Limits on the Primordial Fluctuation Spectrum - Void Sizes and Anisotropy of the Cosmic Microwave Background Radiation

Details Limits on the Primordial Fluctuation Spectrum - Void Sizes and Anisotropy of the Cosmic Microwave Background Radiation Limits on the Primordial Fluctuation Spectrum - Void Sizes and Anisotropy of the Cosmic Microwave Background Radiation

Dec 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993mnras.265..681p&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Vol. 265, NO. 3/DEC1, P. 681, 1993

Astronomy and Astrophysics

Astronomy

28

Scientific paper

We suggest the use of the typical appearance of voids on a scale of 5000 km s^-1^ in the galaxy distribution to estimate the power spectrum on this scale. We use a simple model for the gravitational formation of voids, and we compare the results with the matter fluctuations as constrained by the CMBR observations by COBE. We find that a power spectrum P(k) is proportional to k^n^ with n ~ 1.25 is compatible both with COBE and with the gravitational growth of large voids in an {OMEGA} = 1 universe. A Harrison-Zel'dovich spectrum, n = 1, normalized to produce the observed CMBR fluctuations, does not have enough power for gravitational growth of voids with a diameter of 5000 km s^-1^ in an {OMEGA} = 1 universe. Such a spectrum would be compatible if (i) void diameters were smaller (3500 km s^-1^), the voids were shallower or the voids were rare (we assume that the Universe is void-filled), (ii) {OMEGA} < 1 (i.e. the Universe is open), (iii) galaxies do not trace matter on very large scales, or (iv) the voids do not grow gravitationally.

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