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First‐Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Determination of Cosmological Parameters

  • Authors: D. N. Spergel, L. Verde, H. V. Peiris, E. Komatsu, M. R. Nolta, C. L. Bennett, M. Halpern, G. Hinshaw, N. Jarosik, A. Kogut, M. Limon, S. S. Meyer, L. Page, G. S. Tucker, J. L. Weiland, E. Wollack, and E. L. Wright

Spergel et al. 2003 The Astrophysical Journal Supplement Series 148 175.

  • Provider: AAS Journals

Caption: Fig. 9.

Left: The shaded region in the figure shows the 1 σ contours for the amplitude of the power spectrum as a function of scale for the running spectral index model fit to all data sets. The dotted lines bracket the 2 σ region for this model. The dashed line is the best‐fit power spectrum for the power‐law ΛCDM model. Right: The shaded region in the figure shows the 1 σ contours for the amplitude of the amplitude of mass fluctuations, ﹩\Delta ^{2}( k) =k^{3}P( k) / ( 2\pi ^{2}) ﹩, as a function of scale for the running spectral index model fit to all data sets. The dotted lines bracket the 2 σ region for this model. The dashed line is the best fit for the power‐law ΛCDM model.

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