Abstract

The residual aberrations of adaptive optics (AO) images can be removed by the speckle reconstruction method. To achieve accurate photometry, the knowledge of the speckle transfer function (STF) is necessary. In this Letter, a new method is proposed to evaluate the STF for speckle image reconstruction based on the partial correction AO. The STF is divided into two sections: the low-frequency section and the high-frequency section, and two different generalized Fried parameters for the partial wavefront compensation are used to calculate the STF values of those two different sections. This method is tested with the different seeing conditions and the various correction modes. The results show that the combined STFs have satisfactory agreement with the simulated AO STFs and give more accurate results than the STFs obtained from the traditional spectral ratio method. Further discussions show that the method is more reliable when the AO is operated in low-order correction mode because the approximation of the STF and the two generalized Fried parameters have better accuracy when the pupil diameter is much larger than those generalized Fried parameters.

© 2014 Optical Society of America

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References

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2010 (1)

2007 (1)

2006 (1)

K. Puschmann and M. Sailer, Astron. Astrophys. 454, 1011 (2006).
[CrossRef]

2005 (1)

C. Denker, D. Mascarinas, Y. Xu, W. Cao, G. Yang, H. Wang, P. R. Goode, and T. Rimmele, Sol. Phys. 227, 217 (2005).
[CrossRef]

2001 (1)

2000 (1)

1998 (1)

1990 (1)

N. A. Roddier, Opt. Eng. 29, 1174 (1990).
[CrossRef]

1988 (1)

1984 (1)

1976 (1)

1973 (1)

1970 (1)

A. Labeyrie, Astron. Astrophys. 6, 85 (1970).

Cagigal, M. P.

Canales, V. F.

Cao, W.

C. Denker, D. Mascarinas, Y. Xu, W. Cao, G. Yang, H. Wang, P. R. Goode, and T. Rimmele, Sol. Phys. 227, 217 (2005).
[CrossRef]

Denker, C.

C. Denker, D. Mascarinas, Y. Xu, W. Cao, G. Yang, H. Wang, P. R. Goode, and T. Rimmele, Sol. Phys. 227, 217 (2005).
[CrossRef]

Goode, P. R.

C. Denker, D. Mascarinas, Y. Xu, W. Cao, G. Yang, H. Wang, P. R. Goode, and T. Rimmele, Sol. Phys. 227, 217 (2005).
[CrossRef]

Hardy, J. W.

J. W. Hardy, Adaptive Optics for Astronomical Telescopes (Oxford University, 1998).

Korff, D.

Labeyrie, A.

A. Labeyrie, Astron. Astrophys. 6, 85 (1970).

Mascarinas, D.

C. Denker, D. Mascarinas, Y. Xu, W. Cao, G. Yang, H. Wang, P. R. Goode, and T. Rimmele, Sol. Phys. 227, 217 (2005).
[CrossRef]

Noll, R. J.

Puschmann, K.

K. Puschmann and M. Sailer, Astron. Astrophys. 454, 1011 (2006).
[CrossRef]

Rimmele, T.

C. Denker, D. Mascarinas, Y. Xu, W. Cao, G. Yang, H. Wang, P. R. Goode, and T. Rimmele, Sol. Phys. 227, 217 (2005).
[CrossRef]

Roddier, F.

F. Roddier, in Progress in Optics (North-Holland, 1981), Vol. 19, pp. 281–376.

Roddier, N. A.

N. A. Roddier, Opt. Eng. 29, 1174 (1990).
[CrossRef]

Sailer, M.

K. Puschmann and M. Sailer, Astron. Astrophys. 454, 1011 (2006).
[CrossRef]

Von Der Luehe, O.

von der Lühe, O.

Wang, H.

C. Denker, D. Mascarinas, Y. Xu, W. Cao, G. Yang, H. Wang, P. R. Goode, and T. Rimmele, Sol. Phys. 227, 217 (2005).
[CrossRef]

Wöger, F.

Xu, Y.

C. Denker, D. Mascarinas, Y. Xu, W. Cao, G. Yang, H. Wang, P. R. Goode, and T. Rimmele, Sol. Phys. 227, 217 (2005).
[CrossRef]

Yang, G.

C. Denker, D. Mascarinas, Y. Xu, W. Cao, G. Yang, H. Wang, P. R. Goode, and T. Rimmele, Sol. Phys. 227, 217 (2005).
[CrossRef]

Appl. Opt. (2)

Astron. Astrophys. (2)

A. Labeyrie, Astron. Astrophys. 6, 85 (1970).

K. Puschmann and M. Sailer, Astron. Astrophys. 454, 1011 (2006).
[CrossRef]

J. Opt. Soc. Am. (2)

J. Opt. Soc. Am. A (3)

Opt. Eng. (1)

N. A. Roddier, Opt. Eng. 29, 1174 (1990).
[CrossRef]

Opt. Lett. (2)

Sol. Phys. (1)

C. Denker, D. Mascarinas, Y. Xu, W. Cao, G. Yang, H. Wang, P. R. Goode, and T. Rimmele, Sol. Phys. 227, 217 (2005).
[CrossRef]

Other (2)

J. W. Hardy, Adaptive Optics for Astronomical Telescopes (Oxford University, 1998).

F. Roddier, in Progress in Optics (North-Holland, 1981), Vol. 19, pp. 281–376.

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Figures (6)

Fig. 1.
Fig. 1.

AO STF from the simulation, STF from the traditional SPR method, and the combined STF. The correction number is 16 and D/r0=38.4. The calculated Fried parameters are D/ρ0=19.8531 and D/ρ0=14.5873.

Fig. 2.
Fig. 2.

AO STF from the simulation, STF from the traditional SPR method, and combined STF. The correction number is 30 and D/r0=38.4. The calculated Fried parameters are D/ρ0=17.9712 and D/ρ0=10.5171.

Fig. 3.
Fig. 3.

Cross sections of the reconstructed images from the STF calculated by the SPR method and the combined STF. The Airy disk and the images without and with AO partial compensation are also shown for comparison.

Fig. 4.
Fig. 4.

Cross sections of reconstructed images from the STF calculated by the SPR method and the combined STF. The Airy disk and the images without and with AO partial compensation are also shown for comparison.

Fig. 5.
Fig. 5.

Strehl ratios of the reconstructed images from the STFs of the traditional SPR method and our combined STFs, when the seeing condition is D/r0=38.4 and correction numbers J are 6, 10, 14, 18, 22, 26, 30, 34, 38, and 42.

Fig. 6.
Fig. 6.

Strehl ratios of the reconstructed images from the STFs of the traditional SPR method and our combined STFs when the correction number J is 16 and the seeing conditions D/r0 are 11.7, 20, 30, 38.4, and 50.

Equations (7)

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STF(f⃗)={|Sir0(f⃗)|2f⃗f⃗c0.342(r0D)2MTel(f⃗)f⃗>f⃗c.
STF(f⃗)={|Siρ0(f⃗)|2f⃗f⃗c0.342(ρ0D)2MTel(f⃗)f⃗>f⃗c,
ϕ(r,θ)=i=1aiZi(r,θ),
ϕR(r,θ)=i=J+1aiZi(r,θ).
ΔJ=ϕ2j=1J|aj|2=j=J+1|aj|2=coef(J)(Dr0)5/3,
ρ0=0.286J(0.362)(3.44coef(J))35r0.
ρ0=(0.134coef(J))3/5r0.

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