GALACSI integration and functional tests
2014; SPIE; Volume: 9148; Linguagem: Inglês
10.1117/12.2055159
ISSN1996-756X
AutoresP. La Penna, Stefan Ströbele, E. Aller Carpentier, Javier Argomedo, R. Arsenault, Ralf Conzelmann, Bernard Délabre, R. Donaldson, Michel Duchateau, Enrico Fedrigo, Fernando Gago, N. Hubin, J. Quentin, Paul Jolley, M. Kiekebusch, Jean-Paul Kirchbauer, Barbara Klein, Johann Kolb, H. Kuntschner, Miska Le Louarn, Jean-Louis Lizon, Pierre-Yves Madec, A. Manescau, Leander Mehrgan, B. Sedghi, M. Suárez Valles, C. Soenke, Sébastien Tordo, J. Vernet, Stefano Zampieri,
Tópico(s)Astronomy and Astrophysical Research
ResumoGALACSI is the Adaptive Optics (AO) modules of the ESO Adaptive Optics Facility (AOF) that will correct the wavefront delivered to the MUSE Integral Field Spectrograph. It will sense with four 40×40 subapertures Shack-Hartmann wavefront sensors the AOF 4 Laser Guide Stars (LGS), acting on the 1170 voice-coils actuators of the Deformable Secondary Mirror (DSM). GALACSI has two operating modes: in Wide Field Mode (WFM), with the four LGS at 64" off axis, the collected energy in a 0.2"×0.2" pixel will be enhanced by a factor 2 at 750 nm over a Field of View (FoV) of 1'×1' using the Ground Layer AO (GLAO) technique. The other mode, the Narrow Field Mode (NFM), provides an enhanced wavefront correction (Strehl Ratio (SR) of 5% (goal 10%) at 650 nm) but in a smaller FoV (7.5"×7.5"), using Laser Tomography AO (LTAO), with the 4 LGS located closer, at 10" off axis. Before being shipped to Paranal, GALACSI will be first integrated and fully tested in stand-alone, and then moved to a dedicated AOF facility to be tested with the DSM in Europe. At present the module is fully assembled, its main functionalities have been implemented and verified, and AO system tests with the DSM are starting. We present here the main system features and the results of the internal functional tests of GALACSI.
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