By François Roddier
Adaptive optics is a robust new process used to sharpen telescope photographs blurred by way of the Earth's surroundings. This authoritative e-book is the 1st devoted to using adaptive optics in astronomy. almost always built for defence functions, the means of adaptive optics has just recently been brought in astronomy. Already it has allowed ground-based telescopes to supply photographs with sharpness rivalling these from the Hubble house Telescope. The strategy is predicted to revolutionise the way forward for ground-based optical astronomy. Written by way of a global workforce of specialists who've pioneered the improvement of the sector, this well timed quantity presents either a rigorous advent to the strategy and a entire overview of present and destiny platforms. it's set to develop into the normal reference for graduate scholars, researchers and optical engineers in astronomy and different components of technology the place adaptive optics is discovering intriguing new purposes.
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Extra info for Adaptive Optics in Astronomy
Astronomers are used to de®ning image quality in terms of the full width at half maximum (fwhm) of a point source image. This is an acceptable criterion as long as the image pro®le is independent of seeing quality. In Chapter 2 we saw that the pro®le of an uncompensated, seeinglimited point source image is nearly Gaussian and indeed independent of seeing conditions. Only the width of the pro®le changes. However, we have also seen that a compensated image consists of a narrow diffraction-limited core surrounded by a halo of light scattered by the uncompensated residual wave-front errors.
One can then de®ne the ef®ciency of a real system by comparison with this theoretical model. 2 Modal wave-front representation Atmospheric turbulence produces randomly distorted wave fronts. The wavefront corrector attempts to compensate the distortions with an N-parameter ®t. In some cases a good ®t may be obtained. In other cases the ®t will be poorer. The residual wave-front error is clearly random. The most ef®cient AO system is the one which on the average produces the smallest error. The solution to this optimization problem can be found by expanding the atmospheric wave fronts in a series of orthogonal functions.
J. Opt. Soc. Am. 67, 375±8. Johnson, H. L. (1966) Astronomical measurements in the infrared. Ann. Rev. Astron. Astrophys. 4, 201. Noll, R. J. (1976) Zernike polynomials and atmospheric turbulence. J. Opt. Soc. Am. 66, 207±11. Noll, R. J. (1978) Phase estimates from slope-type wave-front sensors. J. Opt. Soc. Am. 68, 139±40. Roddier, F. (1981) The effects of atmospheric turbulence in optical astronomy. Progress in Optics 19, 281±376. Roddier, F. (1994) The problematic of adaptive optics design. In: Adaptive Optics for Astronomy, eds D.