approach described in [@mos12]. They parameterize the SFR with a combination of observed quantities, including rest-frame optical $B$ magnitudes $M_B$, observed \[O$_{\rm{II}}$\] luminosity, and/or rest-frame color. The parameterized SFR is then calibrated against the SED-fit SFR from UV/optical bands in the AEGIS survey in the redshift range of 0.7 $<$ $z$ $<$ 1.4. By incorporating a dimming factor of $Q$ = 1.3 magnitudes per unit redshift for the measured values $M_B$ to correct for dust extinction, Mostek and collaborators found that the derived $z$ $\sim$ 1 SFRs agree well with the local L\[O$_{\rm{II}}$\]$-$M$_B$ SFR calibration commonly used in the literature [@kew04]. Following the work in [@lin14], we use the fitting formula employing the rest-frame optical $M_B$, $(U-B)$, and a second order $(U-B)$ color as fit parameters. The fitting coefficients can be found in Table 3 in @mos12. [@mos12] reported that even though the \[O$_{\rm{II}}$\] flux of red galaxies may have contributions from AGN activity, this effect is much smaller for star-forming galaxies. Since our main purpose is to explore the star formation rate for the star-forming main sequence and the quiescent fraction in different environments, we do not rely on the SFR measurements for the quiescent galaxies at all, and 