but should be smaller enough to not to be influenced by the intrinsic SED shape. After extensive testing of various measures used to fit a continuum level, we find the method outlined below to be the most effective to fit a continuum level for our sample.

By visual inspection and spectroscopic redshift of the galaxies in our sample, we mask out the [H$\alpha$]{} and [\[\]]{} emission line regions in the spectra. We further mask all known sky lines by selecting a region $\times 2$ the spectral resolution ($\pm5.5$Å) of MOSFIRE K band. We then use the `astropy` [@Astropy2013] sigma-clipping algorithm to mask out remaining strong features in the spectra. These spectra are then used to fit an inverse variance weighted constant level fit, which we consider as the continuum level of the galaxy. Three objects fail to give a positive continuum level using this method and for these we perform a $3\sigma$ clip with two iterations without masking nebular emission lines and sky lines. Using this method we are able to fit positive continuum levels to all galaxies in our sample. We further investigate the robustness of our measures continuum levels in Appendix \[sec:cont\_Halpha\_test\] using ZFOURGE photometric data and conclude 