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Power Spectra for Cold Dark Matter and Its Variants

  • Authors: Daniel J. Eisenstein and Wayne Hu

Eisenstein & Hu 1999 The Astrophysical Journal 511 5.

  • Provider: AAS Journals

Caption: Fig. 3.

(a–d) Ratio of fluctuations within 50 h−1 Mpc spheres to that within 8 h−1 Mpc spheres as a function of neutrino and baryon fractions for various cosmologies. The shaded region shows the preferred range of ﹩\sigma _{50}/ \sigma _{8}=0.151\pm 0.016﹩. (a) ﹩\Omega _{0}=1﹩, ﹩h=0.5﹩, ﹩n=1﹩, and ﹩N_{\nu }=1﹩. (b) As in (a), but with ﹩n=0.95﹩ and tensors as per power‐law inflation. (c) As in (a), but with two degenerate neutrino species (﹩N_{\nu }=2﹩). (d) ﹩\Omega _{0}=0.35﹩, ﹩\Omega _{\Lambda }=0.65﹩, ﹩h=0.7﹩, ﹩n=1﹩, and ﹩N_{\nu }=1﹩. All are COBE normalized. (e–h) Amplitude of fluctuations within 8 h−1 Mpc spheres for the cosmologies given in (a–d), respectively. The shaded region is the preferred range of ﹩\sigma _{8}=( 0.5\pm 0.15) \Omega ^{-0.65}_{0}﹩ (Pen 1998) and ﹩\sigma _{8}> 0.59﹩ (Fan et al. 1997).

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