Stellar Speckle Interferometry with Large Telescopes

2005 ◽  
Author(s):  
Yuri Balega
Keyword(s):  
Speckle Interferometry ◽  
Stellar Speckle Interferometry ◽  
Large Telescopes

scholarly journals Infrared Speckle Interferometry: A Sensitive Technique for Physical Measurements of Unseen Companions to Nearby Stars

1986 ◽  
Vol 109 ◽  
pp. 309-319
Author(s):  
D. W. McCarthy
Keyword(s):  
Main Sequence ◽  
Position Angle ◽  
Speckle Interferometry ◽  
Resolving Power ◽  
Detector Arrays ◽  
Physical Measurements ◽  
Nearby Stars ◽  
Absolute Magnitudes ◽  
Large Telescopes ◽  
Atmospheric Seeing

Infrared speckle interferometry combines the full resolving power of large telescopes with high photometric sensitivity over the wavelength range 2.2 to 12 microns. Despite improved atmospheric seeing at these wavelengths, seeing fluctuations limit measurement precision. Astrometric companions have been detected with angular separations ≥0.1 arcsec and magnitude differences ≤3.7 mag. Results illustrate seeing limitations and show how the usual position angle ambiguity can be overcome. These measurements yield masses and absolute magnitudes for calibrating the lower main sequence. In some cases, orbital motion is detected. A method of “shift-and-add” enables detection of substellar (0.04 to 0.08 M⊙) companions. Future improvements involving detector arrays and seeing monitors are discussed.

Laboratory simulation of stellar speckle interferometry

1979 ◽  
Vol 18 (6) ◽  
pp. 828 ◽  
Author(s):  
Douglas P. Karo ◽  
Arthur M. Schneiderman
Keyword(s):  
Speckle Interferometry ◽  
Laboratory Simulation ◽  
Stellar Speckle Interferometry

Real-time processor for stellar speckle interferometry using microchannel spatial light modulator

1990 ◽  
Author(s):  
Junji Ohtsubo ◽  
Takeshi Utakouji ◽  
Tamiki Takemori ◽  
Katsuyoshi Fujita ◽  
Syuzo Isobe
Keyword(s):  
Real Time ◽  
Spatial Light Modulator ◽  
Speckle Interferometry ◽  
Light Modulator ◽  
Stellar Speckle Interferometry

scholarly journals Infrared Speckle Methods

1984 ◽  
Vol 79 ◽  
pp. 309-336 ◽  
Author(s):  
A. Chelli
Keyword(s):  
Optical Properties ◽  
Image Reconstruction ◽  
Spatial Resolution ◽  
Near Infrared ◽  
Speckle Interferometry ◽  
Reconstruction Methods ◽  
Interferometry Method ◽  
Large Telescopes

I-INTRODUCTION The speckle interferometry method has been introduced in 1970 by A. Labeyrie who showed in the visible dcmain that it was possible to reach the limiting spatial resolution of large telescopes. From 1977, the method is extended to the near infrared between 2 and 5ym (Lena, 1977; Wade and Selby, 1978) ,7 years later infrared speckle systems are operating on several large telescopes (ESO, KPNO, AAT, UKIRT, CFHT... ).The speckle interferometry method has allowed to better understanding the optical properties of the atmosphere, especially owing to the work of F.Roddier (Roddier, 1981). It has raised new problems like the phase restitution of the object spectrum and has largely contributed to the development of image reconstruction methods.

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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