Relevant bibliographies by topics / Astronomical imaging

Contents

  1. Journal articles
  2. Dissertations / Theses
  3. Books
  4. Book chapters
  5. Conference papers
  6. Reports

Academic literature on the topic 'Astronomical imaging'

Author: Grafiati
Published: 4 June 2021
Last updated: 10 March 2023

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Journal articles on the topic "Astronomical imaging"

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ROGGEMANN, MICHAEL C., and DAVID W. TYLER. "Unconventional Astronomical Imaging." Optics and Photonics News 3, no. 3 (March 1, 1992): 16. http://dx.doi.org/10.1364/opn.3.3.000016.

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Pimbblet, Kevin A., and Michael Bulmer. "Random Numbers from Astronomical Imaging." Publications of the Astronomical Society of Australia 22, no. 01 (January 2005): 1–5. http://dx.doi.org/10.1071/as04043.

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Cook, Timothy A., Brian A. Hicks, Paul G. Jung, and Supriya Chakrabarti. "Far-ultraviolet astronomical narrowband imaging." Applied Optics 48, no. 10 (March 26, 2009): 1936. http://dx.doi.org/10.1364/ao.48.001936.

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Buscher, David, Nahid Chowdhury, Ric Davies, Sasha Hinkley, Norbert Hubin, Paul Jorden, Craig Mackay, et al. "Towards high-resolution astronomical imaging." Astronomy & Geophysics 60, no. 3 (June 1, 2019): 3.22–3.27. http://dx.doi.org/10.1093/astrogeo/atz146.

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Pipher, Judith L. "Astronomical imaging with InSb arrays." Experimental Astronomy 3, no. 1-4 (1994): 1–8. http://dx.doi.org/10.1007/bf00430109.

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Puschmann, K. G., and F. Kneer. "On super-resolution in astronomical imaging." Astronomy & Astrophysics 436, no. 1 (May 20, 2005): 373–78. http://dx.doi.org/10.1051/0004-6361:20042320.

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GATLEY, I., D. L. DEPOY, and A. M. FOWLER. "Astronomical Imaging with Infrared Array Detectors." Science 242, no. 4883 (December 2, 1988): 1264–70. http://dx.doi.org/10.1126/science.242.4883.1264.

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Vilas, Faith, and Bradford A. Smith. "Coronagraph for astronomical imaging and spectrophotometry." Applied Optics 26, no. 4 (February 15, 1987): 664. http://dx.doi.org/10.1364/ao.26.000664.

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Saklatvala, George, Stafford Withington, and Michael P. Hobson. "Simulations of astronomical imaging phased arrays." Journal of the Optical Society of America A 25, no. 4 (March 26, 2008): 958. http://dx.doi.org/10.1364/josaa.25.000958.

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Chu, Qing, Stuart Jefferies, and James G. Nagy. "Iterative Wavefront Reconstruction for Astronomical Imaging." SIAM Journal on Scientific Computing 35, no. 5 (January 2013): S84—S103. http://dx.doi.org/10.1137/120882603.

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Dissertations / Theses on the topic "Astronomical imaging"

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Wong, Alison. "Artificial Intelligence for Astronomical Imaging." Thesis, The University of Sydney, 2023. https://hdl.handle.net/2123/30068.

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Astronomy is the ultimate observational science. Objects outside our solar system are beyond our reach, so we are limited to acquiring knowledge at a distance. This motivates the need to advance astrophysical imaging technologies, particularly for the field of high contrast imaging, where some of the most highly prized science goals require high fidelity imagery of exoplanets and of the circumstellar structures associated with stellar and planetary birth. Such technical capabilities address questions of both the birth and death of stars which in turn informs the grand recycling of matter in the chemical evolution of the galaxy and universe itself. Ground-based astronomical observation primarily relies on extreme adaptive optics systems in order to extract signals arising from faint structures within the immediate vicinity of luminous host stars. These systems are distinguished from standard adaptive optics systems in performing faster and more precise wavefront correction which leads to better imaging performance. The overall theme of this thesis therefore ties together advanced topics in artificial intelligence with techniques and technologies required for the field of high contrast imaging. This is accomplished with demonstrations of deep learning methods used to improve the performance of extreme adaptive optics systems and is deployed and benchmarked with data obtained at the Subaru Coronagraphic Extreme Adaptive Optics (SCExAO) system operating at the observatory on the summit of Mauna Kea in Hawaii. Solutions encompass both hardware and software, with optimal recovery of scientific outcomes delivered by model fitting of high contrast imaging data with modern machine learning techniques. This broad-ranging study subjecting acquisition, analysis and modelling of data hopes to yield more accurate and higher fidelity observables which in turn delivers improved interpretation and scientific delivery.
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Leung, Wun Ying Valerie. "Inverse problems in astronomical and general imaging." Thesis, University of Canterbury. Electrical and Computer Engineering, 2002. http://hdl.handle.net/10092/7513.

