in 7C are quiescent, with a quiescent fraction ($f_Q$) for sources with $J \le 23.6$ of $f_Q = 0.50 \pm 0.09$ (see Table \[table:passivefraction\]). Of the “red" galaxies, $80\pm 6$% are quiescent, so the vast majority of these objects are not dust-obscured star forming galaxies, but are already quenched and evolving passively.

ClG0218.3$-$0510 contains fewer passively evolving galaxies ($f_Q=0.30\pm0.08$), with $67\pm11$% of the red galaxies classified as quiescent. These fractions were calculated using the same criteria as in Section \[sec:method\] and within a 0.9arcmin aperture of the cluster core. 7C has a similar fraction of red, quiescent galaxies at a 1$\sigma$ level.

Both of these protoclusters contain a significantly higher quiescent fraction than the average field, which is $f_Q=0.16\pm0.01$. This means that the star formation rates of many cluster members are greatly suppressed relative to the field.

![[*[Top]{}*]{}: Histogram showing the number of excess sources within 0.9arcmin of C compared to the expected numbers in a random blank field, as a function of $J$ band magnitude. [*[Middle]{}*]{}: Colour-magnitude diagram showing a clear structure of red sources at $i'-J \sim 2.5$. The RLAGN is marked with a red star. All sources within 0.9arcmin of the RLAGN are marked with red squares. 