Abstract
(submitted to MNRAS January 10, 2017)
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 (O'Shea et al. 2015). 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.
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