Limits on the Primordial Fluctuation Spectrum Void Sizes and CMBR Anisotropy

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dc.creatorPiran, T.
dc.creatorLecar, M.
dc.creatorGoldwirth, D. S.
dc.creatorda Costa, L. Nicolaci
dc.creatorBlumenthal, G. R.
dc.date1993-05-14
dc.date1993-05-17
dc.date.accessioned2026-07-07T08:58:12Z
dc.date.available2026-07-07T08:58:12Z
dc.descriptionWe suggest to use the common appearance of voids with a scale of $5000 \kms$ in the galaxy distribution to estimate the power spectrum on this scale. We use a simple model for a gravitational formation of voids and we compare the results with the matter fluctuations as constrained by the CMBR observations of COBE. We find that a power spectrum $P(k)\propto k^n$ with $n \approx 1.25$ is compatible both with COBE and with gravitational growth of large voids in an $Ω=1$ 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 $5000 \kms$ in an $Ω=1$ Universe. Such a spectrum would be compatible if (i) void diameters are smaller ($3500 \kms$), the voids are shallower or if the voids are rare (we assume that the universe is void filled); (ii) $Ω< 1$ i.e. the Universe is open; (iii) galaxies do not trace matter on very large scale or if (iv) the voids do not grow gravitationally.
dc.description23 pages, tex, 1 figure can be obtaine from tsvi@cfata4.harvard.edu CFA-3640
dc.identifierhttps://arxiv.org/abs/astro-ph/9305019
dc.identifierhttp://arxiv.org/abs/astro-ph/9305019
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/147229
dc.subjectAstrophysics
dc.titleLimits on the Primordial Fluctuation Spectrum Void Sizes and CMBR Anisotropy
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