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Journal of the Optical Society of America

Journal of the Optical Society of America

  • Vol. 69, Iss. 5 — May. 1, 1979
  • pp: 786–790

Estimation of spatial power spectra in speckle interferometry

J. C. Dainty and A. H. Greenaway  »View Author Affiliations

JOSA, Vol. 69, Issue 5, pp. 786-790 (1979)

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Calculations of the signal-to-noise ratio (SNR) of estimates of the power spectra of spatially varying random processes, such as stellar speckle patterns, usually include realizations that contain less than two detected photons. It is shown in this paper that if these cases are excluded from the analysis procedure either implicitly or explicitly, then under the usual definition of SNR, the overall SNR of an estimate can increase by up to a factor of N¯-½., where N¯ ≪ 1 is the average number of detected photons per realization.

© 1979 Optical Society of America

J. C. Dainty and A. H. Greenaway, "Estimation of spatial power spectra in speckle interferometry," J. Opt. Soc. Am. 69, 786-790 (1979)

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  1. F. Roddier, "Signal-to-noise ratio in speckle interferometry," in Imaging in Astronomy, AAS/SAO/OSA/SPIE Topical Meeting. Preprints paper Th C6, Boston 1975 (unpublished).
  2. J. W. Goodman and J. F. Belsher, "Fundamental limitations in linear invariant restoration of atmospherically degraded images," SPIE Seminar Proc., 75, 141–154 (1976).
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  4. M. G. Miller, "Noise considerations in stellar speckle interferometry," J. Opt. Soc. Am., 67, 1176–1184 (1977).
  5. J. C. Dainty and A. H. Greenaway, "The signal-to-noise ratio in speckle interferometry," Proc. IAU Colloquium No. 50, "High Angular Resolution Stellar Interferometry," Maryland Aug/Sept. 1978 (available from Chatterton Astronomy Department, University of Sydney, NSW, Australia 2006, $20 (Australian) + postage).
  6. A. H. Greenaway, "The signal-to-noise ratio in long baseline stellar interferometry," Optica Acta (in press).
  7. J. J. Burke and J. B. Breckinridge, "Passive imaging through the turbulent atmosphere: Fundamental limits on the spatial frequency resolution of a rotational shearing interferometer," J. Opt. Soc. Am., 68, 67–77 (1978).
  8. A. Labeyrie, "High resolution techniques in optical astronomy," in Progress in Optics; Vol. 14, edited by E. Wolf, (North-Holland, Amsterdam, 1976) p 47–87.
  9. J. C. Dainty, "The transfer function, signal-to-noise ratio and limiting magnitude in stellar speckle interferometry," Mon. Not. R. Astr. Soc., 169, 631–641 (1974).
  10. J. C. Dainty, "Computer simulations of speckle interferometry of binary stars in the photon counting mode," Mon. Not. R. Astr. Soc., 183, 223–236 (1978).
  11. J. G. Walker, "Optimum exposure time and filter bandwidth in speckle interferometry," (see Ref 5).
  12. D. Korff, "Analysis of a method for obtaining near diffractionlimited information in the presence of atmospheric turbulence," J. Opt. Soc. Am., 63, 971–980 (1973).
  13. D. L. Fried, "Optical resolution through a randomly inhomogeneous medium," J. Opt. Soc. Am., 56, 1372–1379 (1966).
  14. The factor 0.435 on the bottom line of Eq. (21) arises from the normalization of the overall transfer function to 1.0 at the origin. Defining a normalized seeing transfer function, [Equation] Eq. (7) of Ref. 5 can be written, for r0D, [Equation] where T0(ν) is the telescope OTF and P is the area of the (unshaded) pupil. With P = πD2/4, performing the integration yields [Equation]

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