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The resolution and the quality of an imaged object are limited by four contributing factors. Firstly, the primary resolution limit of a system is imposed by the aperture of an instrument due to the effects of diffraction. Secondly, the finite sampling frequency, the finite measurement time and the mechanical limitations of the equipment also affect the resolution of the images captured. Thirdly, the images are corrupted by noise, a process inherent to all imaging systems. Finally, a turbulent imaging medium introduces random degradations to the signals before they are measured. In astronomical imaging, it is the atmosphere which distorts the wavefronts of the objects, severely limiting the resolution of the images captured by ground-based telescopes. These four factors affect all real imaging systems to varying degrees. All the limitations imposed on an imaging system result in the need to deduce or reconstruct the underlying object distribution from the distorted measured data. This class of problems is called inverse problems. The key to the success of solving an inverse problem is the correct modelling of the physical processes which give rise to the corresponding forward problem. However, the physical processes have an infinite amount of information, but only a finite number of parameters can be used in the model. Information loss is therefore inevitable. As a result, the solution to many inverse problems requires additional information or prior knowledge. The application of prior information to inverse problems is a recurrent theme throughout this thesis. An inverse problem that has been an active research area for many years is interpolation, and there exist numerous techniques for solving this problem. However, many of these techniques neither account for the sampling process of the instrument nor include prior information in the reconstruction. These factors are taken into account in the proposed optimal Bayesian interpolator. The process of interpolation is also examined from the point of view of superresolution, as these processes can be viewed as being complementary. Since the principal effect of atmospheric turbulence on an incoming wavefront is a phase distortion, most of the inverse problem techniques devised for this seek to either estimate or compensate for this phase component. These techniques are classified into computer post-processing methods, adaptive optics (AO) and hybrid techniques. Blind deconvolution is a post-processing technique which uses the speckle images to estimate both the object distribution and the point spread function (PSF), the latter of which is directly related to the phase. The most successful approaches are based on characterising the PSF as the aberrations over the aperture. Since the PSF is also dependent on the atmosphere, it is possible to constrain the solution using the statistics of the atmosphere. An investigation shows the feasibility of this approach. Bispectrum is also a post-processing method which reconstructs the spectrum of the object. The key component for phase preservation is the property of phase closure, and its application as prior information for blind deconvolution is examined. Blind deconvolution techniques utilise only information in the image channel to estimate the phase which is difficult. An alternative method for phase estimation is from a Shack-Hartmann (SH) wavefront sensing channel. However, since phase information is present in both the wavefront sensing and the image channels simultaneously, both of these approaches suffer from the problem that phase information from only one channel is used. An improved estimate of the phase is achieved by a combination of these methods, ensuring that the phase estimation is made jointly from the data in both the image and the wavefront sensing measurements. This formulation, posed as a blind deconvolution framework, is investigated in this thesis. An additional advantage of this approach is that since speckle images are imaged in a narrowband, while wavefront sensing images are captured by a charge-coupled device (CCD) camera at all wavelengths, the splitting of the light does not compromise the light level for either channel. This provides a further incentive for using simultaneous data sets. The effectiveness of using Shack-Hartmann wavefront sensing data for phase estimation relies on the accuracy of locating the data spots. The commonly used method which calculates the centre of gravity of the image is in fact prone to noise and is suboptimal. An improved method for spot location based on blind deconvolution is demonstrated. Ground-based adaptive optics (AO) technologies aim to correct for atmospheric turbulence in real time. Although much success has been achieved, the space- and time-varying nature of the atmosphere renders the accurate measurement of atmospheric properties difficult. It is therefore usual to perform additional post-processing on the AO data. As a result, some of the techniques developed in this thesis are applicable to adaptive optics. One of the methods which utilise elements of both adaptive optics and post-processing is the hybrid technique of deconvolution from wavefront sensing (DWFS). Here, both the speckle images and the SH wavefront sensing data are used. The original proposal of DWFS is simple to implement but suffers from the problem where the magnitude of the object spectrum cannot be reconstructed accurately. The solution proposed for overcoming this is to use an additional set of reference star measurements. This however does not completely remove the original problem; in addition it introduces other difficulties associated with reference star measurements such as anisoplanatism and reduction of valuable observing time. In this thesis a parameterised solution is examined which removes the need for a reference star, as well as offering a potential to overcome the problem of estimating the magnitude of the object.
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Clare, Richard M. "Wavefront sensing and phase retrieval for astronomical imaging." Thesis, University of Canterbury. Electrical and Computer Engineering, 2004. http://hdl.handle.net/10092/7841.

