are the SSFRs of the star-forming cluster galaxies from [@wag17] after correcting the mass difference. In Figure \[f5\], our values of the quiescent fraction are uniformly lower than those from [@wag17] and the SSFRs of star-forming cluster galaxies from this study are also lower than those from [@wag17] with a systematics of $\sim$ 0.3 or 0.4 dex. The discrepancy is likely due to the different ways of separating star-forming and quiescent populations. We adopt constant SSFRs, while [@wag17] used the strength of the 4000 $\rm{\AA}$ break $D_n$(4000) to divide the two populations.

![image](f6.eps)

[ccccccccccccc]{} 9.7 - 10.1 & 0.035$\pm$0.016 & -9.605$\pm$0.024 & & 0.082$\pm$0.033 & -9.634$\pm$0.046 & & — & — & & — & —\
10.1 - 10.5 & 0.048$\pm$0.021 & -9.796$\pm$0.028 & & 0.103$\pm$0.024 & -9.887$\pm$0.034 & & 0.033$\pm$0.005 & -9.551$\pm$0.009 & & 0.092$\pm$0.047 & -9.692$\pm$0.080\
10.5 - 10.9 & 0.068$\pm$0.017 & -9.972$\pm$0.024 & & -0.114$\pm$0.054 & -9.771$\pm$0.035 & & 0.014$\pm$0.021 & -9.668$\pm$0.037 & & 0.093$\pm$0.018 & -9.806$\pm$0.020\
$>$10.9 & 0.014$\pm$0.003 & -9.879$\pm$0.004 & & 0.068$\pm$0.067 & -9.915$\pm$0.039 & & 0.051$\pm$0.011 & -9.842$\pm$0.014 & & 0.015$\pm$0.033 & -9.858$\pm$0.012\

![image](f7.eps)

[ccccccccccccc]{} 10.1 - 10.5 & -0.098$\pm$0.013 & 0.720$\pm$0.017 & & -0.127$\pm$0.016 & 0.818$\pm$0.016 & & — & — & 