctuations [1] predicts a value of 11/3 for ß; in this case, with the appropriate definition, ℛ0 is equivalent to r0, the Fried parameter [2], Under the Kolmogorov assumption, the parameter r0 entirely describes the time-averaged statistics of the phase fluctuations. A knowledge of r0 can be used, for example, to predict how the energy in the phase fluctuations is distributed between the Zernike modes.","PeriodicalId":256393,"journal":{"name":"Adaptive Optics","volume":"35 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":"124212777","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}
引用次数: 0
Adaptive Optics NIR Imaging of R136 in 30 Doradus: The Stellar Population of a Nearby Starburst 剑鱼座30中R136的自适应光学近红外成像:附近星暴的恒星群
Adaptive Optics Pub Date : 1900-01-01 DOI: 10.1017/S0074180900001674
B. Brandl, B. Sams, F. Bertoldi, A. Eckart, R. Genzel, S. Drapatz, R. Hofmann, M. Loewe, A. Quirrenbach
{"title":"Adaptive Optics NIR Imaging of R136 in 30 Doradus: The Stellar Population of a Nearby Starburst","authors":"B. Brandl, B. Sams, F. Bertoldi, A. Eckart, R. Genzel, S. Drapatz, R. Hofmann, M. Loewe, A. Quirrenbach","doi":"10.1017/S0074180900001674","DOIUrl":"https://doi.org/10.1017/S0074180900001674","url":null,"abstract":"We report 0.″15 resolution near infrared imaging of the starburst cluster R136. Our 12.″8 × 12.″8 images were recorded with the MPE camera SHARP II at the 3.6m ESO telescope, using the adaptive optics system COMEON +. The diffraction-limited spatial resolution and high sensitivity (20th magnitude in K) of our observations allow our H and K band images to be compared and combined with recent HST WFPC2 data of R136. Fitting theoretical models to the observed magnitudes we derive the stellar population, age and dynamics of this starburst region. The radial variation of the mass function and the dependence of the derived core radius on the observed stellar mass range reveal strong mass segregation that is probably due to the cluster’s dynamical evolution.","PeriodicalId":256393,"journal":{"name":"Adaptive Optics","volume":"135 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":"128612645","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}
引用次数: 3
CFHT Adaptive Optics & Adonis observations of Starburst galaxies 星爆星系的CFHT自适应光学与阿多尼斯观测
Adaptive Optics Pub Date : 1900-01-01 DOI: 10.1364/adop.1996.awd.21
O. Lai, D. Rouan, E. Gendron, F. Rigaut
{"title":"CFHT Adaptive Optics & Adonis observations of Starburst galaxies","authors":"O. Lai, D. Rouan, E. Gendron, F. Rigaut","doi":"10.1364/adop.1996.awd.21","DOIUrl":"https://doi.org/10.1364/adop.1996.awd.21","url":null,"abstract":"To be able to understand the link between starburst and AGN (are starburst progenitors of AGNs? e.g. Sanders et al 1988), high angular resolution is essential so as to identify each phenomena, and their respective contribution to the luminosity. Observations first carried out with ADONIS, ESO's adaptive optics instrument, and now with PUEO, CFHT's adaptive optics bonnette of starburst galaxies allow to study the morphology of potential starburst regions, and more precisely, to shed some light on the probable link between starburst activity and characteristic structures; for instance, these can be very young or old star population aggregate, circumnuclear starburst disks or rings. Signs of mergers (multiple nuclei, wisps or tails) are also of interest as they allow to look into the question whether there always is a merger at the onset of a starburst (Mirabel & Sanders, 1989), and if so, at which phase.","PeriodicalId":256393,"journal":{"name":"Adaptive Optics","volume":"142 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":"115991570","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}
引用次数: 0
Progress Toward the 6.5-m MMT Infrared Adaptive Optics System 6.5 m MMT红外自适应光学系统研究进展
Adaptive Optics Pub Date : 1900-01-01 DOI: 10.1364/adop.1996.amb.8
M. Lloyd-Hart, J. Angel, D. Sandler, P. Salinari, D. Bruns, T. Barrett