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Images of astronomical objects captured by ground-based telescopes are distorted by the earth's atmosphere. The atmosphere consists of random time-varying layers of air of differing density and hence refractive index. These refractive index fluctuations cause wavefronts that propagate through the atmosphere to become aberrated, resulting in a loss in resolution of the astronomical images. The wavefront aberrations that are induced by the atmosphere can be compensated by either real-time adaptive optics, where a deformable mirror is placed in the optical path, or by computer post-processing algorithms on the distorted images. In an adaptive optics system, the wavefront sensor is the element that estimates the wavefront phase aberration. The wavefront cannot be measured directly, and instead an aberration is introduced to the optical path to produce two or more intensity distributions, from which the wavefront slope or curvature can be estimated. Wavefront sensing is one of the topics of this thesis. A number of computer post-processing algorithms exist to deblur astronomical images, such as phase diversity, deconvolution from wavefront sensing (DWFS) and phase retrieval, with improvements to the latter two published in this thesis. The pyramid wavefront sensor consists of a four-sided glass prism placed in the focal plane of the telescope, which subdivides the focal plane in four, and a relay lens which re-images the four sections of the focal plane to form four images of the aperture at the conjugate aperture plane. The wavefront slope is estimated as a linear combination of the aperture images. The pyramid sensor can be generalised to a class of N-sided glass prism wavefront sensors that subdivide the focal plane into N equal sections, forming N aperture images at the conjugate aperture plane. The minimum number of sides required to estimate the slope in two orthogonal directions is three, and the cone sensor is derived by letting N tend to infinity. Simulation results show that in the presence of photon, but not read, noise the cone sensor provides the best wavefront estimate. For the pyramid sensor, the wavefront is typically reconstructed from the estimate of the wavefront slope in two orthogonal directions. Some information is inherently lost when the four measurements (aperture images) are reduced to two slope estimates. A new method is proposed to reconstruct the wavefront directly from the aperture images, removing the intermediate step of forming the slope estimates. Reconstructing the wavefront directly from the images is shown through simulation of atmospheric phase screens to give a better wavefront estimate than reconstructing from the slope estimates. This result is true for all pyramid type sensors tested. The pyramid wavefront sensor can be generalised by placing the lenslet array at the focal plane to subdivide the complex field in the focal plane into more than four sections. Using this framework, the pyramid sensor can be considered as the dual of the Shack Hartmann sensor, which subdivides the aperture plane with a lenslet array, since the two sensors subdivide each one of a Fourier pair. Both sensors estimate the wavefront slope with a centroid operator on the low resolution images. Also, in both sensors there exists a trade-off between the spatial resolution obtainable and the accuracy of the slope estimates. This trade-off is determined by the size of the lenslets in the array for both sensors, and is inverted between the two sensors. Simulation results run in open loop demonstrate that the lenslet array at the aperture (Shack-Hartmann) and focal (pyramid) planes do provide wavefront estimates of equivalent quality. The lenslet array at the focal plane, however, can be modulated so as to increase its linear range and thus provide a better wavefront estimate than the Shack-Hartmann sensor in open loop simulations. Phase retrieval is a non-linear iterative technique that is used to recover the phase in the aperture plane from intensity measurements at the focal plane and other constraints. A novel phase retrieval algorithm, which subdivides the focal plane of the telescope with a lenslet array and uses the aperture images formed at the conjugate aperture plane as a magnitude constraint, is proposed. This algorithm is more heavily constrained than conventional phase retrieval or phase retrieval in conjunction with the Shack-Hartmann sensor, with constraints applied at three Fourier planes: the aperture, focal and conjugate aperture planes. The subdivision of the focal plane means that the ambiguity problem that exists in other phase retrieval algorithms between an object A(x,y) and its twin A* (x,y) is removed, and this is supported by simulation results. Simulation results also show that the performance of the algorithm is dependent on the starting point, and that starting with the linear estimate from the aperture images gives a better wavefront estimate than starting with zero phase. DWFS is a computer post-processing algorithm that combines the distorted image and wavefront sensing measurements in order to compensate the image for the atmospheric turbulence. An accurate calibration of the reference positions for the centroids of the Shack-Hartmann sensor is essential for an accurate estimate of the wavefront and hence astronomical object, with DWFS. The conventional method for estimating these reference positions is to image a laser beam through the Shack-Hartmann lenslet array but not through the atmosphere. An alternative calibration technique is to observe a single bright star and optimise the Strehl ratio with respect to the reference positions. Results using DWFS on data captured at the Observatoire de Lyon show that this new technique can provide wavefront estimates of similar quality as the grid calibration technique, but without the need for a separate calibration laser.
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Dunlop, Colin Nigel. "The imaging properties of large reflecting astronomical telescopes." Thesis, Durham University, 1986. http://etheses.dur.ac.uk/7019/.

