Abstract

We present a compact optical design for a multireference Shack–Hartmann-based wavefront sensor (WFS) for multiconjugate adaptive optical systems. The key component of this WFS design is a field lenslet array that separates the exit pupil images in the sensing plane for all reference sources. An analytical method for WFS optical design is presented, and the optimal strategy for selecting optical components from a discrete set is outlined. The feasibility of the WFS design has been demonstrated for a prototype WFS system in a laboratory setup with five reference sources and two deformable mirrors representing a wavefront-distorting medium.

© 2005 Optical Society of America

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References

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  1. G. Rousset, in Adaptive Optics in Astronomy, F. Roddier, ed. (Cambridge U. Press, 1999), pp. 91–130.
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    [CrossRef] [PubMed]

2005 (1)

2003 (1)

2000 (1)

1994 (1)

1985 (1)

R. Foy and A. Labeyrie, Astron. Astrophys. 152, 129 (1985).

1976 (1)

Ageorges, N.

N. Ageorges and J. C. Dainty, Laser Guide Star Adaptive Optics for Astronomy (Kluwer Academic, 2000).
[CrossRef]

Beckers, J. M.

J. M. Beckers, in European Southern Observatory Conference Proceedings, M. H. Ulrich, ed. (European Southern Observatory, 1988), pp. 693–703.

Dainty, C.

Dainty, J. C.

N. Ageorges and J. C. Dainty, Laser Guide Star Adaptive Optics for Astronomy (Kluwer Academic, 2000).
[CrossRef]

Dalimier, E.

Foy, R.

R. Foy and A. Labeyrie, Astron. Astrophys. 152, 129 (1985).

Fried, D. L.

Greenwood, D. P.

Johnston, D. C.

Labeyrie, A.

R. Foy and A. Labeyrie, Astron. Astrophys. 152, 129 (1985).

Lloyd-Hart, M.

Milton, N. M.

Moreno-Barriuso, E.

Navarro, R.

Rousset, G.

G. Rousset, in Adaptive Optics in Astronomy, F. Roddier, ed. (Cambridge U. Press, 1999), pp. 91–130.
[CrossRef]

Welsh, B. M.

Astron. Astrophys. (1)

R. Foy and A. Labeyrie, Astron. Astrophys. 152, 129 (1985).

J. Opt. Soc. Am. (1)

J. Opt. Soc. Am. A (2)

Opt. Express (1)

Opt. Lett. (1)

Other (3)

N. Ageorges and J. C. Dainty, Laser Guide Star Adaptive Optics for Astronomy (Kluwer Academic, 2000).
[CrossRef]

G. Rousset, in Adaptive Optics in Astronomy, F. Roddier, ed. (Cambridge U. Press, 1999), pp. 91–130.
[CrossRef]

J. M. Beckers, in European Southern Observatory Conference Proceedings, M. H. Ulrich, ed. (European Southern Observatory, 1988), pp. 693–703.

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Figures (4)

Fig. 1
Fig. 1

Reimaging of telescope pupil P into several separate exit pupils in plane P .

Fig. 2
Fig. 2

SH spots centered in subframes.

Fig. 3
Fig. 3

Optical layout of the multireference WFS.

Fig. 4
Fig. 4

SH spots affected by wavefront aberrations: (a) defocus near the pupil plane, (b) defocus at the upper-altitude plane.

Tables (1)

Tables Icon

Table 1 Major Optical Parameters of the Multireference WFS

Equations (6)

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W = 2 π d α λ .
m = n ( 1 + W max π ) .
γ = m p CCD d SH ,
f SH = π d SH 2 λ ( W max + π ) .
t = f SH + f COL N CCD p CCD ( γ D FL ) .
N CCD = m D FL ( f 2 COL f FL f SH ) ( f FL f COL d SH ) ,

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