Готові списки джерел за темами / Guide star

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Добірка наукової літератури з теми "Guide star"

Автор: Grafiati
Опубліковано: 10 грудня 2022
Оновлено: 28 січня 2023

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Статті в журналах з теми "Guide star"

1

WADA, Satoshi, and Norihito SAITO. "Laser Guide Star." Review of Laser Engineering 39, no. 1 (2011): 30–33. http://dx.doi.org/10.2184/lsj.39.30.

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2

Thompson, Laird A., Scott W. Teare, Yao-Heng Xiong, Richard M. Castle, Abhijit Chakraborty, Robert A. Gruendl, and Robert W. Leach. "UnISIS: Laser Guide Star and Natural Guide Star Adaptive Optics System." Publications of the Astronomical Society of the Pacific 121, no. 879 (May 2009): 498–511. http://dx.doi.org/10.1086/599574.

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3

Wu, Feng, Xifang Zhu, Ruxi Xiang, Qiuyang Yu, Tingting Huang, Qingquan Xu, and Hui Li. "Novel guide star optimal selection algorithm for star sensors based on star clustering." Modern Physics Letters B 32, no. 34n36 (December 30, 2018): 1840089. http://dx.doi.org/10.1142/s0217984918400894.

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Modern space vehicles face the challenges to obtain more and more accurate attitudes in order to complete the demanding tasks. Onboard star sensors which identify the observed stars in the field of view according to the loaded guide star catalog and output accurate attitude have attracted most interests. Guide stars are usually required to distribute uniformly on the celestial sphere to improve the performance of the star pattern identification. An optimal selection algorithm is proposed to achieve an even distribution of guide stars in this paper. Constellation features are discussed. The mean shift algorithm is analyzed. The idea that distributes stars in the local field of view to constellations is proposed by using the star pair angular separations according to the star positions in the inertial coordinate system. The optimal selection algorithm of guide stars based on star clustering is developed. Its detailed implement procedures are introduced completely. The guide star optimal selection experiment in visible band by using SAO star catalog as the original star data is implemented. It proves that the proposed algorithm has the virtue of simple calculation and easy realization. The obtained guide star distribution is superior to the regression selection algorithm and the magnitude weighted method.
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4

Wu, Feng, Xifang Zhu, Qingquan Xu, Ruxi Xiang, Qiuyang Yu, Jie Zhou, and Xiu Yang. "Optimization of guide star catalog for daytime star sensors." International Journal of Modern Physics B 34, no. 01n03 (December 26, 2019): 2040065. http://dx.doi.org/10.1142/s0217979220400652.

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Daytime star sensor provides accuracy navigation information to air vehicles near the ground in the daytime by observing stars. It has been an important development of modern star sensors. In order to achieve a high signal-to-noise ratio, daytime star sensors work in the infrared band to avoid interferences from sky background. Daytime star sensors output accurate attitudes by identifying the observed stars in the field of view (FOV) according to the loaded guide star catalog. Guide stars are usually required to be distributed uniformly on the celestial sphere to improve the performance of star pattern identification. The parameters including limiting magnitude and FOV are determined by processing the 2MASS star catalog as the original star data and performing star distribution statistics. After constellation features are discussed, the idea of distributing stars in the local FOV to constellations is put forward by using the star pair angular separations. An optimization algorithm to build the guide star catalog for daytime stars is proposed to achieve evenly distributed guide stars. The guide star catalog is established and analyzed, proving that the proposed algorithm has simple calculation and easy realization. The Boltzmann entropy of obtained guide star catalog drops two orders of magnitude. Guide stars are distributed more uniformly.
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5

Li, Jian, Gangyi Wang, and Xinguo Wei. "Generation of Guide Star Catalog for Star Trackers." IEEE Sensors Journal 18, no. 11 (June 1, 2018): 4592–601. http://dx.doi.org/10.1109/jsen.2018.2825355.

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6

Russell, Jane L. "The Guide Star Selection System and the Guide Star Catalog for Space Telescope." Symposium - International Astronomical Union 109 (1986): 721–27. http://dx.doi.org/10.1017/s007418090007724x.