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This thesis is concerned with some of the limitations concerned with the imaging properties of astronomical telescopes of large apertures. These arise from the atmosphere, the diffracting aperture, the residual errors in the optically worked surfaces and the characteristics of the detection devices. Methods of Fourier optics are used to determine modulation transfer functions and associated point spread function. They are applied to three problems. The first of these is a comparison of the diffraction patterns that are expected from the multi-mirror telescopes. These are made either of separated individual mirrors or of segmented mirrors shaped to an overall parabolic shape. The effect of the dilution of the aperture in the former and the effect of misalignment in the latter is investigated. In the second study, the factors contributing to the imaging of the UK Schmidt telescope are considered and design studies of this and other two variants are examined. In particular the limiting effect of the atmosphere and of the detecting photographic emulsion is noted. Thirdly the overall limitation of the atmospheric seeing is considered experimentally. The Durham Polaris seeing monitor has been designed and built with a shear interferometer. It has been tested at local ground level where local measurements of seeing have been made. In the near future it will be taken and used at La Palma.
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Lagadec, Tiphaine. "Advanced photonic solutions for high precision astronomical imaging." Thesis, The University of Sydney, 2019. https://hdl.handle.net/2123/22078.

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The sharply rising productivity of exoplanet searches over the past two decades has delivered profound statistical insights into the prevalence and diversity of worlds around other stars. The frontier for astronomers has now expanded into the new era of exoplanet characterisation. Major progress here will only be achieved with new instrumental advances. Most highly sought-after is the capability to separate the faint light from a planet from the glare of the host star. The direct detection of planetary photons will enable unique spatial and spectral studies, revealing intrinsic properties of atmospheres and surfaces. In this project, a prototype instrument GLINT South (Guided Light Interferometric Nulling Technology) was developed. It employs nulling interferometry in which the light from the host star is actively rejected though destructive interference. Such advanced control and processing of starlight is accomplished by way of photonic technology fabricated into integrated optical chips. A monochromatic null depth was measured in the laboratory consistent with 0 within an uncertainty of 10-3. The instrument was tested at the Anglo Australian Telescope, and a sample of infrared-bright stars were observed retrieving uniform disk diameters in close agreement to the literature values, despite the stellar diameters being beyond the telescopes formal di raction limit. Furthermore, an algorithm was created to optimise the design of integrated optics waveguides for pupil remapping chips leading to the design of a 4-input remapping chip which will signi cantly expand capabilities and deliver multi-channel nulling as well as complex visibility data. The photonic nulling devices, inscribed within miniature, robust and environmentally stable monolithic chips are a promising avenue to one of astronomy's grandest challenges of characterising the chemical and physical environments of exoplanets.
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Tubbs, Robert Nigel. "Lucky exposures : diffraction limited astronomical imaging through the atmosphere." Thesis, University of Cambridge, 2003. https://www.repository.cam.ac.uk/handle/1810/224517.

