Abstract

Cn2 profile monitoring usually relies on the exploitation of wavefront slope correlations or of scintillation pattern correlations. Scintillation is rather sensitive to high turbulence layers whereas wavefront slope correlations are mainly due to layers close to the receiving plane. Wavefront slope and scintillation correlations are therefore complementary. A Shack–Hartmann wavefront sensor (SHWFS) is currently used to measure wavefront slopes only. But it could also be sensitive to scintillation as the average intensity in a given subaperture can be obtained by adding pixel intensities in the subaperture focal plane up. With slopes and scintillation being recorded simultaneously, their correlation is also theoretically available. We propose to exploit wavefront slope and scintillation correlations recorded with a SHWFS to retrieve the Cn2 profile. Two measurement methods are exposed. In CO-SLIDAR (Coupled SLODAR SCIDAR), correlations of SHWFS data recorded on two separated stars are exploited. SCO-SLIDAR (Single CO-SLIDAR) relies on the same principle as CO-SLIDAR, but SHWFS data are recorded on a single star. Results of Cn2 estimation from simulated SHWFS data are presented.

© 2007 Optical Society of America

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References

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2005

C. Petit, J.-M. Conan, C. Kulcsar, H.-F. Raynaud, T. Fusco, J. Montri, and D. Rabaud, C. R. Phys. 6, 1059 (2005).
[CrossRef]

2004

B. Le Roux, J.-M. Conan, C. Kulcsár, H.-F. Raynaud, L. M. Mugnier, and T. Fusco, J. Opt. Soc. Am. A 21, 1261 (2004).
[CrossRef]

R. W. Wilson, J. Bate, J. C. Guerra, N. N. Hubin, M. Sarazin, C. D. Saunter, Proc. SPIE 5490, 758 (2004).
[CrossRef]

2003

A. Tokovinin, V. Kornilov, N. Shatsky, and O. Voziakova, Mon. Not. R. Astron. Soc. 343, 891 (2003).
[CrossRef]

V. Kornilov, A. A. Tokovinin, O. Vozyakova, A. Zaitsev, N. Shatsky, S. F. Potanin, and M. S. Sarazin, Proc. SPIE 4839, 837 (2003).
[CrossRef]

2002

R. W. Wilson, Mon. Not. R. Astron. Soc. 337, 103 (2002).
[CrossRef]

2001

2000

T. Fusco, J.-M. Conan, L. M. Mugnier, V. Michau, and G. Rousset, Astron. Astrophys. Suppl. Ser. 142, 149 (2000).
[CrossRef]

1998

A. Fuchs, M. Tallon, and J. Vernin, Astron. Soc. Pac. 110, 86 (1998).
[CrossRef]

V. A. Klueckers, N. J. Wooder, T. W. Nicholls, M. J. Adcock, I. Munro, and J. C. Dainty, Astron. Astrophys. Suppl. Ser. 130, 141 (1998).
[CrossRef]

1995

J. Vernin and C. Munoz-Tunon, Publ. Astron. Soc. Pac. 107, 265 (1995).
[CrossRef]

1994

J. Vernin and C. Munoz-Tunón, Astron. Astrophys. 284, 311 (1994).

1992

P. Hansen, SIAM Rev. 34, 561 (1992).
[CrossRef]

1988

1966

D. L. Fried, J. Opt. Soc. Am. A 56, 1372 (1966).
[CrossRef]

Appl. Opt.

Astron. Astrophys.

J. Vernin and C. Munoz-Tunón, Astron. Astrophys. 284, 311 (1994).

Astron. Astrophys. Suppl. Ser.

T. Fusco, J.-M. Conan, L. M. Mugnier, V. Michau, and G. Rousset, Astron. Astrophys. Suppl. Ser. 142, 149 (2000).
[CrossRef]

V. A. Klueckers, N. J. Wooder, T. W. Nicholls, M. J. Adcock, I. Munro, and J. C. Dainty, Astron. Astrophys. Suppl. Ser. 130, 141 (1998).
[CrossRef]

Astron. Soc. Pac.

A. Fuchs, M. Tallon, and J. Vernin, Astron. Soc. Pac. 110, 86 (1998).
[CrossRef]

C. R. Phys.

C. Petit, J.-M. Conan, C. Kulcsar, H.-F. Raynaud, T. Fusco, J. Montri, and D. Rabaud, C. R. Phys. 6, 1059 (2005).
[CrossRef]

J. Opt. Soc. Am. A

Mon. Not. R. Astron. Soc.

R. W. Wilson, Mon. Not. R. Astron. Soc. 337, 103 (2002).
[CrossRef]

A. Tokovinin, V. Kornilov, N. Shatsky, and O. Voziakova, Mon. Not. R. Astron. Soc. 343, 891 (2003).
[CrossRef]

Proc. SPIE

R. W. Wilson, J. Bate, J. C. Guerra, N. N. Hubin, M. Sarazin, C. D. Saunter, Proc. SPIE 5490, 758 (2004).
[CrossRef]

V. Kornilov, A. A. Tokovinin, O. Vozyakova, A. Zaitsev, N. Shatsky, S. F. Potanin, and M. S. Sarazin, Proc. SPIE 4839, 837 (2003).
[CrossRef]

Publ. Astron. Soc. Pac.

J. Vernin and C. Munoz-Tunon, Publ. Astron. Soc. Pac. 107, 265 (1995).
[CrossRef]

SIAM Rev.

P. Hansen, SIAM Rev. 34, 561 (1992).
[CrossRef]

Other

R. E. Hufnagel, presented at Topical Meeting on Optical Propagation through Turbulence, July 9-11, 1974, Boulder, Colo., paper Wal-1.

V. I. Tatarski, Wave Propagation in a Turbulent Medium (Dover, 1961).

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Figures (2)

Fig. 1
Fig. 1

Contributions of the turbulent layers to C mes terms. Signal amplitude is coded in grey levels with a logarithmic scale. Every plot has been normalized by its maximum value.

Fig. 2
Fig. 2

Inversion results from CO-SLIDAR, SCO-SLIDAR, and SLODAR data.

Equations (2)

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C mes = M C n 2 + C d + u ,
J = ( C ̂ mes M S ) t C c o n v ( C ̂ mes M S ) + β H 1 Δ S 2 .

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