Confirmation of the Friedmann‐Lemaǐtre universe by the distribution of the larger absorbing clouds

Abstract

A new theoretical approach is applied to the cloud model as an explanation for the Lyman a forest. It is based on the complete Friedmann equations including a A-term. In the data sets of Lu et al. 1991 and Roser 1993 the lines are constrained by a lower limit (0.36 A, 0.32 k ) of the intrinsic equivalent width. This makes them suitable for a cloud model analysis, supplementing the bubble wall models which also make use of the weaker lines. Both data sets can be represented satisfactorily by a Friedmann-Lernaitre model with XO = 1.08 f 0.02 and RO = 0.014 f 0.006, although the regression formulae differ by an essential factor depending on the redshift. The age of the universe according to this model is 2.8.H:'. It is not necessary to invoke any evolutionary effects in the number densities and in the physical parameters of the clouds.

Time-Varying Fine-Structure Constant Requires Cosmological Constant

“…This extremely small value of Ω 0 is compatible with other determinations of Ω 0 derived from examinations of the dynamics of clusters of galaxies if majority of their mass consists of a network of cosmic strings. This hypothetical network contributes to the local mass but do not influence the expansion of the universe 34 Interestingly, the cosmological parameters of the Bonn-Potsdam model 31,42,43 resemble those suggested above. Recently, van de Bruck 44,45 has examined the effects of the hypothetical cosmic string network on the cosmological velocity field within the framework of this model and has shown them to be compatible with cosmological observations.…”

Horizon problem in a closed universe dominated by fluid with negative pressure

“…problem is solved, are given inTable 1. The value W m0 0X015 in the table is justified by the paper of Hoell et al[25] in which it is argued that observations of absorption lines of the Lyman a forests of quasars would suggest that W m0 % 0X014 and W v0 % 1X08. Note that the value W v0 % 1X06 solving the horizon problem in our model is close to the value of Hoell et al Since the energy density parameters W r Y W m and W v are not constant in time and the horizon problem is solved only for the value of W…”

Incompatibility of a comoving Lyαforest with supernova-Ia luminosity distances

“…The basic idea underlying the Q-method is that the Ly-α-forest is caused by intersections of the quasar light with the boundaries of an inhomogeneous bubble structure of the (baryonic) matter (Hoell & Priester 1991a,b;Hoell et al 1994;Liebscher 1994;Liebscher et al 1992a,b). The differences ∆z between the redshifts z of two absorptionlines are observed to be small, so that they are taken as infinitesimal.…”

“…In the 1990's a tightly constrained world model including a Λ term (the so-called Bonn-Potsdam model; henceforth BP-model) was derived by fitting quasar absorption lines (Hoell & Priester 1991a,b;Hoell et al 1994;Liebscher 1994;Liebscher et al 1992a,b). The BP-model was based on the assumption that Lyα-forest quasar absorption lines situated between the Lyα and Lyβ emission lines reproduce the redshifts of comoving galaxy-populated shells (called "bubble walls" by the authors) in the universe.…”