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The Guide Star Selection System (GSSS) will provide relative positions of two guide stars and the target for each observation of the Space Telescope as well as photometry for the guide stars. Being developed at the Space Telescope Science Institute, the GSSS is a production system which is based on PDS measurements of Schmidt survey plates. The specified accuracy for the system is +/−0.33 arcsec for the separation of the guide stars and 0.4 mag in the bandpass of the Space Telescope's Fine Guidance Sensors. The GSSS will produce two catalogs which will be used in the operation of the system. The Guide Star Photometry catalog includes photoelectric measurements (+/−0.05 mag) in B and V for six stars over the guide star range, 9.0 to 14.5 visual magnitude, near the central part of each 6 by 6 deg survey plate. The Guide Star Catalog will include the list of all possible guide stars and brighter, positions (at least +/−1 arcsec) and magnitudes (at least +/−0.4 mag) for essentially the whole sky complete to visual magnitude 15.
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7

Wu, Liang, Qian Xu, Haojing Wang, Hongwu Lyu, and Kaipeng Li. "Guide Star Selection for the Three-FOV Daytime Star Sensor." Sensors 19, no. 6 (March 25, 2019): 1457. http://dx.doi.org/10.3390/s19061457.

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To realize the application of the star sensor in the all-day carrier platform, a three-field-of-view (three-FOV) star sensor in short-wave infrared (SWIR) band is considered. This new prototype employs new techniques that can improve the detection capability of the star sensor, when the huge size of star identification feature database becomes a big obstacle. Hence, a way to thin the guide star catalog for three-FOV daytime star sensor is studied. Firstly, an introduction of three-FOV star sensor and an example of three-FOV daytime star sensor with narrow FOV are presented. According to this model and the requirement of triangular star identification method, two constraints based on the number and the brightness of the stars in FOV are put forward for guide star selection. Then on the basis of these constraints, the improved spherical spiral method (ISSM) is proposed and the optimal number of reference points of ISSM is discussed. Finally, to demonstrate the performance of the ISSM, guide star catalogs are generated by ISSM, magnitude filter method (MFM), 1st order self-organizing guide star selection method (1st-SOPM) and the spherical spiral method (SSM), respectively. The results show that the guide star catalog generated by ISSM has the smallest size and the number and brightness characteristics of its guide stars are better than the other methods. ISSM is effective for the guide star selection in the three-FOV daytime star sensor.
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8

Yang, Xuezong, Ondrej Kitzler, David J. Spence, Zhenxu Bai, Yan Feng, and Richard P. Mildren. "Diamond sodium guide star laser." Optics Letters 45, no. 7 (March 20, 2020): 1898. http://dx.doi.org/10.1364/ol.387879.

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9

Lasker, Barry M., Conrad R. Sturch, Carlos Lopez, Anthony D. Mallamas, Steven F. McLaughlin, Jane L. Russell, Wieslaw Z. Wisniewski, et al. "The Guide Star Photometric Catalog." Astrophysical Journal Supplement Series 68 (September 1988): 1. http://dx.doi.org/10.1086/191282.

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10

McLean, B., G. Hawkins, A. Spagna, M. Lattanzi, B. Lasker, H. Jenkner, and R. White. "The Second Guide Star Catalogue." Symposium - International Astronomical Union 179 (1998): 431–32. http://dx.doi.org/10.1017/s0074180900129225.

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Анотація:
Although the HST GSC–I (Paper-I: Lasker et al. 1990, Paper-II: Russell et al. 1990, Paper-III: Jenkner et al. 1990) has been used with great success operationally, it was always known that it was possible to improve the scientific and operational usefulness by an increase in scope to include multi-color and multi-epoch data. Once the GSC-II concept was established, it was evident that, even beyond the original motivations in HST operations, it would address a number of other astronomical needs such as increasing demands for fainter catalogues to support remote or queue scheduling capabilities and adaptive optics on the next generation of large-aperture, new-technology telescopes. In addition, the all sky nature of the GSC–II makes it a natural data source for research in galactic structure.
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Дисертації з теми "Guide star"

1

Booth, H. J. "Guide star lasers." Thesis, University of Oxford, 1998. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.300872.

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2

Roberts, William Thomas. "Guide star lasers for adaptive optics." Diss., The University of Arizona, 2001. http://hdl.handle.net/10150/290501.

