Image Details
Caption: Fig. 3.
(a, b) Histograms of the recovered ﹩C_{l}﹩ for ﹩l=200﹩, 350, and 475 are shown for ﹩\nu =2.5﹩ (top) and 2.1 (bottom). Smooth lines show the best‐fit Gaussians to the histogram data. (c) ﹩C( \theta ) ﹩ vs. θ for the SCDM model; the theoretical value is shown with a dotted line. The values for one realization are shown with solid (for ﹩\nu =2.1﹩) and dashed (﹩\nu =2.5﹩) lines. (d) ﹩C_{l}﹩ vs. l for the SCDM model. The solid line corresponds to the theoretical input value. The spectrum recovered with our method from simulated 90 GHz MAP maps is shown after band averaging with ﹩\Delta l=50﹩ with filled diamonds (﹩\nu =2.1﹩) and crosses (﹩\nu =2.5﹩). To enable a clearer display, the central values of multipoles are shifted by five to the left for ﹩\nu =2.1﹩ and to the right for ﹩\nu =2.1﹩. The error bars correspond to the dispersion of the Gaussian fits such as as shown in (a) and practically coincide with 68% confidence limits, which in turn are approximately half the 95% limits.
© 2001. The American Astronomical Society. All rights reserved. Printed in U.S.A.