  We present synthetic observations for the first generations of galaxies in
the Universe and make predictions for future deep field observations for
redshifts greater than 6. Due to the strong impact of nebular emission lines
and the relatively compact scale of HII regions, high resolution cosmological
simulations and a robust suite of analysis tools are required to properly
simulate spectra. We created a software pipeline consisting of FSPS, Hyperion,
Cloudy and our own tools to generate synthetic IR observations from a fully
three-dimensional arrangement of gas, dust, and stars. Our prescription allows
us to include emission lines for a complete chemical network and tackle the
effect of dust extinction and scattering in the various lines of sight. We
provide spectra, 2-D binned photon imagery for both HST and JWST IR filters,
luminosity relationships, and emission line strengths for a large sample of
high redshift galaxies in the Renaissance Simulations. Our resulting synthetic
spectra show high variability between galactic halos with a strong dependence
on stellar mass, metallicity, gas mass fraction, and formation history. Halos
with the lowest stellar mass have the greatest variability in [OIII]/H$\beta$,
[OIII] and CIII] while halos with higher masses are seen to show consistency in
their spectra and [OIII] equivalent widths (EW) between 1\AA\ and 10\AA.
Viewing angle accounted for three-fold difference in flux due to the presence
of ionized gas channels in a halo. Furthermore, JWST color plots show a
discernible relationship between redshift, color, and mean stellar age.
