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Space Optics for Astrophysics and Earth and Planetary Remote Sensing最新文献

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Stellar Interferometer Design for Minimizing Polarization-Induced Visibility Losses 最小偏振能见度损失的恒星干涉仪设计
Space Optics for Astrophysics and Earth and Planetary Remote Sensing Pub Date : 1900-01-01 DOI: 10.1364/soa.1988.tua4
W. Traub
{"title":"Stellar Interferometer Design for Minimizing Polarization-Induced Visibility Losses","authors":"W. Traub","doi":"10.1364/soa.1988.tua4","DOIUrl":"https://doi.org/10.1364/soa.1988.tua4","url":null,"abstract":"The effects of non-normal-incidence optical phase shifts at the surfaces of mirrors in the arms of stellar interferometers are considered. An explicit expression is given for the wavelength-dependant loss in fringe visibility which results from measureable phase shifts between the perpendicular and parallel reflected components of unpolarized radiation. This loss occurs as a result of the generally different reflection to-pologies in the various arms of an interferometer. An optical design method is presented which eliminates these potentially degrading effects. This method essentially says that the radiation in each arm should experience reflections having the same sequence of direction cosines between the point where the beam is divided and the point where it is combined. We also show that other useful properties of interferometers are obtained by following this rule. Wavelength-dependent phase-shift measurements on real mirrors are presented, allowing numerical evaluation of the degradation factor for any optical configuration. Various optical configurations are shown to illustrate the effect, including new COSMIC (Coherent Optical System of Modular Interferometric Collectors) designs.","PeriodicalId":184695,"journal":{"name":"Space Optics for Astrophysics and Earth and Planetary Remote Sensing","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":"128906979","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
Ground-Based Multipurpose 1.5m Telescope System for Space Optics 陆基多用途1.5m空间光学望远镜系统
Space Optics for Astrophysics and Earth and Planetary Remote Sensing Pub Date : 1900-01-01 DOI: 10.1364/soa.1991.mf12
T. Aruga, T. Itabe, N. Hiromoto, H. Takami, T. Aoki, M. Toyoda, H. Kunimori, W. Smith, J. E. Kimbrell, D. Duggins
{"title":"Ground-Based Multipurpose 1.5m Telescope System for Space Optics","authors":"T. Aruga, T. Itabe, N. Hiromoto, H. Takami, T. Aoki, M. Toyoda, H. Kunimori, W. Smith, J. E. Kimbrell, D. Duggins","doi":"10.1364/soa.1991.mf12","DOIUrl":"https://doi.org/10.1364/soa.1991.mf12","url":null,"abstract":"A new optical system with a 1.5 m diameter telescope for multiple studies was designed and has been under construction for three years at CRL. Now the construction is almost complete and it is in the phase of operation. In this paper, we will introduce the outline of the new optical system for space optics and report several important results of preliminary experiments.","PeriodicalId":184695,"journal":{"name":"Space Optics for Astrophysics and Earth and Planetary Remote Sensing","volume":"72 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":"132070804","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
A Triple Fabry-Perot Spectrometer for the Far Infrared 用于远红外的三重法布里-珀罗光谱仪
Space Optics for Astrophysics and Earth and Planetary Remote Sensing Pub Date : 1900-01-01 DOI: 10.1364/soa.1988.wd2
H. Pickett
{"title":"A Triple Fabry-Perot Spectrometer for the Far Infrared","authors":"H. Pickett","doi":"10.1364/soa.1988.wd2","DOIUrl":"https://doi.org/10.1364/soa.1988.wd2","url":null,"abstract":"A Far Infrared Limb Observing Spectrometer (FILOS) is being developed for observations of OH and other upper atmospheric species. It uses three Fabry-Perot etalons in series to obtain resolution of 1 part in 100,000 at a wavelength of 100 microns. The largest of the three etalons is placed between the telescope and the atmosphere and has dimensions of 10 cm. The smaller two etalons are cooled to 4 K and function to filter out a single order of the large Fabry-Perot resonator. A Triple Fabry-Perot spectrometer is a very simple and effective way of obtaining high resolution spectra of atmospheric emission. Versions are being developed for balloon observations and are being proposed as part of the Earth Observing System for the Polar Orbiting Platform or for the Manned Space Station. Current methods of fabrication and testing the etalons will be described, along with measured and projected performance.","PeriodicalId":184695,"journal":{"name":"Space Optics for Astrophysics and Earth and Planetary Remote Sensing","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":"126781393","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
