Investigating the dynamical models of cosmology with recent observations and upcoming gravitational-wave data

Jie Zheng; Yun Chen; Tengpeng Xu; Zong-Hong Zhu

doi:10.1140/epjp/s13360-022-02718-3

2023 Impact factor 2.8

EPJ PLUS - Condensed Matter and Complex Systems

Eur. Phys. J. Plus (2022) 137: 509
https://doi.org/10.1140/epjp/s13360-022-02718-3

Regular Article

Investigating the dynamical models of cosmology with recent observations and upcoming gravitational-wave data

Jie Zheng¹, Yun Chen²^,3^b, Tengpeng Xu²^,3 and Zong-Hong Zhu¹^,4^d

¹ Gravitational Wave and Cosmology Laboratory, Department of Astronomy, Beijing Normal University, 100875, Beijing, China
² Key Laboratory for Computational Astrophysics, National Astronomical Observatories, Chinese Academy of Sciences, 100101, Beijing, China
³ College of Astronomy and Space Sciences, University of Chinese Academy of Sciences, 100049, Beijing, China
⁴ School of Physics and Technology, Wuhan University, 430072, Wuhan, China

^b chenyun@bao.ac.cn
^d zhuzh@bnu.edu.cn

Received: 19 January 2022
Accepted: 12 April 2022
Published online: 25 April 2022

Abstract

We explore and compare the capabilities of the recent observations of standard cosmological probes and the future observations of gravitational-wave (GW) standard sirens on constraining cosmological parameters. It is carried out in the frameworks of two typical dynamical models of cosmology, i.e., the $ω_{0} ω_{a}$ $\omega _0\omega _a$ CDM model with $ω (z) = ω_{0} + ω_{a} * z / (1 + z)$ $\omega (z) = \omega _0 +\omega _a*z/(1+z)$ , and the $ξ$ $\xi$ -index model with $ρ_{X} \propto ρ_{m} a^{ξ}$ $\rho _X\propto \rho _ma^{\xi }$ , where $ω (z)$ $\omega (z)$ is the dark energy equation of state, and $ρ_{X}$ $\rho _X$ and $ρ_{m}$ $\rho _m$ are the energy densities of dark energy and matter, respectively. In the cosmological analysis, the employed data sets include the recent observations of the standard cosmological probes, i.e., Type Ia supernovae (SNe Ia), baryon acoustic oscillation (BAO) and cosmic microwave background (CMB), and also the mock GW standard siren sample with 1000 merging neutron star events anticipated from the third-generation detectors. In the scenarios of both $ω_{0} ω_{a}$ $\omega _0\omega _a$ CDM and $ξ$ $\xi$ -index models, it turns out that the mock GW sample can reduce the uncertainty of the Hubble constant $H_{0}$ $$H_0$$ by about 50% relative to that from the joint SNe+BAO+CMB sample; nevertheless, the SNe+BAO+CMB sample demonstrates better performance on limiting other parameters. Furthermore, the Bayesian evidence is applied to compare the dynamical models with the $Λ$ $\Lambda$ CDM model. The Bayesian evidences computed from the SNe+BAO+CMB sample reveal that the $Λ$ $\Lambda$ CDM model is the most supported one; moreover, the $ω_{0} ω_{a}$ $\omega _0\omega _a$ CDM model is more competitive than the $ξ$ $\xi$ -index model.