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Statistical properties of the maps are presented as a function of sky coverage, angular resolution, and instrument noise, and the implications of these results for observability of the Doppler peak are discussed. fluid compression in potential peaks àHOT spots in CMB enhanced by (1+6R) because baryons’ inertia makes them compresses in wells and move away from peaks Doppler velocity term: amplitude is given by +/- of this amplitude does not change much; baryon-loaded fluid moves slowly Quantitative treatment of … We have simulated full‐sky maps of the Cosmic Microwave Background (CMB) anisotropy expected from Cold Dark Matter (CDM) models at 0°.5 and 1°.0 angular resolution. J.RTgd,(@? the CMB fluctuations is to increase the amplitude of the power spectrum by approximately 0.25% in the velocity direction, and decrease it correspondingly in the anti-direction. [X+mFWGm($?,p*n>K/2uW@
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Renal artery stenosis: analysis of Doppler waveform parameters and tardus–parvus pattern. Throughout the 1990's constraints on the location of the first peak steadily improved culminating with precise determinations from the TOCO [Miller et al, 1999], Boomerang, [de Bernardis et al, 2000] and Maxima-1 [Hanany et al, 2000] experiments (see Plate 1 top). "Y
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