speckle imaging

The first answer to this problem was speckle imaging, which allowed bright objects to be observed with very high resolution.

Speckle imaging recreates the original image through image processing techniques.

See adaptive optics, speckle imaging and optical interferometry.

Amateur astronomers also commonly use digital cameras, including the use of webcams for speckle imaging or "video astronomy".

Lucky imaging (also called lucky exposures) is one form of speckle imaging used for astronomical photography.

Resolution limits can also be overcome by adaptive optics, speckle imaging or lucky imaging for ground-based telescopes.

The task of measuring and quantifying what happens to these is borrowed from methods in physics and computational imaging like Speckle imaging.

In these cases, speckle imaging or adaptive optics imaging using ground based telescopes can be used to greatly reduce the likelihood of background eclipsing binaries.

However the resolution handicap has begun to be overcome by adaptive optics, speckle imaging and interferometric imaging, as well as the use of space telescopes.

All of these were obtained using speckle imaging and have higher resolution than can be obtained with e.g. the Hubble Space Telescope:

A less familiar example of speckle is the highly magnified image of a star through imperfect optics or through the atmosphere (see speckle imaging).

The speckle effect is also used in stellar speckle astronomy, speckle imaging and in eye testing using speckle.

Speckle masking (or bispectral analysis) is a speckle imaging method which involves estimation of the bispectrum or closure phases from each of the short exposures.

Use of the WIYN Observatory for speckle imaging found that the host star of KOI-98 was actually a close-knit binary star, which complicated the analysis.

Speckle imaging (also known as video astronomy) describes a range of high-resolution astronomical imaging techniques based either on the shift-and-add ("image stacking") method or on speckle interferometry methods.

The fact that many of the speckle imaging methods have multiple names results largely from amateur astronomers re-inventing existing speckle imaging techniques and giving them new names.

Other approaches that can yield resolving power exceeding the limits of atmospheric seeing include speckle imaging, aperture synthesis, lucky imaging and space-based telescope such as NASA's Hubble Space Telescope.

The use of speckle imaging using adaptive optics at the WIYN Observatory in Arizona and the Palomar Observatory in California isolated the starlight of Kepler-5 from background stars.

The WIYN Observatory, which was used for speckle imaging, supported Keck's findings and verified that the signal caused by KOI-20 was not caused by a nearby background star's interference.

Other methods can achieve resolving power exceeding the limit imposed by atmospheric distortion, such as speckle imaging, aperture synthesis, and lucky imaging, or by moving outside the atmosphere with space telescopes, such as the Hubble Space Telescope.

Modern webcams and camcorders have the ability to capture rapid short exposures with sufficient sensitivity for astrophotography, and these devices are used with a telescope and the shift-and-add method from speckle imaging (also known as image stacking) to achieve previously unattainable resolution.

It causes the images of point sources (such as stars), which in the absence of atmospheric turbulence would be steady Airy patterns produced by diffraction, to break up into speckle patterns, which change very rapidly with time (the resulting speckled images can be processed using speckle imaging)