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Exploitation of the imaging capabilities of the new generation of ground-based astronomical telescopes relies heavily on Adaptive Optics (AO). Current AO system designs call for sodium guide star lasers capable of producing at least eight Watts of power tuned to the peak of the sodium D₂ line, with a high duty cycle to avoid saturation, and with 0.5-1.0 GHz spectral broadening. This work comprises development and testing of six candidate laser systems and materials which may afford a path to achieving these goals. An end-pumped CW dye laser producing 4.0 Watts of tuned output power was developed and used to obtain the first accurate measurement of sodium layer scattering efficiency. Methods of optimizing the laser output through improving pump overlap efficiency and reducing the number of intracavity scattering surfaces are covered. The 1181 nm fluorescence peak of Mn⁵⁺ ion in Ba₅(PO₄)₃Cl could be tuned and doubled to reach 589 nm. While efforts to grow this crystal were under way, the Mn⁵⁺ ion in natural apatite (Ca₅(PO₄)₃F) was studied as a potential laser material. Fluorescence saturation measurements and transmission saturation are presented, as well as efforts to obtain CW lasing in natural apatite. A Q-switched laser color-center laser in LiF : F⁻₂ was developed and successfully tuned and doubled to the sodium D₂ line. Broad-band lasing of 80 mW and tuned narrow-band lasing of 35 mW at 1178 nm were obtained with 275 mW of input pump power at 1064 nm. The measured thermal properties of this material indicate its potential for scaling to much higher power. A Q-switched intracavity Raman laser was developed in which CaWO₄ was used to shift a Nd:YAG laser, the frequency-doubled output of which was centered at 589.3 nm. To obtain light at 589.0 nm, a compositionally tuned pump laser of Nd : Y₃Ga₁.₁Al₃.₉O₁₂ was produced which generated the desired shift, but was inhomogeneous broadened, limiting the tunable power of the material. Finally, temperature tuning of a Nd:YAG laser was demonstrated in which the laser emitted up to 8.6 Watts at a temperature of -21.5 C, bringing the wavelength into a regime favorable for efficient Raman shifting by CaWO₄.
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3

Sereni, Giulia. "Optical design of MAORY Laser Guide Star Objective." Master's thesis, Alma Mater Studiorum - Università di Bologna, 2017. http://amslaurea.unibo.it/14069/.

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The turbulence affects the angular resolution of images. Single Conjugate Adaptive optics, SCAO, is the simplest way to correct the atmospheric turbulence using a Natural Guide Star, but it has some limitations such as the anisoplanatism. Multi Conjugate Adaptive Optics is a technique which overcomes this issue by using as many NGSs, as Wavefront Sensors. In order to increase the sky coverage, Laser Guide Stars, LGSs, are also used. One of the first light instrument of the 40 meter European Extremely Large Telescope is MICADO, or the Multi-Adaptive Optics Imaging Camera for Deep Observations. It works with the post-focal MCAO relay, called MAORY, which uses six LGSs. A description of MAORY optical design is provided in this thesis. These LGSs suffer from aberrations and thus, after separating the light by a dichroic, an objective is designed to reduce these aberrations. In fact, since during sky tracking the zenith angle changes, the six LGSs launched at the Sodium layer vary their distances from the telescope primary mirror. As a consequence, the LGSs at different distances will focus on different positions along the optical axis. Through the procedure of optimization one can improve or modify the design in order to reduce or remove aberrations. Since no component can be perfectly manufactured and aligned, a tolerance analysis is important to ensure that the final, assembled instrument meets the requested performance. All in all, the goal of this thesis is to optimize and perform the tolerance analysis for the LGS Objective of MAORY and show the results. The mechanical constraints and the variations of the aberrations with the zenith and azimuthal angle are taken into account. The number of optical surfaces has been minimized keeping the LGS Objective requirements satisfied. Moreover, the residual aberrations of the LGSs have been kept as small as possible in order to reach the performance requirements of MAORY. The software Zemax has been used.
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4

Hart, Michael, Stuart Jefferies, and Neil Murphy. "Daylight operation of a sodium laser guide star." SPIE-INT SOC OPTICAL ENGINEERING, 2016. http://hdl.handle.net/10150/622016.

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We report photometric measurements of a sodium resonance guide star against the daylight sky when observed through a tuned magneto-optical filter (MOF). The MOF comprises a sodium vapor cell in a kilogauss-level magnetic field between crossed polarizers and has a very narrow transmission profile at the sodium D-2 resonance of approximately 0.008 nm. Our observations were made with the 1.5 m Kuiper telescope on Mt. Bigelow, AZ, which has a separately mounted guide star laser projecting a circularly polarized single-frequency beam of approximately 6.5 W at 589.16 nm. Both the beam projector and the 1.5 m telescope were pointed close to zenith; the baseline between them is approximately 5 m. Measurements of the guide star were made on the morning of 2016 March 24 using an imaging camera focused on the beacon and looking through the full aperture of the telescope. The guide star flux was estimated at 1.20x10(6) photon/m(2)/s while at approximately 45 minutes after sunrise, the sky background through the MOF was 1100 photon/m(2)/s/arcsec(2). We interpret our results in terms of thermal infrared observations with adaptive optics on the next generation of extremely large telescopes now being built.
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5

Jacobsen, Bruce Paul 1964. "Sodium laser guide star projection for adaptive optics." Diss., The University of Arizona, 1997. http://hdl.handle.net/10150/288754.

