Adaptive Optics

What is Adaptive Optics?

Often used in astronomical applications, Adaptive Optics (AO) or sometimes called wavefront sensing (WFS) is a technique to measure wavefront errors or distortions, and correct the resulting image in real time.

In astronomy systems with AO, a reference star that is brighter is usually used in place of the object of interest to measure the shape of the optical wavefront. The reference star would have to be in close proximity to the object of interest.

Using infrared in wavefront sensing

Fainter stars in the sky can be made visible using low noise short-wave infrared cameras. 

This in turn makes it easier to locate natural guide stars to be used as reference in wavefront sensing. Identification of self-referencing red objects too faint in the visible range can also be used for wavefront sensing. 


What do we offer?

Xenics offers various types of SWIR camera in four wavelength ranges:

1. 500 to 1700 nm (visible-enhanced InGaAs)
2. 900 to 1700 nm (standard InGaAs)
3. 900 to 2350 nm (T2SL)
4. 900 to 2500 nm (T2SL)


See Related Products below for a full list of our cameras that are compatible with this application.

What features are needed?

  • Short exposure time
    A short exposure time (< 1 ms) has to be used to “freeze” the effect of atmospheric turbulence.
  • High frame rates and low image lag
    High frame rates and low latency are required to send the correction info to the deformable mirror, in order to correct the wavefronts in real time.
  • Sensitivity
    For relatively bright guide stars, high sensitivity detectors are needed to guarantee a high enough signal to noise ratio on the WFS.

Are you looking for more information? 

Let us know. We are happy to help.

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Short-wave infrared adaptive optics and applications In this article, we have discuss the basic working principle of AO in astronomy, microscopy, retinal imaging and laser communication application.

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