Download e-book for kindle: Advances in Electronics and Electron Physics, Vol. 67 by Peter W. Hawkes (ed.)

By Peter W. Hawkes (ed.)

ISBN-10: 0120146673

ISBN-13: 9780120146673

This quantity comprises evaluation articles masking a extensive diversity of subject matters in photograph processing and research. the themes coated contain picture research - which has united and harmonized a bunch of heterogeneous fabric; modern methods to the Fourier remodel; quantity theoretic transforms, that are relatively appealing for discrete, finite signs; using the Wigner distribution - which encodes either spatial and spectral details, for picture filtering; and functions of the idea that of knowledge power. those up to date surveys are meant to supply the reader with entry to the newest leads to the tremendous energetic box of photograph technology.

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16. While this image-form bears little resemblance to Fig. A). It represents an appreciably better first version of r ( x , y ) . Figure 17a and b show image-forms obtained after 30 hybrid input-output iterations starting, respectively, with the direct pseudo-random initial phase estimate and the CPE. The accelerated numerical convergence manifested by the latter is obvious. 16. Image-form of starfield given by the Fourier transform of IF,(u,o)l combined with its crude phase estimate. C. B, it from the given IF,+,,,+,Imakes sense to try and reconstruct the IEm+p,n+vl refer to the definition [Eq.

Further improvement of image-forms obtained after an additional 50 Fienup hybrid input-output iterations, starting from Fig. 9. (a) Puffin, (b) starfield. 1 I. Profiles (plotted logarithmically)through magnitudes of visibilities of puffin and starfield. (a) (F,(u,O)(;(b) 1F,(O, u)l; (c) IF2(u,0)I;(d) IF2(0,u)l. Note that the fringe frequency in (a) and (b) is greater than in (c) and (d). by E - ( v )and defined by (37) B(x. Y I N) where v can be any positive number, but is usually set equal to 1 (defines the magnitude error) or 2 (defines the intensity error).

Profiles through quantities in visibility space, along positive u axis. (a) Magnitude of visibility of foggy starfield; (b) defogging function, W(u,0); (c)defogged visibility magnitude. Subscripts F and DF stand for foggy and defogged, respectively. 22. Image-forms of foggy starfield obtained after a single Fienup cycle (v, = 20, lo), starting with CPE and using (a) defogged visibility magnitude (see Fig. 21c), (b) original visibility magnitude (see Fig. 21a). v, = 80, v3 = 54 R. H. T. MNYAMA Another commonly encountered difficulty is the “partial fog” problem, illustrated by Fig.

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