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ARGOS - Easy AO Introduction


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Ground Layer Adaptive Optics - A Simple Introduction


Adaptive Optics in general

Why does a telescope, like the Large Binocular Telescope, need an adaptive optics system?

The resolution of large ground based telescopes is limited by atmospheric turbulences. Placing the telescope on a satellite would avoid this, but space telescopes are limited in size and expensive.

The atmospheric turbulences can be corrected in real time by an adaptive optics system. Therefor the wavefront of a bright star is analyzed and corrected by a deformable mirror (inspired by Claire Max, CfAO).

So the resolution of a telescope is no longer limited by the atmosphere. This example shows the galactic center.

The adaptive optics system needs a bright light source to work. If there is no suitable object near the scientific object, an well defined, artificial star is generated by a laser. The picture shows PARSEC, the natrium guide star of ESO's VLT-UT4.

Ground Layer Adaptive Optics

cn2 profile
A CN2-profile shows the amount of air turbulences over height from ground. It is obvious, that the strongest turbulences are close to the ground. The aim of a Ground Layer Adaptive Optics system is to compensate these turbulences over a wide field of view. (figure by E. Masciadri, INAF)

GLAO timing
As the used laser is pulsed with 10kHz, it looks like a continuous beam. But in fact the facility deals with single pulses.

How it works:

GLAO scheme
  1. A laser pulse is launched above the secondary mirror and focused on a point in a height of about 12km. With the pulse propagating through atmosphere, a small percentage of its energy is scattered by air-molecules on its path (rayleigh scattering).

  2. As the speed of light is known, the time can be calculated when the pulse reaches a height of about 12km. Twice this time is when the scattered light will be back at the telescope. Here it is detected by the wavefront sensor, which is focusing on the same point as the laser beam. Due to the use of a single laser pulse, we see only the scattered light from the desired height.
    As the scattered light passes the ground layers on its way back, the distortion of these layers can be optained from the wavefront.
    But as seen on the figure, one star covers only a small field above the telescope.

GLAO more stars
By generating more stars, a wider field of the air above the telescope can be analyzed.

Laser setup
Green lasers are often used because:
  • rayleigh scattering works best for short wavelengths
  • the telescope optics are optimized for visible and infrared light
  • visible light simplifies the alignment of the instrument
  • they are robust and cheap. They are usually used for industrial applications.

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