DYNAMIC EFFECTS OF THE COSMOLOGICAL CONSTANT.
MON NOT R ASTRON SOC
128 - 136.
The possibility of measuring the density parameter OMEGA-0 and the cosmological constant lambda-0 = LAMBDA/(3H0(2)) using dynamical tests is explored in linear and non-linear theory. In linear theory we find that the rate of growth of the perturbations at the present epoch is approximated by f(z = 0) almost-equal-to-OMEGA-0(0.6) + 1/70 lambda-0(1 + 1/2 OMEGA-0). Therefore, dynamical tests such as infall around clusters and dipoles at the present epoch do not distinguish well between universes with and without a cosmological constant. At higher redshifts, the perturbations also depend mainly on the matter density at a particular epoch, f(z) almost-equal-to OMEGA-0.6(z), which has a strong dependence on lambda-0 at z almost-equal-to 0.5-2.0. Therefore, information on both parameters can be obtained by looking at clustering at different redshifts. In practice, however, the other observables also depend on the cosmology, and in some cases conspire to give a weak dependence on lambda-0. By using the non-linear spherical infall model for a family of Cold Dark Matter (CDM) power-spectra we also find that dynamics at z = 0 does not tell much about lambda-0. At higher redshifts there is unfortunately another conspiracy between conventional observables, which hides information about lambda-0. The final radius of a virialized cluster (relative to the turnaround radius) is approximated by R(f)/R(ta) almost-equal-to (1 - eta/2)/(2 - eta/2), where eta is the ratio of LAMBDA to the density at turn-around. Therefore a repulsive-LAMBDA gives a smaller final radius than a vanishing-LAMBDA.
|Title:||DYNAMIC EFFECTS OF THE COSMOLOGICAL CONSTANT|
|Keywords:||COLD DARK MATTER, LARGE-SCALE STRUCTURE, RICH CLUSTERS, BIG-BANG, GALAXIES, UNIVERSE, EVOLUTION, REDSHIFT, LAMBDA, MODELS|
|UCL classification:||UCL > School of BEAMS
UCL > School of BEAMS > Faculty of Maths and Physical Sciences
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