K band is $\sim80\%$, which is extremely similar to the observed completeness. Therefore, non-detections rate is consistent with uncertainties in the photometric redshifts. To further account for any detection bias, we employ a stacking technique of the non-detected spectra in order to calculate a lower-limit to the stacked EW values. This is further discussed in Section \[sec:EW\_stacking\].

[ccccccccccc]{} $<9.5$ & 568 & 59 & 44 & 0 & 2 & 1 & 41 & 34 & 9 &\
$9.5-10.0$ & 318 & 47 & 39 & 0 & 1 & 0 & 35 & 16 & 6 &\
$10.0<$ & 273 & 54 & 45 & 0 & 20 & 1 & 26 & 6 & 5 &\
Total &1159 &160 & 128 & 0 & 23 & 2 &102 & 56 & 20 &\

Continuum fitting and [H$\alpha$]{} EW calculation {#sec:cont_fit}
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In this section, we describe our continuum fitting method for our 102 [H$\alpha$]{} detected galaxies selected from the ZFIRE survey. Fitting a robust continuum level to a spectrum requires nebular emission lines and sky line residuals to be masked. Furthermore, the wavelength interval used for the continuum fit should be sufficient enough to perform an effective fit 