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Title:
AMBER instrument control software
Authors:
leCoarer, Etienne P.; Zins, Gerard; Gluck, Laurence; Duvert, Gilles; Driebe, Thomas; Ohnaka, Keiichi; Heininger, Matthias; Connot, Claus; Behrend, Jan; Dugue, Michel; Clausse, Jean Michel; Millour, Florentin
Affiliation:
AA(Lab. d'Astrophysique de l'Observatoire de Grenoble (France)), AB(Lab. d'Astrophysique de l'Observatoire de Grenoble (France)), AC(Lab. d'Astrophysique de l'Observatoire de Grenoble (France)), AD(Lab. d'Astrophysique de l'Observatoire de Grenoble (France)), AE(Max-Planck-Institut fur Radioastronomie (Germany)), AF(Max-Planck-Institut fur Radioastronomie (Germany)), AG(Max-Planck-Institut fur Radioastronomie (Germany)), AH(Max-Planck-Institut fur Radioastronomie (Germany)), AI(Max-Planck-Institut fur Radioastronomie (Germany)), AJ(Observatoire de la Cote d'Azur (France)), AK(Observatoire de la Cote d'Azur (France)), AL(Lab. d'Astrophysique de l'Observatoire de Grenoble (France) and Univ. de Nice (France))
Publication:
Ground-based Instrumentation for Astronomy. Edited by Alan F. M. Moorwood and Iye Masanori. Proceedings of the SPIE, Volume 5492, pp. 1423-1430 (2004). (SPIE Homepage)
Publication Date:
09/2004
Origin:
SPIE
DOI:
10.1117/12.551301
Bibliographic Code:
2004SPIE.5492.1423L

Abstract

AMBER (Astronomical Multiple BEam Recombiner) is a 3 aperture interferometric recombiner operating between 1 and 2.5 um, for the Very Large Telescope Interferometer (VLTI). The control software of the instrument, based on the VLT Common Software, has been written to comply with specific features of the AMBER hardware, such as the Infrared detector read out modes or piezo stage drivers, as well as with the very specific operation modes of an interferomtric instrument. In this respect, the AMBER control software was designed to insure that all operations, from the preparation of the observations to the control/command of the instrument during the observations, would be kept as simple as possible for the users and operators, opening the use of an interferometric instrument to the largest community of astronomers. Peculiar attention was given to internal checks and calibration procedures both to evaluate data quality in real time, and improve the successes of long term UV plane coverage observations.
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