English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

The distance scale to cosmic gamma-ray bursts (GRBs) is still uncertain by many orders of magnitude; however, one viable scenario places GRBs at cosmological distances, thereby permitting them to be used as tracers of the cosmological expansion over a significant range of redshifts z. Also, several recent measurements of the Hubble constant H0 appearing in the referred literature report values of 70H − 80 km s−1 Mpc−1. Although there is significant debate regarding these measurements, we proceed here under the assumption that they are evidence of a large value for H0. This is done in order to investigate the additional constraints on cosmological models that can be obtained under this hypothesis when combined with the age of the universe and the brightness distribution of cosmological gamma-ray bursts. We show that the range of cosmological models that can be consistent with the GRB brightness distribution, a Hubble constant of 70 − 80 km s−1 >Mpc−1, and a minimum age of the universe of 13–15 Gyr is constrained significantly, largely independent of a wide range of assumptions regarding the evolutionary nature of the burst population. Low-density, Λ q0 < 0 and density parameter σ0 in the range ≈ 0.10 − 0.25 (Ω0 ≈ 0.2 − 0.5) are strongly favored.

The Compatibility of Friedmann Cosmological Models with Observed Properties of Gamma‐Ray Bursts and a Large Hubble Constant