\begin{document}$H(z)$\end{document} as an additional constraint on the first-order derivative can partially reduce the uncertainty; however, it is still not sufficiently precise to distinguish between the evolving and the constant dark energy. Moreover, the results heavily rely on the prior of the Hubble constant \begin{document}$H_0$\end{document}. The \begin{document}$H_0$\end{document} value inferred from SNe+\begin{document}$H(z)$\end{document} without prior is \begin{document}$H_0=70.5\pm 0.5~{\rm km~s^{-1}~Mpc^{-1}}$\end{document}. Moreover, the matter density \begin{document}$\Omega_M$\end{document} has a non-negligible effect on the reconstruction of dark energy. Therefore, more accurate determinations on \begin{document}$H_0$\end{document} and \begin{document}$\Omega_M$\end{document} are required to tightly constrain the EoS of dark energy."> Non-parametric reconstruction of dark energy and cosmic expansion from the Pantheon compilation of type Ia supernovae -
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