Origin of the voids in the galaxy distribution
The distribution of galaxies on scales larger than approx.10 h/sup -1/ Mpc seems to be characterized by large voids, (20--40) h/sup -1/ Mpc in diameter and of amplitude deltaapprox.-(0.7--0.8). It was previously argued that the mere existence of such voids poses a severe problem to all dissipationless clustering theories. Here we show that the voids may, in fact, be a natural outcome of a dissipationless clustering scenario if both adiabatic and isothermal density perturbations exist primordially. When the nonlinear evolution of spherical voids of this type is followed for adiabatic perturbations with an index n>-1, it is seen that they become surrounded by a shell of positive density contrast. Their structure is insensitive to ..cap omega../sub 0/ while their dynamics is quite sensitive to it. The maximum peculiar velocity (relative to Hubble flow) within the void is found to be: v/sub p//v/sub H/approx.(0.4--0.5) for ..cap omega../sub 0/ = 1.0, approx.(0.2--0.25) for ..cap omega../sub 0/ = 0.45, and < or approx. =0.09 for ..cap omega../sub 0/ = 0.1.
- Research Organization:
- Department of Physics and Astronomy, Tel Aviv University
- OSTI ID:
- 6236493
- Journal Information:
- Astrophys. J., Lett. Ed.; (United States), Vol. 262:2
- Country of Publication:
- United States
- Language:
- English
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