Models for VLTI fringe sensor units: FINITO and PRIMA FSUs

Donata Bonino; Mario Gai; Leonardo Corcione; Giuseppe Massone

doi:10.1117/12.550361

20 October 2004 Models for VLTI fringe sensor units: FINITO and PRIMA FSUs

Donata Bonino, Mario Gai, Leonardo Corcione, Giuseppe Massone

Proceedings Volume 5491, New Frontiers in Stellar Interferometry; (2004) https://doi.org/10.1117/12.550361
Event: SPIE Astronomical Telescopes + Instrumentation, 2004, Glasgow, United Kingdom

Abstract

The VLTI system foresees two generations of fringe sensor: FINITO and PRIMA FSUs. The former is dedicated to H band; it controls the internal OPD with a temporal modulation with an external reference OPD. The latter, working with the ABCD model and in K band, is based on the introduction of known phase offsets for the interferometric signal (spatial phase modulation) and on the measurement of the corresponding combined power. Simulation models for both FSUs are developed with Matlab. Instrumental parameters, i.e. phase, transmission, visibility, are tabulated for ease of maintenance and to speed execution time. For the use of siderostats, due to fast turbulence, the need for intensity calibration arises. Assuming slow intensity variations with respect to phase variations, different algorithms can apply, yielding to numerical control of perturbations as a function of model parameters.

Citation Download Citation

Donata Bonino, Mario Gai, Leonardo Corcione, and Giuseppe Massone "Models for VLTI fringe sensor units: FINITO and PRIMA FSUs", Proc. SPIE 5491, New Frontiers in Stellar Interferometry, (20 October 2004); https://doi.org/10.1117/12.550361

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