in the spectra, and two galaxies due to extreme sky line interference.

Our sample constitutes of the remaining 102 galaxies out of which, 46 have continuum detections (see Section \[sec:cont\_fit\]). Furthermore, 38 (out of which, 16 are continuum detected) galaxies are confirmed cluster members [@Yuan2014] and the remaining 64 (out of which, 30 are continuum detected) galaxies comprise of field galaxies. 32 galaxies targeted with photometric redshifts between $1.90<z<2.66$ show no [H$\alpha$]{} emission detection. We divide our sample into 3 mass bins with masses between $\log_{10}(\mathrm{M}_\odot)<9.5$, $\mathrm{9.5\leq log_{10}(M_\odot)\leq 10.0}$, $\mathrm{10.0<log_{10}(M_\odot)}$ and show the corresponding data as described above in Table \[tab:sample\_details\].

We define observing completeness as the percentage of detected galaxies (Q$_z>1$) with photometric redshifts between $1.90<z<2.66$ and calculate it to be $\sim80\%$. However, it is possible that the 32 null detections with photometric redshifts within $1.90<z<2.66$ to have been detected if the ZFIRE survey was more sensitive. We stack the the photometric redshift likelihood functions ($P(z)$) of the ZFIRE targeted galaxies within this redshift range, to compute the expectation of detections based of photometric redshift accuracies (See @Nanayakkara2016 Section 3.2 to further details on how $P(z)$ stacking is performed) . The calculated expectation for [H$\alpha$]{} to be detected within 