for the median SSFR of star-forming galaxies caused by the method are -0.04 dex and 0.006 for high-mass galaxies and -0.02 dex and 0.003 for low-mass galaxies, which is much less lower than the errors from the jackknife resampling. Additionally, the bias for the quiescent fraction can be as large as -8$\%$ (-0.07) for high-mass galaxies and -4$\%$ (-0.02) for low-mass galaxies, and the corresponding scatter is an order of magnitude smaller than the bias, $\sim$2-3 $\times$10$^{-3}$. The introduced bias and scatter appear to be significantly smaller than the errors from the jackknife resampling. We thus neglect to include the uncertainties in the error bars.

Group/Cluster Sample
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The group/cluster sample is constructed using the group identification method called the probability friend-of-friend group finder [PFOF; @liu08; @jian14]. On the basis of the conventional FOF method [@huc82], PFOF additionally takes into account the probability distribution function of the photometric redshifts of each galaxy and computes the linking probability of a given pair of galaxies to quantify their association in the line-of-sight direction. Given a linking probability threshold along with the linking lengths, PFOF then identifies groups and clusters. With a training set containing known spectroscopically identified groups and clusters in the 