First-Order Optical Design Considerations for Spaced-Based Array Telescopes 空间阵列望远镜的一阶光学设计考虑
Space Optics for Astrophysics and Earth and Planetary Remote Sensing Pub Date : 1900-01-01 DOI: 10.1364/soa.1988.wb9
E. Hochberg, N. Page
{"title":"First-Order Optical Design Considerations for Spaced-Based Array Telescopes","authors":"E. Hochberg, N. Page","doi":"10.1364/soa.1988.wb9","DOIUrl":"https://doi.org/10.1364/soa.1988.wb9","url":null,"abstract":"For the purpose of comparing the various optical design approaches for a space-based array telescope, the following performance goals will be used: The UV operational goal is motivated by the desire to obtain information inaccessible to the ground based astronomer while the 30 meter baseline obtains from the desire for milliarc-second class angular resolution;","PeriodicalId":184695,"journal":{"name":"Space Optics for Astrophysics and Earth and Planetary Remote Sensing","volume":"38 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":"121705541","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
Theoretical Analysis of Two Off-Axis Parabolic Mirrors for Solar Physics Applications 两个离轴抛物面镜在太阳物理应用中的理论分析
Space Optics for Astrophysics and Earth and Planetary Remote Sensing Pub Date : 1900-01-01 DOI: 10.1364/soa.1991.me1
T. Saha, D. Leviton
{"title":"Theoretical Analysis of Two Off-Axis Parabolic Mirrors for Solar Physics Applications","authors":"T. Saha, D. Leviton","doi":"10.1364/soa.1991.me1","DOIUrl":"https://doi.org/10.1364/soa.1991.me1","url":null,"abstract":"The SUMER - Solar Ultraviolet Measurements of Emitted Radiation - instrument will be flown on the SOHO mission. The instrument will study the upper atmosphere of the sun in the 600 Å -1600 Å wavelength region. The SUMER instrument consists of an off-axis paraboloid followed by a slit, off-axis collimating paraboloid, scan mirror, grating, and a detector. The design parameters for the rectangular SUMER telescope mirror are listed in Table I.","PeriodicalId":184695,"journal":{"name":"Space Optics for Astrophysics and Earth and Planetary Remote Sensing","volume":"60 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":"121829773","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
Cross-Dispersed IR Spectrometer for Atmospheric Sounding 大气探测用交叉分散红外光谱仪
Space Optics for Astrophysics and Earth and Planetary Remote Sensing Pub Date : 1900-01-01 DOI: 10.1364/soa.1988.thb2
R. Pagano, A. Vaughan
{"title":"Cross-Dispersed IR Spectrometer for Atmospheric Sounding","authors":"R. Pagano, A. Vaughan","doi":"10.1364/soa.1988.thb2","DOIUrl":"https://doi.org/10.1364/soa.1988.thb2","url":null,"abstract":"Accurate knowledge of the Earth's vertical atmospheric temperature structure is fundamental to numerical weather prediction. The National Weather Services (NWS) have stated an ultimate goal for temperature measurement of 1 degree accuracy and 1 km vertical resolution throughout the troposphere. To approach this goal next generation temperature sounders must have increased spectral coverage and increased spectral resolution. Extensive simulations indicate that a temperature sounder with spectral resolving power (λ/Δλ) of 1200 and wavelength coverage from 3.4 - 17.0 µm will significantly improve the rms temperature retrieval accuracy.","PeriodicalId":184695,"journal":{"name":"Space Optics for Astrophysics and Earth and Planetary Remote Sensing","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":"125271742","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
On the Threshold: Astrometric Optical Interferometry in Space with POINTS 论阈值:空间点阵天文光学干涉测量
Space Optics for Astrophysics and Earth and Planetary Remote Sensing Pub Date : 1900-01-01 DOI: 10.1364/soa.1988.tub2
R. D. Reasenberg
{"title":"On the Threshold: Astrometric Optical Interferometry in Space with POINTS","authors":"R. D. Reasenberg","doi":"10.1364/soa.1988.tub2","DOIUrl":"https://doi.org/10.1364/soa.1988.tub2","url":null,"abstract":"POINTS (Precision Optical INTerferometry in Space) would measure the angular separation of two stars, separated by about 90 deg on the sky, with a nominal measurement error of 5 microarcseconds (μas). See Figure 1 for an artist’s rendition of the instrument mounted on the NASA MMS. A discussion of some astrophysical applications of POINTS is given by Reasenberg et al. (1988) and in less detail by Reasenberg (1984). For a pair of mag 10 stars, an observation would require about 10 minutes; the instrument would measure daily the separation of two stars for each of about 60 pairs of stars. A random sequence of such measurements, if suitably redundant, contains the closure information necessary to detect and correct time-dependent measurement biases to well below the nominal measurement accuracy. The 90 deg target separation permits absolute parallax to be determined, obviating the need for adjacent zero-parallax objects and making possible parallax measurements in all directions.","PeriodicalId":184695,"journal":{"name":"Space Optics for Astrophysics and Earth and Planetary Remote Sensing","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":"133754594","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
