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What is the Cosmological Density Parameter ΩO?

  • Amos Yahil
Conference paper
Part of the Santa Cruz Summer Workshops in Astronomy and Astrophysics book series (SANTA CRUZ)

Abstract

It has been clear for more than a decade that the deceleration of the universe can not be determined from the magnitude-redshift relation for first-ranked elliptical galaxies, which suffer from strong evolution, dominating the cosmological effects. Attention has therefore shifted to alternate methods which relate peculiar velocities to the density inhomogeneities which have given rise to them. These fall under three categories:
  • The study of well defined structures, primarily the local Virgo supercluster (VSC) of galaxies and its surrounding.

  • The use of a statistical relation between the positional correlation functions of galaxies and their velocity dispersion, known as the “cosmic virial theorem” (CVT).

  • Direct comparison between the observed density and velocity distributions of galaxies and N-body simulations, in which Ωo is an input parameter.

Keywords

Local Group Peculiar Velocity Open Universe Dipole Anisotropy Tidal Field 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

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Copyright information

© Springer-Verlag New York Inc. 1987

Authors and Affiliations

  • Amos Yahil

There are no affiliations available

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