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In order to increase sky coverage, adaptive optics (AO) systems for large telescopes will require laser systems to provide artificial reference beacons. The most prominent method for creating an artificial beacon is to project laser light tuned to the 589nm, D2 line of sodium onto the mesospheric sodium atoms at an altitude of 90km. When correcting with AO, the best wavefront measurements are obtained when the image of the sodium beacon is as bright and sharp as possible. Blurring occurs due to spot elongation, as a result of sub-aperture displacement from the projector axis, and from diffraction and seeing effects on the projected beam. Mounting the projector in the center of the telescope minimizes the effect of elongation. Simulations were conducted that show that matching the beam waist to ∼2 times the atmospheric turbulence parameter r₀ minimizes the beacon size. For r₀ = 15cm and a 48cm projector, calculations show the optimum projected waist is 29cm. A prototype projector has been built and operated. Recent experiments have shown that this projector is capable of producing 0.75arcsec beacons under good seeing. In addition, spot elongation of 0.5arcsec was observed corresponding to a sodium layer thickness of 10km. The first experimental evidence for optical pumping in the mesospheric layer were obtained. They show a non-thermal profile for the sodium hyperfine structure (3.5:1 line ratio as opposed to 5:3) when projecting circularly polarized light. This profile indicates that the maximum return per watt is obtained by pumping the F = 2 level with a narrow bandwidth compared with pumping both F = 2 and F = 1 with a broad bandwidth. In addition, evidence shows a 30% increase in beacon brightness when pumping the sodium layer with circularly polarized light over linear. A projector for the 6.5m MMT conversion has been designed based on experience gained with the prototype. Analysis of the Strehl reduction due to wavefront reconstruction error shows a reduction in Strehl of < 1% for the optimal operating parameters at the MMT. This less than the fundamental limit of 0.79 for focus anisoplanatism.
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6

Reeves, Andrew Paul. "Laser Guide Star only adaptive optics : the development of tools and algorithms for the determination of Laser Guide Star tip-tilt." Thesis, Durham University, 2015. http://etheses.dur.ac.uk/11199/.

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Adaptive Optics (AO) is a technology which corrects for the effects of the atmosphere and so improves the optical quality of ground based astronomical observations. The bright “guide stars” required for correction are not available across the entire sky, so Laser Guide Stars (LGSs) are created. A Natural Guide Star (NGS) is still required to correct for tip-tilt as the LGS encounters turbulence on the uplink path resulting in unpredictable “jitter”, hence limiting corrected sky coverage. In this thesis an original method is proposed and investigated that promises to improve the correction performance for tomographic AO systems using only LGSs, and no NGS, by retrieving the LGS uplink tip-tilt. To investigate the viability of this method, two unique tools have been developed. A new AO simulation has been written in the Python programming language which has been designed to facilitate the rapid development of new AO concepts. It features realistic LGS simulation, ideal to test the method of LGS uplink tip-tilt retrieval. The Durham Real-Time Adaptive Optics Generalised Optical Nexus (DRAGON) is a laboratory AO test bench nearing completion, which features multiple LGS and NGS Wavefront Sensors (WFSs) intended to further improve tomographic AO. A novel method of LGS emulation has been designed, which re-creates focus anisoplanatism, elongation and uplink turbulence. Once complete, DRAGON will be the ideal test bench for further development of LGS uplink tip-tilt retrieval. Performance estimates from simulation of the LGS uplink tip-tilt retrieval method are presented. Performance is improved over tomographic LGS AO systems which do not correct for tip-tilt, giving a modest improvement in image quality over the entire night sky. Correction performance is found to be dependent on the atmospheric turbulence profile. If combined with ground layer adaptive optics, higher correction performance with a very high sky coverage may be achieved.
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7

Hart, Michael, Stuart Jefferies, and Douglas Hope. "Tomographic wave-front sensing with a single guide star." SPIE-INT SOC OPTICAL ENGINEERING, 2016. http://hdl.handle.net/10150/622717.

