Figure 15 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 15.

Left: power spectral densities of the differential OPD variations between the two AO-corrected LBT apertures in closed loop (blue line) and open loop (black line). Middle, corresponding reverse cumulative OPD variations showing the improvement in stability over 20 s from 5 μm rms in open loop to ∼400 nm rms in closed loop. Right: corresponding frequency response. Data obtained on 2015 February 4 on the bright star μ Gem. Loop gains were K_p = 1, K_i = 300, and K_d = 0.

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