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N-Body Simulations and the Value of ω

Published online by Cambridge University Press:  14 August 2015

J. Richard Gott III
J. Richard Gott III*
Affiliation:
Princeton University Observatory

Extract

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We have recently completed a series of N-body simulations of galaxy clustering in an expanding universe (Aarseth, Gott and Turner 1977). the initial conditions and our results concerning galaxy clustering will be summarized by Sverre Aarseth at this meeting. in this paper I would like to tell about the implications of these models for the value of Ω = 8πGρO/3HO2 (where ρO is the present mean density of the universe and HO = 50 km s−1 Mpc−1 is Hubble's constant). in the standard Friedmann models with Λ = 0, Ω > 1 implies that the universe will eventually recollapse while Ω < 1 implies the expansion will continue forever. As discussed in Gott, Gunn, Schramm, and Tinsley (1974), there are a number of theoretical arguments to suggest that even the unseen matter in the universe is clustered the way the galaxies are so that virial mass determinations from groups and clusters and statistical virial theorem methods can provide good estimates of the mean mass density in the universe. We can utilize our N-body simulations to check the accuracy of these techniques.

Type
I. Galaxies in Small Groups
Information
Symposium - International Astronomical Union , Volume 79: The Large Scale Structure of the Universe , 1978 , pp. 63 - 70
Copyright
Copyright © Reidel 1978 

References

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