# First Light: exploring the Spectra of High-Redshift Galaxies in the Renaissance Simulations

## TL;DR

This paper develops a comprehensive simulation pipeline to generate synthetic spectra and images of high-redshift galaxies, aiding future observations with JWST and HST by analyzing spectral variability and galaxy properties.

## Contribution

It introduces a novel software pipeline combining multiple tools to produce detailed synthetic spectra and images of early galaxies, accounting for nebular emission, dust, and viewing angles.

## Key findings

- Spectral variability correlates with galaxy mass, metallicity, and formation history.
- Higher mass halos show consistent emission line strengths, while low mass halos vary significantly.
- Viewing angle can cause a three-fold flux difference due to ionized gas channels.

## Abstract

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.