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Adaptive optics or numerical restoration algorithms that restore high resolution imaging through atmospheric turbulence are subject to isoplanatic wave-front errors. Mitigating those errors requires that the wave-front aberrations be estimated within the 3D volume of the atmosphere. Present techniques rely on multiple beacons, either natural stars or laser guide stars, to probe the atmospheric aberration along different lines of sight, followed by tomographic projection of the measurements onto layers at defined ranges. In this paper we show that a three-dimensional estimate of the wave-front aberration can be recovered from measurements by a single guide star in the case where the aberration is stratified, provided that the telescope tracks across the sky with non-uniform angular velocity. This is generally the case for observations of artificial earth-orbiting satellites, and the new method is likely to find application in ground based telescopes used for space situational awareness.
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8

Czarske, J., H. Radner, and L. Büttner. "Adaptive interferometric velocity measurements using a laser guide star." SPIE, 2015. https://tud.qucosa.de/id/qucosa%3A35038.

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We have harnessed the power of programmable photonics devices for an interferometric measurement technique. Laser interferometers are widely used for flow velocity measurements, since they offer high temporal and spatial resolutions. However, often optical wavefront distortions deteriorate the measurement properties. In principle, adaptive optics enables the correction of these disturbances. One challenge is to generate a suitable reference signal for the closed loop operation of the adaptive optics. An adaptive Mach Zehnder interferometer is presented to measure through a dynamic liquid-gas phase boundary, which can lead to a misalignment of the interfering laser beams. In order to generate the reference signal for the closed loop control, the Fresnel reflex of the phase boundary is used as Laser Guide Star (LGS) for the first time to the best of the authors’ knowledge. The concept is related to the generation of artificial stars in astronomy, where the light transmitted by the atmosphere is evaluated. However, the adaptive interferometric flow velocity measurements at real world experiments require a different concept, since only the reflected light can be evaluated. The used LGS allows to measure the wavefront distortions induced by the dynamic phase boundary. Two biaxial electromagnetically driven steering mirrors are employed to correct the wavefront distortions. This opens up the possibility for accurate flow measurements through a dynamic phase boundary using only one optical access. Our work represents a paradigm shift in interferometric velocity measurement techniques from using static to dynamic optical elements.
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9

Ge, Jian 1966. "Sodium laser guide star technique, spectroscopy and imaging with adaptive optics." Diss., The University of Arizona, 1998. http://hdl.handle.net/10150/282740.

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A sodium laser guide star (LGS) adaptive optics (AO) system developed at Stewart Observatory is to be used at the 6.5m MMT. Annual measurements at Kitt Peak show that the mean mesospheric sodium column density varies from ∼2x10⁹cm⁻² (summer) to ∼5x10⁹cm⁻² (winter). The sodium column density also varies by a factor of two during a one hour period. The first simultaneous measurements of sodium LGS brightness, sodium column density and laser power were obtained. The absolute sodium return for a continuous wave circularly polarized beam is 1.2(±0.3)x10⁶ photons s⁻¹m⁻²W⁻¹ for the sodium column density of 3.7x10⁹cm⁻². Theoretical studies demonstrate that the 6.5m MMT LGS AO can provide Strehl ratios better than 0.15 and about 50% flux concentration within 0.2" aperture for 1-5.5μm under median seeing. This correction will be available for the full sky. Better Strehl and higher flux concentration can be achieved with natural guide stars, but limited sky coverage. The AO corrected field-of-view is about 60". The Arizona IR Imager and Echelle Spectrograph (ARIES) was designed to match the 6.5m MMT AO. Detection limits of more than 2 magnitude fainter can be reached with the AO over without the AO. A pre-ARIES wide field near-IR camera was designed, built and tested. The camera provides 1" images in the near-IR over an 8.5 x 8.5arcmin² field. The 10-σ detection limit with one minute exposures is 17.9 mag. in the K band. A prototype very high resolution cross-dispersed optical echelle spectrograph was designed and built to match the Starfire Optical Range 1.5m AO images. Interstellar KI 7698Å absorption lines have been detected in the spectra of αCyg and ζPer. The spectral resolution is 250.000. About 300Å wavelengths were covered in a single exposure. Total detection efficiency of 1% has been achieved. For the first time, a near-single-mode fiber with 10μm core size was applied to transmit the Mt. Wilson 100inch AO corrected beams to a spectrograph. The coupling efficiency of the fiber reached up to 70%. Spectra of αOri were recorded. The spectral resolution is 200,000. The total wavelength coverage is about 650Å per exposure.
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10

Moldovan, Ioana Cristina. "Étude photométrique de l’atome de sodium : application aux étoiles lasers (LGS ET PLGS)." Grenoble 1, 2008. http://www.theses.fr/2008GRE10060.

