16 June 2000 Field stabilization on the ESO VLT telescopes
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The Field Stabilization functionality compensates for image motions, mainly due to wind gusts, with a frequency of up to 50 Hz. Position errors are detected with a CCD mounted in the guide probe, and the correction vectors are passed to the secondary mirror, which can perform tip/tilt corrections with a frequency up to 100 Hz. This functionality is in regular use on the first two VLT telescopes, Antu and Kueyen; on Antu in operational use since 1st of April 1999 and on Kueyen for commissioning tests. In fact, Field Stabilization is ALWAYS used during observations. It is started as an integral part of the setting of the telescope. This paper describes the software and hardware that performs the Field Stabilization functionality. The architecture of the system, both software and hardware, is presented, with a discussion about problems and special solutions. The actual status, including some results from the commissioning and operational phases of the two first telescopes, is described. Finally, we present a short discussion about possible future extensions and improvements.
© (2000) COPYRIGHT Society of Photo-Optical Instrumentation Engineers (SPIE). Downloading of the abstract is permitted for personal use only.
Gianluca Chiozzi, Gianluca Chiozzi, Robert Karban, Robert Karban, Krister Wirenstrand, Krister Wirenstrand, } "Field stabilization on the ESO VLT telescopes", Proc. SPIE 4009, Advanced Telescope and Instrumentation Control Software, (16 June 2000); doi: 10.1117/12.388382; https://doi.org/10.1117/12.388382


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