selected by the criteria outlined in Section \[sec:5\], and our data processing pipeline is working well on the preliminary data collected from FAST. Hopefully, we expect that these ETI signal candidates could come from some warm Earth-size planets in the Milky Way, the number of which can be roughly predicted by Drake equation[@1961PhT....14d..40D; @2010LPICo1538.5211D; @2018PASP..130e4101G].

With the SETI capabilities demonstrated in this work, one can estimate the Equivalent Isotropic Radiated Power (EIRP)[@2017ApJ...849..104E] required of an alien transmitter to be detected by FAST. For a source of ETI signal candidates at at $d_{*}=$50 pc, a $\delta\nu=$ 4 Hz bandwidth, and a $t_{obs}=$ 0.25 second integration, the EIRP limit of FAST is $3.53\times 10^{13}$ W, given by:

$$EIRP = 4\pi d{_{*}}^{2}\sigma _{thresh}SEFD\sqrt{\frac{\delta \nu }{n_{pol}t_{obs}}},$$

where the system equivalent flux density $SEFD = 2k_{B}T_{sys}/A_{eff}$ and $\sigma _{thresh}$=S/N$_{min}$ is a signal-to-noise threshold value.

We are planning to take data on FAST’s commensal drift-scan surveys, such as the multiyear CRAFTS survey; we also intend to observe targets from the Transiting Exoplanet Survey Satellite(TESS), as well as selected stars within $d_{*}=$50 pc from the sun, for example: [@Isaacson_2017].

We are planning several improvements to the multi-year CRAFTS multi-beam SETI sky survey on FAST:

To improve FAST’s 