the best-fitting values, which is insufficient for providing complete information on the survival range of the wormholes for a given cosmological scenario. In addition, the wormholes may not come into being immediately when the EoS parameter $\omega_{eff}(z)<-1$ and the specific formation mechanism of wormholes still needs to be explored further.

 Constant redshift function
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Considering the simplest case $\Phi=C$, where $C$ is an arbitrary constant, we can obtain the shape function by replacing Eqs. (\[2\]) and (\[8\]) in Eq. (\[3\]): $$b(r)=r_0^{\frac{1}{\omega_{eff}}+1}r^{-\frac{1}{\omega_{eff}}}. \label{10}$$ It is not difficult to find that the flare-out conditions are well satisfied by numerical calculations. To be more precise, the shape function $b(r)<r$ when $r>r_0$ and evaluating at the throat $r_0$, we can obtain $$b'(r_0)=-\frac{1}{\omega_{eff}}. \label{11}$$ Subsequently, if taking the model parameter pair ($\Omega_{m0}$, $\Omega_{r_c}$) from the joint constraints of SNe Ia+OHD+Planck-2015+GW data sets in terms of the lower boundary of the $2\sigma$ confidence band (see Fig. \[f3\]), we can obtain $b'(r_0)=0.931099<1$ ($\omega_{eff}=-1.074$) at the present epoch. The solution is both traversable and asymptotically flat, because the redshift function $\Phi$ is finite everywhere and $b/r\rightarrow0$ when $r\rightarrow\infty$. Furthermore, it is constructive and necessary to depict the space–time structure of the traversable wormhole. As described in Ref. [@50], 