  Despite the fact that the progenitor of fast blue optical transients (FBOTs)
is still up for debate, FBOTs are sometimes suggested to originate from the
core-collapse of ultra-stripped stars and be powered by a spinning-down neutron
star. Following this consideration, it is expected that the late-time evolution
of the progenitor stars can leave important imprints in the circumstellar
material (CSM) of the FBOTs, due to the strong mass loss of the stars. The
interaction of the FBOT ejecta with the CSM can drive a long-lasting shock to
generate radio emission, which thus enables us to probe the CSM properties
through radio observation although such observations are still rare. Within the
framework of the magnetar-powered model, Liu et al.(2022) fitted the multi-band
optical light curves of 40 FBOTs and, hence, the statistical distributions of
the FBOT magnetar and ejecta parameters were obtained. Based on these FBOT
population results, we investigate the dependence of the radio emission on the
mass-loss rate of the progenitors and evaluate the detectability of radio
emission from FBOTs with current and future telescopes. It is found that the
distribution of the peak time and peak luminosity of the emission at 8.4 GHz
are primarily in the regions of $t_{\rm{peak},\nu}=10^{2.12\pm0.63}$ days and
$L_{\rm{peak},\nu}=10^{28.73\pm0.83}$ erg s$^{-1}$ Hz$^{-1}$, respectively. A
joint detection of the Zwicky Transient Facility and Very Large Array could
achieve success in about 8.7% FBOTs of $z\leq1$. Furthermore, if considering a
joint observation of the Chinese Space Station Telescope and Square Kilometer
Array, this fraction can be increased to about 23.9%.
