Observational constraints from SNe Ia and Gamma-Ray Bursts on a clumpy universe

TL;DR

This study tests the Dyer-Roeder model's ability to describe local inhomogeneities in the universe using supernovae and gamma-ray burst data, constraining matter density and clumpiness parameters.

Contribution

It provides observational constraints on the universe's clumpiness and matter density using SNe Ia and GRBs within the Dyer-Roeder framework, highlighting potential limitations of the model.

Findings

Clumpiness parameter indicates a inhomogeneous universe.

Results show no impact on dark energy amount.

Dyer-Roeder approximation may not fully capture clumpiness effects.

Abstract

The luminosity distance describing the effect of local inhomogeneities in the propagation of light proposed by Zeldovich-Kantowski-Dyer-Roeder (ZKDR) is tested with two probes for two distinct ranges of redshifts: supernovae Ia (SNe Ia) in 0.015 < z < 1.414 and gamma-ray bursts (GRBs) in 1.547 < z < 3.57. Our analysis is performed by a Markov Chain Monte Carlo (MCMC) code that allows us to constrain the matter density parameter \Omega_m as well as the smoothness parameter $\alpha$ that measures the inhomogeneous-homogeneous rate of the cosmic fluid in a flat \LambdaCDM model. The obtained best fits are (\Omega_m=0.285^{+0.019}_{-0.018}, \alpha= 0.856^{+0.106}_{-0.176}) from SNe Ia and (\Omega_m=0.259^{+0.028}_{-0.028}, \alpha=0.587^{+0.201}_{-0.202}) from GRBs, while from the joint analysis the best fits are (\Omega_m=0.284^{+0.021}_{-0.020}, \alpha= 0.685^{+0.164}_{-0.171}) with a \chi^2_{\rm red}=0.975. The value of the smoothness parameter $\alpha$ indicates a clumped universe however it does not have an impact on the amount of dark energy (cosmological constant) needed to fit observations. This result may be an indication that the Dyer-Roeder approximation does not describe in a precise form the effects of clumpiness in the expansion of the universe.