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The Wide Field Survey Telescope (WFST) is a dedicated time-domain multi-band($u$, $g$, $r$, $i$, and $z$) photometric survey facility under construction.In this paper, we present a preliminary study that assesses the quality ofphotometric redshifts based on WFST by utilizing mock observations derived withthe galaxy catalog in the COSMOS/UltraVISTA field. We apply the templatefitting technique to estimate photometric redshifts by using the ZEBRAphotometric-redshift code and adopting a modified set of adaptive templates. Weevaluate the bias (median relative offset between the output photometricredshifts and input redshifts), normalized median absolute deviation($\sigma_{\rm NMAD}$) and outlier fraction ($f_{\rm outlier}$) of photometricredshifts in two typical WFST observational cases, the single 30-secondexposure observations (hereafter shallow mode) and co-added 50-minute exposureobservations (hereafter deep mode). We find bias$\la0.006$, $\sigma_{\rmNMAD}\la0.03$, and $f_{\rm outlier}\la5\%$ in the shallow mode and bias$\approx0.005$, $\sigma_{\rm NMAD}\approx 0.06$, and $f_{\rm outlier}\approx17\%$--$27\%$ in the deep mode, respectively, under various lunar phases.Combining the WFST mock observational data with that from the upcoming CSST andEuclid surveys, we demonstrate that the $z_{\rm phot}$ results can besignificantly improved, with $f_{\rm outlier}\approx 1\%$ and $\sigma_{\rmNMAD}\approx 0.02$.

A preliminary study of photometric redshifts based on the Wide Field Survey Telescope