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Анотація:
Pour corriger la dégradation des images astronomiques due aux turbulences atmosphériques, les astronomes ont proposé de créer une étoile laser dans la haute atmosphère. Cette thèse a pour objectif l'étude théorique et expérimentale au laboratoire des différents processus d'excitation du sodium mésosphérique pour obtenir une source monochromatique et polychromatique, afin d'estimer avec précision le flux retourné d'une expérience sur le ciel. Les deux premières parties sont consacrées au contexte scientifique à l'interface entre la physique et l'astronomie, et à la description de diverses propriétés de l'atome de sodium, ainsi qu'à deux études portant sur les propriétés de polarisation de la fluorescence de Na. L'étude du laser sans mode UV, développé au LSP, est ensuite réalisée. La partie suivante décrit en détail l'expérience de photométrie ainsi que la mesure des paramètres nécessaires comme les profils spatiaux, temporels et spectraux du laser, ainsi que la densité de sodium. Enfin, on présente le développement d'un modèle cinétique (REM) de l'excitation du sodium utilisant des équations de taux dans plusieurs cas: excitation à un photon à 589 nm, excitation à un photon à 330 nm et excitation à deux photons résonants ou non résonants. Un très bo accord avec le code BEA CON et les résultats expérimentaux confirme la validité de ce modèle. A l'aide du code REM, les différentes méthodes sont comparées et l'efficacité de l'excitation du sodium mésosphérique est calculée. Ce travail montre que, dans les meilleures conditions et pour les puissances laser envisagées dans le projet ELPOA actuel, le flux retourné à 330 nm ne dépassera pas 5x104 photons/m2/s
Ln order to correct the astronomical images degradation due to the atmospheric turbulences, the astronomers propose to create a laser guide star in the high atmosphere. The purpose of this thesis is to study experimentally and theoretically in the laboratory different mesospheric sodium excitation methods to obtain a monochromatic and a polychromatic source, to choose the most appropriate solution, and to estimate accurately the returned flux of an experiment to the sky. The first two parts of this report describe respectively the scientific context which is at the interface of physics and astronomy, and several properties of the sodium atom as weIl as two theoretical and experimental studies about the polarisation properties of the Na fluorescence. The study of the UV modeless laser developed at LSP is presented. The next part explains precisely the photometry experiment and also the measurement of the needed parameters, such as spatial, temporal and spectral laser profiles and the atomic density. At last, we present the development of a kinetic model (called REM) of the sodium excitation via the rate equations in several cases: one photon excitation at 589 nm, one photon excitation at 330 nm, and two-resonant-or-non-resonant-photons excitation. A very good agreement with the BEACON code and the experimental results confirms the validity of this model. Thanks to REM code, the different methods are compared and the mesospheric sodium excitation efficiency is calculated. This work shows that in the best case and for the present ELP-OA project lasers power, the returned flux at 330 nm is around 5 x 104 photons/m2/s
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Книги з теми "Guide star"

1

ill, Eagle Ellen, ed. Star guide. New York: T.Y. Crowell, 1987.

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2

Shining star: Assessment guide. White Plains, N.Y: Longman, 2004.

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3

Friedman, Michael Jan. Star trek Federation travel guide. New York: Pocket Books, 1997.

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4

Snyder, Jeffrey B. A trekker's guide to collectibles with price guide. Atglen, PA: Schiffer Pub., 1996.

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5

Inglis, Mike. Observer's guide to star clusters. New York: Springer, 2013.

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6

Arnold, J. Douglas, Mark Elies, and Keahi Freeland. Star Fox 64: Survival Guide. Maui, USA: Sandwich Islands Publishing, 1998.

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7

Lease, Wayne. Texas forts: Lone Star guide. Garland, Tex: Texas Forts Distributors, 2001.

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8

Inglis, Mike. Observer’s Guide to Star Clusters. New York, NY: Springer New York, 2013. http://dx.doi.org/10.1007/978-1-4614-7567-5.

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9

Star Wars: Guide des personnages. Paris]: Éditions Pages ouvertes, 2015.

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10

Kerrod, Robin. The star guide: Learn how to read the night sky star by star. New York: Prentice Hall General Reference, 1993.