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The resolution of astronomical imaging from large optical telescopes is usually limited by the blurring effects of refractive index fluctuations in the Earth's atmosphere. By taking a large number of short exposure images through the atmosphere, and then selecting, re-centring and co-adding the best images this resolution limit can be overcome. This approach has significant benefits over other techniques for high-resolution optical imaging from the ground. In particular the reference stars used for our method (the Lucky Exposures technique) can generally be fainter than those required for the natural guide star adaptive optics approach or those required for other speckle imaging techniques. The low complexity and low instrumentation costs associated with the Lucky Exposures method make it appealing for medium-sized astronomical observatories. The method can provide essentially diffraction-limited I-band imaging from well-figured ground-based telescopes as large as 2.5 m diameter. The faint limiting magnitude and large isoplanatic patch size for the Lucky Exposures technique at the Nordic Optical Telescope means that 25% of the night sky is within range of a suitable reference star for I-band imaging. Typically the 1%-10% of exposures with the highest Strehl ratios are selected. When these exposures are shifted and added together, field stars in the resulting images have Strehl ratios as high as 0.26 and full width at half maximum flux (FWHM) as small as 90 milliarc seconds. Within the selected exposures the isoplanatic patch is found to be up to 60 arc seconds in diameter at 810 nm wavelength. Images within globular clusters and of multiple stars from the Nordic Optical Telescope using reference stars as faint as I 16 are presented. A new generation of CCDs (Marconi L3Vision CCDs) were used in these observations, allowing extremely low noise high frame-rate imaging with both fine pixel sampling and a relatively wide field of view. The theoretical performance of these CCDs is compared with the experimental results obtained.
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Zadnik, Jerome A. "The use of charge coupled devices in astronomical speckle imaging." Diss., Georgia Institute of Technology, 1993. http://hdl.handle.net/1853/14947.

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Young, N. G. "The digital processing of astronomical and medical coded aperture images." Thesis, University of Southampton, 1985. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.482729.

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Brockie, Richard. "Extending the limits of direct high angular resolution infrared astronomical imaging." Thesis, University of Edinburgh, 1998. http://hdl.handle.net/1842/30315.

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Observing in the infrared (IR) part of the electromagnetic spectrum is now an established tool of astronomy. It allows investigations of, among others, high redshift galaxies, star formation regions and very low mass stars close to the hydrogen burning limit as well as providing information complementary to that obtained in other regions of the spectrum. The dimensions of infrared arrays have increased over the years from 62 x 58 in IRCAM1, the first infrared imager on the UK Infrared Telescope, to the 2562 array in IRCAM3, the current camera, soon to be superseded by 10242 arrays in the next generation of instruments. In this thesis, I describe the first observing programme which uses infrared observations to measure trigonometric parallaxes - made possible through the introduction of larger IR assays. In this programme, certain difficulties associated with infrared techniques are encountered and described with results presented for a previously measured star and a brown dwarf candidate. A major benefit of observing in the infrared is that atmospheric distortion has less of an effect on the formation of images - seeing on a good site can be < 0.5" at 2μm. The recent development of Adaptive Optics (AO) systems, which compensate for wavefront aberrations as observations are made, further reduce the effects of atmospheric distortion. AO systems have a servo-loop in which a deformable mirror attempts to remove the distortion present in the measured wavefront. In this thesis, I describe a method of real time characterisation of the most recent behaviour of the atmosphere, as observed by an AO system. Rather than reacting to the last measured distortion, this knowledge can be used in the servo-loop to reduce mirror fitting errors by predicting the next mirror shape. I describe a series of simulations which prove the validity of this novel technique. Finally, with simulations of the AO system being built for the William Herschel Telescope, I show that the improvement in performance available through prediction allows use of an AO guide star about 0.25 magnitudes fainter when compared with the non-predictive case.
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Duncan, Stephen Howard. "The application of parallel processing techniques in coded aperture imaging." Thesis, University of Southampton, 1992. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.239709.

