Abstract

We present the results of the co-phasing closed loop performed with a pyramid wavefront sensor for what we believe to be the first time in the presence of emulated atmospheric disturbance. The performance of the co-phasing loop is significantly improved by applying two spatial filters in the sensor signal space. The first is a zonal filter applied to the interaction matrix before the computation of the reconstructor; the second is a modal filter applied to the sensor signals before the correction command computation. The presented laboratory results demonstrate that, applying both filters, the time requested to average out the atmospheric disturbance in each loop step is reduced by 2 orders of magnitude, improving the loop stability and accuracy.

© 2007 Optical Society of America

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  1. G. Chanan, M. Troy, I. Crossfield, J. Nelson, and T. Mast, Proc. SPIE 6267, 62672V (2006).
  2. S. Esposito and N. Devaney, in Beyond Conventional Adaptive Optics, Vol. 58 of ESO Conference and Workshop Proceedings (European Southern Observatory, 2001), pp. 161-166.
  3. That is because there will be tens of segments on the diameter of the ELT primary mirror and the signal is localized on the segments edges.
  4. S. Esposito and A. Riccardi, Astron. Astrophys. 369, L9 (2001).
  5. N. Yaitskova, F. Gonte, F. Derie, L. Noethe, I. Surdej, R. Karban, K. Dohlen, M. Langlois, S. Esposito, E. Pinna, M. Reyes, L. Montoya, and D. Terrett, Proc. SPIE 626762672Z (2006).
  6. S. Esposito, O. Feeney, and A. Riccardi, Proc. SPIE 4007, 416 (2000).
    [CrossRef]
  7. S. Esposito, E. Pinna, A. Puglisi, A. Tozzi, and P. Stefanini, Opt. Lett. 30, 2572 (2005).
    [CrossRef]

2006

G. Chanan, M. Troy, I. Crossfield, J. Nelson, and T. Mast, Proc. SPIE 6267, 62672V (2006).

N. Yaitskova, F. Gonte, F. Derie, L. Noethe, I. Surdej, R. Karban, K. Dohlen, M. Langlois, S. Esposito, E. Pinna, M. Reyes, L. Montoya, and D. Terrett, Proc. SPIE 626762672Z (2006).

2005

2001

S. Esposito and A. Riccardi, Astron. Astrophys. 369, L9 (2001).

2000

S. Esposito, O. Feeney, and A. Riccardi, Proc. SPIE 4007, 416 (2000).
[CrossRef]

Astron. Astrophys.

S. Esposito and A. Riccardi, Astron. Astrophys. 369, L9 (2001).

Opt. Lett.

Proc. SPIE

N. Yaitskova, F. Gonte, F. Derie, L. Noethe, I. Surdej, R. Karban, K. Dohlen, M. Langlois, S. Esposito, E. Pinna, M. Reyes, L. Montoya, and D. Terrett, Proc. SPIE 626762672Z (2006).

S. Esposito, O. Feeney, and A. Riccardi, Proc. SPIE 4007, 416 (2000).
[CrossRef]

G. Chanan, M. Troy, I. Crossfield, J. Nelson, and T. Mast, Proc. SPIE 6267, 62672V (2006).

Other

S. Esposito and N. Devaney, in Beyond Conventional Adaptive Optics, Vol. 58 of ESO Conference and Workshop Proceedings (European Southern Observatory, 2001), pp. 161-166.

That is because there will be tens of segments on the diameter of the ELT primary mirror and the signal is localized on the segments edges.

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