General Cosmography Model with Spatial Curvature

Abstract

The cosmographic approach is adopted to determine the spatial curvature (i.e., ${\Omega }_K$) combining the latest released cosmic chronometers data (CC), the Pantheon sample of type Ia supernovae observations, and the baryon acoustic oscillation measurements. We use the expanded transverse comoving distance $D_M(z)$ as a basic function for deriving $H(z)$ and the other cosmic distances. In this scenario, ${\Omega }_K$ can be constrained only by CC data. To overcome the convergence issues at high-redshift domains, two methods are applied: the Padé approximants and the Taylor series in terms of the new redshift $y=z/(1+z)$. Adopting the Bayesian evidence, we find that there is positive evidence for the Padé approximant up to order ($2,2$) and weak evidence for the Taylor series up to 3-rd order against $\Lambda \text{CDM}+{\Omega }_K$ model. The constraint results show that a closed universe is preferred by the present observations under all the approximants used in this study. And the tension level of the Hubble constant $H_0$ is less than $2\sigma$ significance between different approximants and the local distance ladder determination. For each assumed approximant, $H_0$ is anti-correlated with ${\Omega }_K$ and the sound horizon at the end of the radiation drag epoch, which indicates that the $H_0$ tension problem can be slightly relaxed by introducing ${\Omega }_K$ or any new physics which can reduce the sound horizon in the early universe.

13 pages, 4 figures, major revised, update data and conclusions

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