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Books on the topic "Astronomical imaging"

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Kennedy, L. A. One-Shot Color Astronomical Imaging. Boston, MA: Springer US, 2012. http://dx.doi.org/10.1007/978-1-4614-3247-0.

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Woodhouse, Chris. The astrophotography manual: A practical and scientific approach to deep space imaging. Burlington, MA: Focal Press, 2015.

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E, Kontizas, and IAU Commission 9, eds. Wide-field spectroscopy: Proceedings of the 2nd conference of the working group of IAU Commission 9 on "Wide-field imaging" held in Athens, Greece, May 20-25, 1996. Dordrecht: Kluwer, 1997.

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Introduction to digital astrophotography: Imaging the universe with a digital camera. 2nd ed. Richmond, VA: Willmann-Bell, 2011.

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Electronic imaging in astronomy: Detectors and instrumentation. 2nd ed. Berlin: Springer, 2008.

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Electronic imaging in astronomy: Detectors and instrumentation. Chichester: Wiley, 1997.

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J, Hanisch R., Brissenden R. J. V, Barnes Jeannette V, and Analysis Software and Systems (2nd : 1992 : Boston, Mass.), eds. Astronomical Data Analysis Software and Systems II. San Francisco, Calif: Astronomical Society of the Pacific, 1993.

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service), SpringerLink (Online, ed. One-Shot Color Astronomical Imaging: In Less Time, For Less Money! Boston, MA: Springer US, 2012.

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J, Laureijs R., ed. PHT--the imaging photo-polarimeter. Noordwijk, The Netherlands: ESA Publications, 2003.

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D, Monnier John, Schöller Markus, Danchi William Clifford, American Astronomical Society, and Society of Photo-optical Instrumentation Engineers., eds. Advances in stellar interferometry: 25-30 May 2006, Orlando, Florida, USA. Bellingham, Wash: SPIE, 2006.

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Book chapters on the topic "Astronomical imaging"

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Pipher, Judith L. "Astronomical Imaging with InSb Arrays." In Infrared Astronomy with Arrays, 1–8. Dordrecht: Springer Netherlands, 1994. http://dx.doi.org/10.1007/978-94-011-1070-9_1.

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Moore, Stan. "The Theory of Astronomical Imaging." In Lessons from the Masters, 1–28. New York, NY: Springer New York, 2013. http://dx.doi.org/10.1007/978-1-4614-7834-8_1.

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Mobberley, Martin. "Electronic Imaging and the Electronics Revolution." In Astronomical Equipment for Amateurs, 153–97. London: Springer London, 1999. http://dx.doi.org/10.1007/978-1-4471-0583-1_8.

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Du Foresto, V. Coudé. "Integrated Optics in Astronomical Interferometry." In Very High Angular Resolution Imaging, 261–71. Dordrecht: Springer Netherlands, 1994. http://dx.doi.org/10.1007/978-94-011-0880-5_46.

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Murtagh, F. "Classification: Astronomical and Mathematical Overview." In Astronomy from Wide-Field Imaging, 227–33. Dordrecht: Springer Netherlands, 1994. http://dx.doi.org/10.1007/978-94-011-1146-1_47.

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Norris, Ray P. "AIPS++: A New Astronomical Imaging Package." In Very High Angular Resolution Imaging, 247–56. Dordrecht: Springer Netherlands, 1994. http://dx.doi.org/10.1007/978-94-011-0880-5_44.

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Veenboer, Bram, and John W. Romein. "Radio-Astronomical Imaging: FPGAs vs GPUs." In Lecture Notes in Computer Science, 509–21. Cham: Springer International Publishing, 2019. http://dx.doi.org/10.1007/978-3-030-29400-7_36.

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Griffiths, Martin. "A Brief History of Astronomical Imaging." In The Patrick Moore Practical Astronomy Series, 1–8. New York, NY: Springer New York, 2014. http://dx.doi.org/10.1007/978-1-4939-1044-1_1.

