near $\sim$ 0.1 $M_{\odot }$ stars ten trillion years from now. [@2019MNRAS.485.5924L] study photosynthesis on habitable planets around low-mass stars to examine if this kind of planet can receive enough photons in the waveband of an active range of 400-750 nm to sustain Earth-like biospheres.

Radio SETI [@1959Natur.184..844C] is an important technique because Earth’s atmosphere is relatively transparent at many radio wavelengths, and radio emissions have low extinction through the interstellar medium (ISM). Many radio SETI experiments have been conducted at Green Bank, Arecibo, Parkes, Meerkat, and several other single dish and array telescopes. Some recent examples are @2013ApJ...767...94S, @2013ApJ...767...94S, @2018PASP..130d4502M, @2018PASA...35...41P, @Chennamangalam_2017, and @2017ApJ...849..104E. The first experiment for SETI with the Murchison Widefield Array (MWA), one of four Precursors for Square Kilometre Array (SKA) telescope, has an extremely large field of view [@2016ApJ...827L..22T]. The VLA SETI experiment by [@2017AJ....153..110G] implemented the search for artificial radio signals from nearby galaxies M31 (Andromeda) and M33 (Triangulum).

FAST, Earth’s largest single-aperture telescope [@2000ASPC..213..523N; @doi:10.1142/S0218271811019335], has unique advantages for SETI observations. FAST can observe declinations from $-14.3^{o}<\delta <+65.7^{o}$ (versus $+1.5^{o}<\delta < +38.5^{o}$ at Arecibo) due to its geographical location and active surface. FAST’s sensitivity is $\sim 1800\ {\mathrm m^2/K}$ (Arecibo is about $1100$ 