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By Gert G. Schlessinger

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That will give us about 1/10 wave accuracy across our wavefront and let us close the loop at around 10 Hz. So, cranking all these assumptions into the bigger assumption, we find out that we need a magnitude 12 star or brighter. 96 m stars/rad 2 . 4) For visible wavelengths, there are about 150,000 stars/rad2 with magnitude greater than m = 12. For longer wavelengths, things get a little better, but 150,000 seems like a lot until we remember that Carl Sagan said that there are billions and billions.

If  >0, the Strehl is between 1 and 0 and the intensity is reduced. In an adaptive optics 2 M. Born, E. , Pergamon, Oxford, 1975. 110. org/terms 24 Chapter 2 system, where our objective is to reduce the wavefront error to better propagate a laser or transmit an image, we can say how well it performs by stating the residual Strehl ratio of the optical system. If the wavefront error is constant but the beam is jittering,3 we add another term to show the effect. With a single-axis angular root-mean-square jitter motion jit, an rms wavefront error , a peak intensity I0 from Eq.

Am. 56, pp. 1380-1384 (1966). D. L. Fried, “Anisoplanatism in adaptive optics,” J. Opt. Soc. Am. 72, pp. 52-61 (1982). R. J. Noll, “Zernike polynomials and atmospheric turbulence,” J. Opt. Soc. Am. 66, pp. 207-211 (1976). D. P. Greenwood, “Bandwidth specification for adaptive optics systems,” J. Opt. Soc. Am. 67, pp. 390-393 (1977). 110. org/terms Chapter 5 Laser guide stars — beacons in the wilderness Knowledge of the aberrated wavefront is the critical input for an adaptive optics system. Measuring the wavefront requires sufficient signal to keep the estimation error low.

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