Optical Aperture Synthesis Clean and Closure Phase Image Reconstruction

2008 ◽  
Author(s):  
Weijun Fan
Keyword(s):  
Image Reconstruction ◽  
Aperture Synthesis ◽  
Phase Image ◽  
Optical Aperture

Multi-wavelength Optical Aperture Synthesis

1992 ◽  
Vol 10 (1) ◽  
pp. 71-73 ◽  
Author(s):  
R.G. Marson ◽  
T.R. Bedding ◽  
J.G. Robertson
Keyword(s):  
Radio Astronomy ◽  
Angular Resolution ◽  
Diffraction Limit ◽  
Double Star ◽  
Aperture Synthesis ◽  
Angular Diameter ◽  
Optical Aperture ◽  
Multi Wavelength ◽  
Red Giant ◽  
Large Telescopes

AbstractThe technique of aperture synthesis is well developed in radio astronomy. When applied to the optical regime, aperture synthesis allows one to partially overcome the blurring effects of the atmosphere and increase the angular resolution of large telescopes to the diffraction limit. MAPPIT (Masked APerture-Plane Interference Telescope) is a multi-element interferometer which operates at the coude focus of the 3.9 m Anglo-Australian Telescope. This instrument has recently been reconfigured to operate in a dispersed mode so that simultaneous observations in a band of wavelengths are possible. We will discuss this instrument’s new mode and present observations of the double star δ Sco and an angular diameter of the previously unresolved red giant β Gru.

Research on Sub-Telescopes′ Beams Parallel and Path Difference Adjustment to the Optical Aperture Synthesis Telescope

2009 ◽  
Vol 29 (5) ◽  
pp. 1397-1402 ◽  
Author(s):  
王海涛 Wang Haitao ◽  
朱永凯 Zhu Yongkai ◽  
蔡佳慧 Cai Jiahui ◽  
张雅静 Zhang Yajing ◽  
田贵云 Tian Guiyun
Keyword(s):  
Path Difference ◽  
Aperture Synthesis ◽  
Optical Aperture

Image Reconstruction for Mirrored Aperture Synthesis Radiometers

2020 ◽  
Vol 58 (11) ◽  
pp. 7720-7733
Author(s):  
Yufang Li ◽  
Qingxia Li ◽  
Liangqi Gui ◽  
Li Feng ◽  
Haofeng Dou ◽  
...  
Keyword(s):  
Image Reconstruction ◽  
Aperture Synthesis

Aperture synthesis image reconstruction study for the mid-infrared VLTI imager MATISSE

2006 ◽  
Author(s):  
Karl-Heinz Hofmann ◽  
Stefan Kraus ◽  
Bruno Lopez ◽  
Gerd Weigelt ◽  
Sebastian Wolf
Keyword(s):  
Image Reconstruction ◽  
Aperture Synthesis ◽  
Mid Infrared

scholarly journals Optimal Linear Arrays for Wide Bandwidths

1994 ◽  
Vol 158 ◽  
pp. 331-333
Author(s):  
R. G. Marson
Keyword(s):  
Image Reconstruction ◽  
New Technology ◽  
Reconstruction Algorithm ◽  
Aperture Synthesis ◽  
Complete Coverage ◽  
Linear Arrays ◽  
Image Reconstruction Algorithm ◽  
Optimal Linear ◽  
Frequency Variations

New technology has enabled modern aperture synthesis instruments to employ increasingly larger bandwidths. Large bandwidths can be exploited to enable a more complete coverage in the (u, v) plane and hence aid image reconstruction. This relies on the source having a structure that is invariant with observing frequency or a suitable image reconstruction algorithm to take frequency variations into account.

scholarly journals On the Importance of Active Image Stabilisation

1984 ◽  
Vol 79 ◽  
pp. 367-378
Author(s):  
J.E. Noordam
Keyword(s):  
Point Source ◽  
Speckle Interferometry ◽  
Aperture Synthesis ◽  
Atmospheric Conditions ◽  
Optical Telescope ◽  
Aperture Diameter ◽  
Logical Approach ◽  
Optical Aperture ◽  
Large Telescopes ◽  
Mirror Telescope

AbstractThe performance of an optical telescope can be improved considerably by opening the shutter only at moments of good seeing. The resulting instantaneous highresolution images must be corrected for shift before adding them all together. The optimum aperture diameter for which this technique works well is 1 meter or less, depending on atmospheric conditions. Image stabilisation not only improves the resolution and thus the point-source sensitivity, but it is also expected to improve the performance of speckle interferometry and optical aperture synthesis. This makes its implementation on large telescopes desirable. While it is certainly possible to do this by treating a large filled aperture like a set of independent subapertures, a much more logical approach would be to build an array of 1-meter telescopes, preferably mounted in a single large frame so that it can be pointed in all directions without extensive pathlength compensation. Such a “Many Mirror Telescope” has many advantages, and is feasible because image stabilisation helps to solve the beam-combining problem.

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