Observational constraints on Hubble constant and deceleration parameter in power-law cosmology

Abstract

In this paper, we show that the expansion history of the Universe in power‐law cosmology essentially depends on two crucial parameters, namely the Hubble constant H0 and deceleration parameter q. We find the constraints on these parameters from the latest H(z) and SNe Ia data. At 1σ level the constraints from H(z) data are obtained as and km s−1 Mpc−1, while the constraints from the Type Ia supernovae (SNe Ia) data are and km s−1 Mpc−1. We also perform the joint test using H(z) and SNe Ia data, which yields the constraints and km s−1 Mpc−1. The estimates of H0 are found to be in close agreement with some recent probes carried out in the literature. The analysis reveals that the observational data successfully describe the cosmic acceleration within the framework of power‐law cosmology. We find that the power‐law cosmology accommodates well the H(z) and SNe Ia data. We also test the power‐law cosmology using the primordial nucleosynthesis, which yields the constraints q≳ 0.72 and H0≲ 41.49 km s−1 Mpc−1. These constraints are found to be inconsistent with the ones derived from the H(z) and SNe Ia data. We carry out the statefinder analysis, and find that the power‐law cosmological models approach the standard Λ cold dark matter (ΛCDM) model as q→−1. Finally, we conclude that despite having several good features power‐law cosmology is not a complete package for the cosmological purposes.

Power-law cosmology, SN Ia, and BAO

“…[14], the difference can be explained by the different data sets used, i.e. we are using more recent and extended data sets on SN Ia.…”

“…we are using more recent and extended data sets on SN Ia. Also, in the paper [14] a non-zero spatial curvature has not been considered. We sharply disagree with Ref.…”

Non-minimal derivative coupling gravity in cosmology

“…The power-law expansion has been considered widely in astrophysical observations, see e.g. [107][108][109][110] (see also [111] for constraints). It is realized as an attractor solution of a canonical scalar field evolving under exponential potential [112] and solution of a barotropic fluid-dominant universe.…”

Phenomenological models of Universe with varying G and Λ

“…and H 0 = 68 93 ± 0 53 Km sMpc [117]. Recent astronomical data based on a new infrared camera on the HST gave [118].…”

“…And as an a particular example we consider a potential V (φ) = −βφ of the form, where β is a constant. According to the 1σ level [117]. Also a joint test using H( ) and SN I gave −0 39 ≤ ≤ −0 29…”