Figure. 5. Sampled (108 histories) energy spectra S[ω] as in Figure 1b for A) a Gaussian distribution (galaxies transparent), B) a Planck distribution (galaxies opaque, exponentially accelerated expansion), and C) a Planck-type distribution with distorted tail (galaxies opaque, but no accelerated expansion)

From

Is CMB just an Observational Effect of a Universe in Accelerated Expansion?

Arne Bergstrom

International Journal of Physics. 2013, 1(6), 133-137 doi:10.12691/ijp-1-6-1