Figure 5 from NULLING DATA REDUCTION AND ON-SKY PERFORMANCE OF THE LARGE BINOCULAR TELESCOPE INTERFEROMETER

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NULLING DATA REDUCTION AND ON-SKY PERFORMANCE OF THE LARGE BINOCULAR TELESCOPE INTERFEROMETER

Authors: D. Defrère, P. M. Hinz, B. Mennesson, W. F. Hoffmann, R. Millan-Gabet, A. J. Skemer, V. Bailey, W. C. Danchi, E. C. Downey, O. Durney, P. Grenz, J. M. Hill, T. J. McMahon, M. Montoya, E. Spalding, A. Vaz, O. Absil, P. Arbo, H. Bailey, G. Brusa, G. Bryden, S. Esposito, A. Gaspar, C. A. Haniff, G. M. Kennedy, J. M. Leisenring, L. Marion, M. Nowak, E. Pinna, K. Powell, A. Puglisi, G. Rieke, A. Roberge, E. Serabyn, R. Sosa, K. Stapeldfeldt, K. Su, A. J. Weinberger, and M. C. Wyatt

2016 The Astrophysical Journal 824 66.

Provider: AAS Journals

Caption: Figure 5.

Block diagram of LBTI OPD controller. The measured phase is first unwrapped and then goes through a classical PID controller. A peaking filter is also used to improve the rejection of specific vibration frequencies. An outer loop running at typically 1 Hz is used to monitor the group delay and capture occasional fringe jumps. In addition, real-time OPD variations induced by the LBT structure are measured by accelerometers all over the telescope (OVMS system) and feed-forwarded to the FPC. Differential tip/tilt is controlled following the same principle, except for the unwrapper and the outer loop.

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