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Частини книг з теми "Guide star"

1

Max, C. E. "Laser Guide Star Operational Issues." In Laser Guide Star Adaptive Optics for Astronomy, 89–106. Dordrecht: Springer Netherlands, 2000. http://dx.doi.org/10.1007/978-94-015-9624-4_5.

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2

Mclean, B., G. Hawkins, A. Spagna, M. Lattanzi, B. Lasker, H. Jenkner, and R. White. "The Second Guide Star Catalogue." In New Horizons from Multi-Wavelength Sky Surveys, 431–32. Dordrecht: Springer Netherlands, 1997. http://dx.doi.org/10.1007/978-94-009-1485-8_108.

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3

Inglis, Michael David. "Star Clusters." In Field Guide to the Deep Sky Objects, 115–200. London: Springer London, 2001. http://dx.doi.org/10.1007/978-1-4471-3680-4_3.

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4

Federman, David. "Star Ruby." In Modern Jeweler’s Consumer Guide to Colored Gemstones, 174–77. Boston, MA: Springer US, 1990. http://dx.doi.org/10.1007/978-1-4684-6488-7_42.

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5

Federman, David. "Star Sapphire." In Modern Jeweler’s Consumer Guide to Colored Gemstones, 202–5. Boston, MA: Springer US, 1990. http://dx.doi.org/10.1007/978-1-4684-6488-7_49.

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6

Smart, R. L., D. Carollo, M. G. Lattanzi, B. McLean, and A. Spagna. "The Second Guide Star Catalogue and Cool Stars." In Ultracool Dwarfs, 119–24. Berlin, Heidelberg: Springer Berlin Heidelberg, 2001. http://dx.doi.org/10.1007/978-3-642-56672-1_11.

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7

Inglis, Mike. "Beginnings—Star Birth." In Observer’s Guide To Stellar Evolution, 69–119. London: Springer London, 2003. http://dx.doi.org/10.1007/978-1-4471-0059-1_2.

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8

Russell, Jane L. "The Guide Star Selection System and the Guide Star Catalog for Space Telescope." In Astrometric Techniques, 721–27. Dordrecht: Springer Netherlands, 1986. http://dx.doi.org/10.1007/978-94-009-4676-7_90.

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9

Rodríguez-González, J. M., J. J. Fuensalida, and J. M. Rodríguez-Ramos. "Laser Guide Star for Segmented Telescopes." In Highlights of Spanish Astrophysics II, 313–16. Dordrecht: Springer Netherlands, 2001. http://dx.doi.org/10.1007/978-94-017-1776-2_73.

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10

Inglis, Mike. "The End Point — Star Death." In Observer’s Guide To Stellar Evolution, 169–214. London: Springer London, 2003. http://dx.doi.org/10.1007/978-1-4471-0059-1_4.

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Тези доповідей конференцій з теми "Guide star"

1

Foy, Renaud, Michel Tallon, Herbert W. Friedman, Andre Baranne, Francois Biraben, Gilbert Grynberg, Miska Le Louarn, et al. "Polychromatic guide star." In High-Power Laser Ablation, edited by Claude R. Phipps. SPIE, 1998. http://dx.doi.org/10.1117/12.321566.

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2

Yang, Xuezong, Ondrej Kitzler, David J. Spence, Zhenxu Bai, Yan Feng, and Richard P. Mildren. "Diamond Sodium Guide Star Laser." In Conference on Lasers and Electro-Optics/Pacific Rim. Washington, D.C.: OSA, 2020. http://dx.doi.org/10.1364/cleopr.2020.c7a_1.

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3

Foy, Renaud. "Polychromatic guide star: feasibility study." In High-Power Laser Ablation III. SPIE, 2000. http://dx.doi.org/10.1117/12.407359.

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4

Bonaccini, Domenico, Eric Allaert, Constanza Araujo, Enzo Brunetto, Bernard Buzzoni, Mauro Comin, Martin J. Cullum, et al. "VLT laser guide star facility." In Astronomical Telescopes and Instrumentation, edited by Peter L. Wizinowich and Domenico Bonaccini. SPIE, 2003. http://dx.doi.org/10.1117/12.459277.

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5

Clare, Richard M., Marcos A. van Dam, and Antonin H. Bouchez. "Modeling Laser Guide Star Aberrations." In Adaptive Optics: Methods, Analysis and Applications. Washington, D.C.: OSA, 2007. http://dx.doi.org/10.1364/aopt.2007.atub5.

