This simply corresponds to a slight shift in the bin centre in Figure \[fig:passivefraction\]. Using these equations, we recalculate the quiescent fractions as a function of stellar mass (Figure \[fig:passivefraction\]). These fractions were calculated as in Section \[sec:UVJ\] for sources in \[4.5\] magnitude bins (corresponding to stellar mass).

There is also a strong correlation between galaxy mass and passivity, with a higher fraction of the massive sources being quiescent. Figure \[fig:passivefraction\] shows that this trend is steeper for the protocluster galaxies than for the field galaxies, and there is a divide at $M_* \sim 10^{10.5}$M$_{\odot}$. Only $20-30$% of galaxies with stellar masses $M_* < 10^{10.5}$M$_{\odot}$ are quiescent in both environments, whereas 80-100% of $M_* > 10^{10.5}$M$_{\odot}$ galaxies are quiescent in the protocluster, compared to only $\sim40$% in the field (Table \[table:passivefraction\]).

We find that the fraction of quiescent galaxies is dependent on environment: 7C contains double the quiescent fraction of the control field at $z\sim1.6$. However, this environmental effect is also mass dependent: only the population of high-mass galaxies has an enhanced quenched fraction relative to the control field. These results are consistent with recent literature on red galaxies in clusters at $z>1.5$. @Rudnick2012 and @Fassbender2014 found a strong excess 