Utility of observational Hubble parameter data on dark energy evolution

Abstract

Aiming at exploring the nature of dark energy, we use thirty-six observational Hubble parameter data (OHD) in the redshift range $0⩽z⩽2.36$ to make a cosmological model-independent test of the two-point $Om{h}^2(z_2;z_1)$ diagnostic. In $\Lambda$CDM, we have $Om{h}^2\equiv {\Omega }_m{h}^2$, where ${\Omega }_m$ is the matter density parameter at present. We bin all the OHD into four data points to mitigate the observational contaminations. By comparing with the value of ${\Omega }_m{h}^2$ which is constrained tightly by the Planck observations, our results show that in all six testing pairs of $Om{h}^2$ there are two testing pairs are consistent with $\Lambda$CDM at $1\sigma$ confidence level (CL), whereas for another two of them $\Lambda$CDM can only be accommodated at $2\sigma$ CL. Particularly, for remaining two pairs, $\Lambda$CDM is not compatible even at $2\sigma$ CL. Therefore it is reasonable that although deviations from $\Lambda$CDM exist for some pairs, cautiously, we cannot rule out the validity of $\Lambda$CDM. We further apply two methods to derive the value of Hubble constant $H_0$ utilizing the two-point $Om{h}^2(z_2;z_1)$ diagnostic. We obtain $H_0=71.23\pm 1.54$ $\mathrm{km}{\mathrm{s}}^{-1}\mathrm{Mp}{\mathrm{c}}^{-1}$ from inverse variance weighted $Om{h}^2$ value (method (I)) and $H_0=69.37\pm 1.59$ $\mathrm{km}{\mathrm{s}}^{-1}\mathrm{Mp}{\mathrm{c}}^{-1}$ that the $Om{h}^2$ value originates from Planck measurement (method (II)), both at $1\sigma$ CL. Finally, we explore how the error in OHD propagate into $w(z)$ at certain redshift during the reconstruction of $w(z)$. We argue that the current precision on OHD is not sufficient small to ensure the reconstruction of $w(z)$ in an acceptable error range, especially at the low redshift

8 pages, 6 figures

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