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6

Wu, Feng, Ruxi Xiang, Qingquan Xu, Jie Zhou, and Xiu Yang. "Study on guide star selection for infrared star sensors." In SPIE Future Sensing Technologies, edited by Christopher R. Valenta and Masafumi Kimata. SPIE, 2019. http://dx.doi.org/10.1117/12.2542602.

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7

De La Rue, Imelda A., and Brent L. Ellerbroek. "Multiple guide stars to improve the performance of laser guide star adaptive optical systems." In Astronomical Telescopes & Instrumentation, edited by Domenico Bonaccini and Robert K. Tyson. SPIE, 1998. http://dx.doi.org/10.1117/12.321723.

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8

Pennington, D. M., J. W. Dawson, A. Drobshoff, S. Mitchell, and A. Brown. "Advanced Sodium Guide Star Technology Development." In Frontiers in Optics. Washington, D.C.: OSA, 2006. http://dx.doi.org/10.1364/fio.2006.fwl2.

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9

Lombini, Matteo. "Laser Guide Star Objective of MAORY." In Adaptive Optics for Extremely Large Telescopes 5. Instituto de Astrofísica de Canarias (IAC), 2017. http://dx.doi.org/10.26698/ao4elt5.0056.

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10

Boyer, C., B. Ellerbroek, L. Gilles, and L. Wang. "The TMT Laser Guide Star Facility." In 1st AO4ELT conference - Adaptive Optics for Extremely Large Telescopes. Les Ulis, France: EDP Sciences, 2010. http://dx.doi.org/10.1051/ao4elt/201004004.

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Звіти організацій з теми "Guide star"

1

Lehman, S. Wave-Based Subsurface Guide Star. Office of Scientific and Technical Information (OSTI), July 2011. http://dx.doi.org/10.2172/1022929.

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2

Powell, Richard C. DURIP-97 Sodium Guide Star Raman Laser. Fort Belvoir, VA: Defense Technical Information Center, April 2000. http://dx.doi.org/10.21236/ada378796.

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3

Max, C., D. Gavel, H. Friedman, S. Olivier, B. Macintosh, J. Brase, K. Avicola, S. Gibbard, and J. An. Laser Guide Star Based Astrophysics at Lick Observatory. Office of Scientific and Technical Information (OSTI), March 2000. http://dx.doi.org/10.2172/793551.

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4

Olivier, S. S., J. An, and K. Avicola. Performance of laser guide star adaptive optics at Lick Observatory. Office of Scientific and Technical Information (OSTI), July 1995. http://dx.doi.org/10.2172/114020.

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5

Pennington, D., R. Beach, C. Ebbers, G. Erbert, H. Nguyen, R. Page, S. Payne, and M. Perry. Laser Research and Development Studies for Laser Guide Star Systems. Office of Scientific and Technical Information (OSTI), February 2000. http://dx.doi.org/10.2172/793459.

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6

Max, C. E. ,. LLNL. Image improvement from a sodium-layer laser guide star adaptive optics system. Office of Scientific and Technical Information (OSTI), June 1997. http://dx.doi.org/10.2172/305943.

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7

Hogan, Geoff, and C. E. Webb. A CW Laser Master Oscillator for a Scaleable Sodium Guide Star. General Issues. Fort Belvoir, VA: Defense Technical Information Center, January 1997. http://dx.doi.org/10.21236/ada326345.

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8

Worrell, Ernst, Tana Angelini, and Eric Masanet. Managing Your Energy: An ENERGY STAR(R) Guide for Identifying Energy Savings in Manufacturing Plants. Office of Scientific and Technical Information (OSTI), July 2010. http://dx.doi.org/10.2172/985911.

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9

Shtyrkova, Katia, Michael D. Oliker, Kevin P. Vitayaudom, Denis W. Oesch, Darryl J. Sanchez, Patrick R. Kelly, Carolyn M. Tewksbury-Christle, and Julie C. Smith. Experimental Demonstration of Real Time Gradient Gain Correction for Sodium Beacon Laser Guide Star: Postprint. Fort Belvoir, VA: Defense Technical Information Center, June 2010. http://dx.doi.org/10.21236/ada531341.

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10

Olivier, S. S., C. E. Max, H. W. Friedman, J. An, K. Avicola, B. V. Beeman, H. D. Bissinger, et al. First significant image improvement from a sodium-layer laser guide star adaptive optics system at Lick Observatory. Office of Scientific and Technical Information (OSTI), July 1997. http://dx.doi.org/10.2172/576003.

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