{"title":"Progress Toward the 6.5-m MMT Infrared Adaptive Optics System","authors":"M. Lloyd-Hart, J. Angel, D. Sandler, P. Salinari, D. Bruns, T. Barrett","doi":"10.1364/adop.1996.amb.8","DOIUrl":"https://doi.org/10.1364/adop.1996.amb.8","url":null,"abstract":"In late 1996, the existing six mirrors of the Multiple Mirror Telescope (MMT) will be replaced by a single 6.5-m mirror, which is now being polished at the Steward Observatory Mirror Lab. Earlier work [1, 2] has shown that an adaptive optics system using a single sodium laser projected co-axially with the telescope can provide imaging at the diffraction limit in the H and K photometric bands over most of the sky. In the design of the system for the 6.5-m, we will project a 4-W beam from a continuous-wave dye laser from a refractive launch telescope [3] located behind the secondary mirror. Returning light will be corrected for the effects of atmospheric turbulence at the secondary mirror, which will be a 2-mm thick continuous facesheet whose shape can be modified at 1 kHz update rate by 300 voice-coil actuators. The major components of the system are shown in the schematic of Figure 1.","PeriodicalId":256393,"journal":{"name":"Adaptive Optics","volume":"7 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":"117086871","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}
引用次数: 0
United Kingdom Adaptive Optics Programs 英国自适应光学项目
Adaptive Optics Pub Date : 1900-01-01 DOI: 10.1364/adop.1995.ma2
G. Gilmore
{"title":"United Kingdom Adaptive Optics Programs","authors":"G. Gilmore","doi":"10.1364/adop.1995.ma2","DOIUrl":"https://doi.org/10.1364/adop.1995.ma2","url":null,"abstract":"The UK has a funded, national program underway to design and construct facility (common user) natural guide star (NGS) adaptive optics systems for two telescopes: • The 4.2m William Hershel Telescope (WHT) on La Palma, Canary Islands. • The 3.8m United Kingdom Infrared Telesope (UKIRT) on Mauna Kea, Hawaii. These will be locally-supported systems, capable of feeding a number of science instruments, including dedicated AO-optimised imagers and spectrographs. They will be optimised for operation in the near infrared, ~ 2 μm.","PeriodicalId":256393,"journal":{"name":"Adaptive Optics","volume":"67 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":"116748900","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}
引用次数: 0
Optimization of the Starfire Optical Range 3.5 M adaptive optics for astronomical imaging Starfire光学距离3.5 M天文成像自适应光学系统的优化
Adaptive Optics Pub Date : 1900-01-01 DOI: 10.1364/adop.1996.amb.17
D. Link, R. Vernon
{"title":"Optimization of the Starfire Optical Range 3.5 M adaptive optics for astronomical imaging","authors":"D. Link, R. Vernon","doi":"10.1364/adop.1996.amb.17","DOIUrl":"https://doi.org/10.1364/adop.1996.amb.17","url":null,"abstract":"SAIC has developed a wave-optics, time domain, engineering simulation of adaptive optics systems. The Atmospheric Compensation Simulation (ACS) includes both physics effects (e.g., inner and outer scale, various turbulence profiles, wind, anisoplanatism, time of flight, scattering, absorption, sodium layer saturation) and engineering effects (e.g. jitter, misregistration, latency, digital controls, control surface electro-mechanical response, gain variation, shot and detector noise, quantization, aberrations). The code includes the ability to model multiple three-dimensional laser guidestars, propagating the lasers up from the ground and imaging the irradiance from multiple atmospheric layers onto the detector plane using multiple optical transfer functions or speckle imaging. This simulation has been used to support engineering development on a number of programs and has been validated against theory, experiments, and other codes.","PeriodicalId":256393,"journal":{"name":"Adaptive Optics","volume":"20 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":"115495746","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}
引用次数: 0
Preliminary mechanical design of an adaptive secondary unit for the MMT-Conversion telescope mmt转换望远镜自适应二次单元的初步机械设计
Adaptive Optics Pub Date : 1900-01-01 DOI: 10.1364/adop.1995.tua33
C. Vecchio, W. Gallieni, P. Salinari, P. Gray
