Abstract

We propose here a novel way to analyze Shack–Hartmann wavefront sensor images in order to retrieve more modes than the two centroid coordinates per sub-aperture. To do so, we use the linearized focal-plane technique (LIFT) phase retrieval method for each sub-aperture. We demonstrate that we can increase the number of modes sensed with the same computational burden per mode. For instance, we show the ability to control a 21×21 actuator deformable mirror using a 10×10 lenslet array.

© 2014 Optical Society of America

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References

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2013 (1)

2010 (1)

2006 (1)

A. Tokovinin and S. Heathcote, Publ. Astron. Soc. Pac. 118, 1165 (2006).
[CrossRef]

2004 (1)

2001 (1)

2000 (1)

1999 (1)

1995 (1)

1994 (1)

1992 (2)

F. Rigaut and E. Gendron, Astron. Astrophys. 261, 677 (1992).

R. G. Paxman, T. J. Schulz, and J. R. Fienup, J. Opt. Soc. Am. A 9, 1072 (1992).
[CrossRef]

1976 (1)

1971 (1)

R. Shack and B. Platt, J. Opt. Soc. Am. A 61, 656 (1971).

Atta, L. V.

Bille, J. F.

Bliss, E. S.

Cannon, R. C.

Conan, J.-M.

Dailey, M. J.

Feldman, M.

Fienup, J. R.

Fusco, T.

Gendron, E.

F. Rigaut and E. Gendron, Astron. Astrophys. 261, 677 (1992).

Goelz, S.

Gonsalves, R. A.

Grey, A. A.

Grimm, B.

Heathcote, S.

A. Tokovinin and S. Heathcote, Publ. Astron. Soc. Pac. 118, 1165 (2006).
[CrossRef]

Holdener, F. R.

Koch, J. A.

Liang, J.

Meimon, S.

Meynadier, L.

Michau, V.

Mugnier, L. M.

Nicolle, M.

Noll, R. J.

Paxman, R. G.

Plantet, C.

Platt, B.

R. Shack and B. Platt, J. Opt. Soc. Am. A 61, 656 (1971).

Presta, R. W.

Rigaut, F.

F. Rigaut and E. Gendron, Astron. Astrophys. 261, 677 (1992).

Rousset, G.

Sacks, R. A.

Salmon, J. T.

Schulz, T. J.

Seppala, L. G.

Shack, R.

R. Shack and B. Platt, J. Opt. Soc. Am. A 61, 656 (1971).

Toeppen, J. S.

Tokovinin, A.

A. Tokovinin and S. Heathcote, Publ. Astron. Soc. Pac. 118, 1165 (2006).
[CrossRef]

Velluet, M.-T.

Whistler, W. T.

Winters, S. E.

Wonterghem, B. M. V.

Woods, B. W.

Zacharias, R. A.

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Figures (2)

Fig. 1.
Fig. 1.

Noise propagation for a given sub-aperture on local slope estimates with a CoG (red dotted line) and a WCoG (blue dashed line). The noise propagation on local mode estimates with LIFT are plotted in black. Detector readout noise: 10e. For LIFT configuration, a 0.5 rad RMS astigmatism offset is added. The CoG and WCoG curves correspond to diffraction-limited spots (without any astigmatism offset). The cross symbols correspond to a diffractive simulation, whereas the solid lines correspond to the analytic formulas (from [13] for CoG/WCoG).

Fig. 2.
Fig. 2.

Eigenvalues of the interaction matrix on a deformable Gaussian influence function on a 21×21 grid (with 25% coupling between modes) for a 10×10 sub-aperture SH WFS with classical centroiding [see Eqs. (1) and (2)], with a two mode per sub-aperture and a five mode per sub-aperture LIFT estimation. For comparison, we have plotted the eigenvalues obtained for a 20×20 sub-aperture SH WFS with classical centroiding.

Equations (2)

Equations on this page are rendered with MathJax. Learn more.

Y=[sx,1sy,1sx,Npupsy,Npup],YLIFT=[a1,1a2,1a3,1a4,1a5,1a1,Npupa2,Npupa3,Npupa4,Npupa5,Npup].
Mint=[Y(m1)||Y(mNab)];MintLIFT=[YLIFT(m1)||YLIFT(mNab)].

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