Telescope Array Performance in the Optical Limit 光学极限下的望远镜阵列性能
Space Optics for Astrophysics and Earth and Planetary Remote Sensing Pub Date : 1900-01-01 DOI: 10.1364/soa.1988.wb10
Maj Steven M. Watson, J. Mills
{"title":"Telescope Array Performance in the Optical Limit","authors":"Maj Steven M. Watson, J. Mills","doi":"10.1364/soa.1988.wb10","DOIUrl":"https://doi.org/10.1364/soa.1988.wb10","url":null,"abstract":"Many astrophysical observations require large diameter space borne optics. Because of the limited space and weight requirements for boost into orbit and manufacturing limitations, large diamteter optics pose a problem. Multi-aperture optical systems may provide a solution. This theoretical analysis examined many multi-aperture systems (Figure 1) and determined that multi-aperture systems composed of 19, 37, 61, and 91 apertures could provide impulse responses (displayed in Figure 2) which were superior to that of a single large optic of an equivalent diameter. The multi-aperture systems were superior in the sense that the secondary lobe irradiance maxima of these systems was less than 0.0175, the secondary lobe irradiance of the single large aperture. In all cases, the central lobe widths of the impulse responses were equal to that of the single large aperture of equivalent diameter. The addition of obstructions which covered the central portion of each aperture (to simulate a Cassegrain telescope system) caused the secondary lobe irradiance maxima to be reduced further for the 19 and 19 (rotated) aperture systems. Figure 3 displays the results of this analysis. For obscured and unobscured cases, the 19 (rotated) aperture system exhibited the lowest side lobes.","PeriodicalId":184695,"journal":{"name":"Space Optics for Astrophysics and Earth and Planetary Remote Sensing","volume":"5 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":"129092526","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
Point-to-Point Laser Metrology for POINTS 点对点激光测量
Space Optics for Astrophysics and Earth and Planetary Remote Sensing Pub Date : 1900-01-01 DOI: 10.1364/soa.1988.tub4
J. Phillips, R. D. Reasenberg
{"title":"Point-to-Point Laser Metrology for POINTS","authors":"J. Phillips, R. D. Reasenberg","doi":"10.1364/soa.1988.tub4","DOIUrl":"https://doi.org/10.1364/soa.1988.tub4","url":null,"abstract":"The Precision Optical INTerferometer in Space (POINTS) is an astrometric instrument comprising a metrology system and two starlight interferometers mounted at an angle ϕ ≈ 90 deg. This angle, which must be measured with an uncertainty small compared to the nominal instrument accuracy of 5 microarcseconds (μas), is determined by measuring the six distances among four fiducial points, two for each interferometer. The fiducial points are connected to the starlight optics via Full Aperture Metrology (Babcock et al., in this Digest; Reasenberg, in this Digest). Because of the observing geometry, the uncorrelated part of the error in the distance measurements must be held to a few picometers (pm). In this paper, we consider a new, “two color” laser gauge that appears to meet the requirements of POINTS. We are developing a test version of such a gauge.","PeriodicalId":184695,"journal":{"name":"Space Optics for Astrophysics and Earth and Planetary Remote Sensing","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":"132826912","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
Space Infrared Telescope Facility 空间红外望远镜设施
Space Optics for Astrophysics and Earth and Planetary Remote Sensing Pub Date : 1900-01-01 DOI: 10.1364/soa.1991.tub1
D. Norris, M. Bothwell, J. Plamondon
{"title":"Space Infrared Telescope Facility","authors":"D. Norris, M. Bothwell, J. Plamondon","doi":"10.1364/soa.1991.tub1","DOIUrl":"https://doi.org/10.1364/soa.1991.tub1","url":null,"abstract":"The Space Infrared Telescope Facility (SIRTF) is the fourth and last Great Observatory of the NASA Astrophysics Program. The challenges in providing this Observatory range from new cryogenic optical and sensing technology to operating in a fixed price research environment.","PeriodicalId":184695,"journal":{"name":"Space Optics for Astrophysics and Earth and Planetary Remote Sensing","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":"115871196","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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