1D spectra. We define extraction apertures using a representative profile of the flux monitor star and perform multiple extractions per slit depending on their spatial size. A total of 93 1D sky spectra are extracted and their continuum level is measured by masking out sky lines and performing a sigma-clipping algorithm. The error of the sky continuum fit is calculated by bootstrap re-sampling of the sky fluxes 1000 times. We consider the $1\sigma$ scatter of the bootstrapped continuum values to be the error of the sky continuum fit and $1\sigma$ scatter of the flux values used for the continuum fit as the RMS of the flux.

The comparison between the flux continuum level for the sky spectra with the [ZFIRE-SP sample]{} spectra are shown in Figure \[fig:noise\_levels\]. The median and the 2$\sigma$ standard deviation for the continuum levels of the sky spectra are $\mathrm{-2.3\times 10^{-21} ergs/s/cm^2/\AA}$ and $\mathrm{5.4 \times 10^{-20} ergs/s/cm^2/\AA}$ respectively. We consider the horizontal blue dashed line in the Figure \[fig:noise\_levels\], which is $2\sigma$ above the median sky level, to be our lower limit for the continuum detections in our sample. The [46]{} galaxies in our [ZFIRE-SP sample]{} with continuum levels above this flux level detections are considered 