{"title":"Preliminary mechanical design of an adaptive secondary unit for the MMT-Conversion telescope","authors":"C. Vecchio, W. Gallieni, P. Salinari, P. Gray","doi":"10.1364/adop.1995.tua33","DOIUrl":"https://doi.org/10.1364/adop.1995.tua33","url":null,"abstract":"The potential advantages of using the secondary mirror of a telescope to perform adaptive correction of the wave front distorted by propagation through the atmosphere are known for long time. Among them are the drastic reduction of the number of optical surfaces, that increases the transmission and reduces the emissivity, and the possibility of providing adaptive corrections to different focal stations. The reduced emissivity makes adaptive secondary mirrors particularly attractive for work at infrared wavelengths where thermal background is of concern, provided that the design of the unit doesn’t affect emissivity in other ways (e. g., with high emissivity surfaces surrounding the secondary). Another desirable feature of an adaptive secondary (AS) is the capability of providing, in addition to wave front correction with many degrees of freedom, also a large (> 0.1 mm) range of motion to perform “chopping”, that is useful for sky subtraction even with modern two dimensional IR detectors. A conceptual approach to the design of an AS with the above features (+) was followed by a variety of studies and experiments that are still in progress (Bruns et al., Biasi et al., Biliotti et al., in this Conference). This paper reports the results of a preliminary study of the various problems related to the general layout, to the support of the optics and to the thermal aspects, in the specific case of the secondary mirror unit for the F/15 Cassegrain focus of the MMT Conversion telescope.","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":"114280483","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}
引用次数: 12
All-Optical Adaptive Systems: Nonlinear Optics Approach for Phase Distortion Suppression 全光自适应系统:相位畸变抑制的非线性光学方法
Adaptive Optics Pub Date : 1900-01-01 DOI: 10.1364/adop.1996.afa.4
M. Vorontsov
{"title":"All-Optical Adaptive Systems: Nonlinear Optics Approach for Phase Distortion Suppression","authors":"M. Vorontsov","doi":"10.1364/adop.1996.afa.4","DOIUrl":"https://doi.org/10.1364/adop.1996.afa.4","url":null,"abstract":"Recent studies of nonlinear optical systems with two-dimensional (2D) feedback have led to the possibility of a new type of adaptive optical system having extremely high spatial resolution for wavefront distortion suppression - the All-Optical Adaptive (AOA) system [1-3]. Presently, dynamic phase distortion suppression is achieved through one of three basic techniques:","PeriodicalId":256393,"journal":{"name":"Adaptive Optics","volume":"487 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":"116192662","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}
引用次数: 0
Intensity peak tracking in extended-object astronomical imaging 扩展目标天文成像中的强度峰值跟踪
Adaptive Optics Pub Date : 1900-01-01 DOI: 10.1364/adop.1996.awd.5
D. Tyler
{"title":"Intensity peak tracking in extended-object astronomical imaging","authors":"D. Tyler","doi":"10.1364/adop.1996.awd.5","DOIUrl":"https://doi.org/10.1364/adop.1996.awd.5","url":null,"abstract":"Adaptive optics are becoming more common at astronomical facilities. At sites such as Mauna Kea, near-IR seeing can be good enough that aberration power is largely confined to tip-tilt, even with larger telescopes. Accordingly, many low-order systems are being planned and studied, with simple tilt compensation schemes being used at several observatories [1,2,3] for near-IR imaging. Image motion can also be removed in post­detection processing if an ensemble of short-exposure images is collected. For either real-time or post­detection processing, proper choice of a tilt removal scheme can improve resolution in long-exposure images.","PeriodicalId":256393,"journal":{"name":"Adaptive Optics","volume":"29 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":"125260028","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}
引用次数: 0
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