0.78 in 0.2 $< z <$ 0.7. The amplitudes from these two works are corrected for the difference in the IMF, i.e. 1.8 $M_{*,\textrm{C}}$ = $M_{*,\textrm{S}}$, where C and S denote the Chabrier and Salpeter IMF, respectively. Our best-fit parameters agree well with those from [@whi12] and [@noe07].

Moreover, in Figure \[f5\], the quiescent fraction (top) of cluster galaxies and SSFR (bottom) of star-forming cluster galaxies are displayed as a function of stellar mass and compared to those from [@wag17]. In the top panel, the purple pluses and blue stars are the quiescent fractions of cluster galaxies from this work in 0.2 $< z <$ 0.5 and 0.5 $< z <$ 0.8, respectively, while the green squares and yellow squares are those in the range of 0.15 $< z <$ 0.41 and 0.41 $< z <$ 0.80 from [@wag17]. The quiescent fractions in the two different redshift ranges from this work and from [@wag17] are both agree well. In the bottom panel, the purple pluses and blue crosses are the SSFRs of star-forming cluster (solid lines) and field (dashed lines) galaxies in the range of 0.2 $< z <$ 0.5 and 0.5 $< z <$ 0.8, respectively. The green squares 