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Völk, Heinrich J., and Konrad Bernlöhr. "Imaging very high energy gamma-ray telescopes." In 400 Years of Astronomical Telescopes, 171–89. Dordrecht: Springer Netherlands, 2009. http://dx.doi.org/10.1007/978-90-481-2233-2_12.

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Starck, Jean-Luc, Fionn Murtagh, and Mario Bertero. "Starlet Transform in Astronomical Data Processing." In Handbook of Mathematical Methods in Imaging, 1489–531. New York, NY: Springer New York, 2011. http://dx.doi.org/10.1007/978-0-387-92920-0_34.

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Conference papers on the topic "Astronomical imaging"

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Vigroux, L., and G. Wlerick. "Astronomical Imaging." In International Topical Meeting on Image Detection and Quality, edited by Lucien F. Guyot. SPIE, 1987. http://dx.doi.org/10.1117/12.966764.

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Smith, Alan R., Richard J. McDonald, Donna C. Hurley, Steven E. Holland, Donald E. Groom, William E. Brown, David K. Gilmore, Richard J. Stover, and Mingzhi Wei. "Radiation events in astronomical CCD images." In Electronic Imaging 2002, edited by Morley M. Blouke, John Canosa, and Nitin Sampat. SPIE, 2002. http://dx.doi.org/10.1117/12.463423.

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Makovoz, David, Iffat Khan, and Frank Masci. "Mosaicking of astronomical images with MOPEX." In Electronic Imaging 2006, edited by Charles A. Bouman, Eric L. Miller, and Ilya Pollak. SPIE, 2006. http://dx.doi.org/10.1117/12.643521.

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Ferrero, Alejandro, Riccardo Felletti, Lorraine Hanlon, Joaquin Campos, and Alicia Pons. "Electron-multiplying CCD astronomical photometry." In IS&T/SPIE Electronic Imaging, edited by Erik Bodegom and Valérie Nguyen. SPIE, 2010. http://dx.doi.org/10.1117/12.840225.

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Bryant, Julia J., and Joss Bland-Hawthorn. "Square-core bundles for astronomical imaging." In SPIE Astronomical Telescopes + Instrumentation, edited by Ian S. McLean, Suzanne K. Ramsay, and Hideki Takami. SPIE, 2012. http://dx.doi.org/10.1117/12.925127.

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Fu, Chi-Wing, Andrew J. Hanson, and Eric A. Wernert. "Navigation techniques for large-scale astronomical exploration." In Electronic Imaging 2006, edited by Robert F. Erbacher, Jonathan C. Roberts, Matti T. Gröhn, and Katy Börner. SPIE, 2006. http://dx.doi.org/10.1117/12.648287.

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Hildebrand, Roger H., Jessie L. Dotson, Charles D. Dowell, Giles Novak, David A. Schleuning, and J. Vaillancourt. "Hertz: an imaging polarimeter." In Astronomical Telescopes & Instrumentation, edited by Thomas G. Phillips. SPIE, 1998. http://dx.doi.org/10.1117/12.317364.

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Ribak, Erez, E. K. Hege, Nicolas V. Strobel, and Julian C. Christou. "Shift-And-Add For Astronomical Imaging." In 6th Mtg in Israel on Optical Engineering, edited by Rami Finkler and Joseph Shamir. SPIE, 1989. http://dx.doi.org/10.1117/12.951077.

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Ribak, Erez. "Astronomical Imaging By Pupil Plane Interferometry." In 6th Mtg in Israel on Optical Engineering, edited by Rami Finkler and Joseph Shamir. SPIE, 1989. http://dx.doi.org/10.1117/12.951078.

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Hogg, David W., Dustin Lang, and Coryn A. L. Bailer-Jones. "Astronomical imaging: The theory of everything." In CLASSIFICATION AND DISCOVERY IN LARGE ASTRONOMICAL SURVEYS: Proceedings of the International Conference: “Classification and Discovery in Large Astronomical Surveys”. AIP, 2008. http://dx.doi.org/10.1063/1.3059072.

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Reports on the topic "Astronomical imaging"

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Marois, C. High Resolution Imaging of Satellites with Ground-Based 10-m Astronomical Telescopes. Office of Scientific and Technical Information (OSTI), January 2007. http://dx.doi.org/10.2172/1036840.

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