The luminosity-redshift relation in brane-worlds: II. Confrontation with experimental data

Abstract

The luminosity distance -redshift relation for a wide class of generalized Randall-Sundrum type II brane-world models with Weyl fluid is compared to the presently available supernova data. We find that there is a class of spacially flat models with different amounts of matter Ω ρ and Weyl fluid Ω d , which have a very similar fitting quality. The best-fit models are equally likely and can be regarded as extensions of the ΛCDM model, which is also included. We examine three models with different evolutionary history of the Weyl fluid, characterized by a parameter α = 0, 2 and 3. The first model describes a brane which had radiated energy into the bulk some time ago, but in recent times this energy exchange has ceased and only a dark radiation (α = 0) is left. In the other two models the Weyl-fluid describes a radiating brane throughout the cosmological evolution, up to our days. We find that the throughout of the fitting surface extends over a wider Ω d -range with increasing α, but the linear correlation of Ω d and Ω ρ holds all over the examined Ω d range.

The luminosity-redshift relation in brane-worlds: I. Analytical results

“…While the focus of the present paper is the integrability of the luminosity distance -redshift relation in various brane-world models, in a forthcoming paper [62] we will discuss how well the presently available supernova data support the brane-world models with a small amount of Weyl fluid. …”

Cosmological constraints on parameters of one-brane models with extra dimension

“…The normalized age of the Universe t 0 H 0 is obtained of order unity, if Let us compare the estimates of the present paper in which were used parameters of the standard cosmological model with those with parameters obtained in these fits. Identifying the corresponding terms in the Friedmann equation in the form employed in the present paper H 2 = σ 2 − µ 2 + 2σρ + ρ 2 + Cz 4 with those in [37,38,39] , we obtain the relations…”

“…Some examples of the best fits of parametersΩ are presented in the Table. ref.Ω ρΩΛΩdΩλ −q 0 derived [39] prior(0.15, 0. 35) prior(-0.03,0.07) 0.225 0.735 0.04 0 0.58 [40] prior (-0.1, 0.1) 0.15 0.80 0.008 0.026 0.67 [40] prior (0.2, 0.4) prior(-0.1, 0.1) 0.29 0.78 -0.09 0.02 0.68 [37] prior 0 0.25 0.73 0 0.02 0.57…”

Constraints on Parameters of Models With Extra Dimension From Primordial Nucleosynthesis

“…Generally, numerical values of cosmological parameters depend on a model in which the experimental data were processed. Recently fits of parameters were made in RSII-like models with positive tension of the brane [21,22,23,24]. The main cosmological parameters obtained in these fits do not considerably differ from those of the standard model used in the present note.…”