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Developments
Development of OmegaCAM cooling system
Fibre Bundle
Interferometer
IR test camera
OmegaCAM cooling
AO test bench
The 2.6-m VLT Survey Telescope (VST) will be equipped with the optical wide-angle camera OmegaCAM, which features a field of view and pixel scale that perfectly match the VST and Paranal, respectively. OmegaCAM will be mounted in the Cassegrain focus, and the focal plane is populated with a mosaic of thirty-two 2K x 4K CCDs plus 4 virtually identical auxiliary CCDs for autoguiding and image analysis. For the optimal trade-off between dark current, sensitivity, and cosmetics, these detectors need to be operated at a temperature of about 155 K.
Introduction and goal
Principle: heat exchange
Principle: nitrogen way out
Principle: Defogging system
Principle: temperature regulation
Principle: Nitrogen re-filling
Anti-overflow system
Thermal balance
Mosaic plate
Cooling system integration
Dewar integration
Measured performances
RELATED LINKS:
VST home page
OMEGA-CAM homepage
DOWNLOADS:
Early Article
INTEGRATION RESPONSIBLE:
Jean Louis Lizon
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