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          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents



ID: 559073.0, MPI für Astronomie / Publikationen_mpia
The MCAO systems within LINC-NIRVANA: control aspects beyond wavefront correction
Authors:Bertram, T.; Arcidiacono, C.; Berwein, J.; Bizenberger, P.; Briegel, F.; Diolaiti, E.; Farinato, J.; Gässler, W.; Herbst, T. M.; Hofferbert, R.; Kittmann, F.; Kürster, M.; Ragazzoni, R.; Schreiber, L.; Trowitzsch, J.; Viotto, V.
Publisher:SPIE
Date of Publication (YYYY-MM-DD):2010
Title of Proceedings:Adaptive Optics Systems II
Start Page:77361S-77361S
End Page:10
Volume (in Series):7736
Name of Conference/Meeting:Adaptive Optics Systems II
Audience:Not Specified
Abstract / Description:LINC-NIRVANA is the near-infrared homothetic imaging camera for the Large Binocular Telescope. Once operational, it will provide an unprecedented combination of angular resolution, sensitivity and field of view. Its layer-oriented MCAO systems (one for each arm of the interferometer) are conjugated to the ground layer and an additional layer in the upper atmosphere. In this contribution MCAO wavefront control is discussed in the context of the overall control scheme for LINC-NIRVANA. Special attention is paid to a set of auxiliary control tasks which are mandatory for MCAO operation: The Fields of View of each wavefront sensor in the instrument have to be derotated independent from each other and independently from the science field. Any wavefront information obtained by the sensors has to be matched to the time invariant modes of the deformable mirrors in the system. The tip/tilt control scheme is outlined, in which atmospheric, but also instrumental tip/tilt corrections are sensed with the high layer wavefront sensor and corrected by the adaptive secondary mirror of the LBT. Slow image motion effects on the science detector have to be considered, which are caused by flexure in the non-common path between AO and the science camera, atmospheric differential refraction, and alignment tolerances of the derotators. Last but not least: The sensor optics (pyramids) have to be accurately positioned at the images of natural reference stars.
Comment of the Author/Creator:Date: 2010, July 1, 2010
External Publication Status:published
Document Type:Conference-Paper
Communicated by:N. N.
Affiliations:MPI für Astronomie
Identifiers:URL:http://adsabs.harvard.edu/abs/2010SPIE.7736E..60B
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