@article{barrow_first_2017,
	title = {First light: exploring the spectra of high-redshift galaxies in the {Renaissance} {Simulations}},
	volume = {469},
	issn = {0035-8711},
	shorttitle = {First light},
	url = {http://adsabs.harvard.edu/abs/2017MNRAS.469.4863B},
	doi = {10.1093/mnras/stx1181},
	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 H II 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, 2D 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
haloes with a strong dependence on stellar mass, metallicity, gas mass
fraction, and formation history. Haloes with the lowest stellar mass
have the greatest variability in [O III]/Hβ, [O III], and C III],
while haloes with higher masses are seen to show consistency in their
spectra and [O III] equivalent widths between 1 and 10 Å. Viewing
angle accounted for threefold difference in flux due to the presence of
ionized gas channels in a halo. Furthermore, JWST colour plots show a
discernible relationship between redshift, colour, and mean stellar age.},
	urldate = {2020-03-26},
	journal = {Monthly Notices of the Royal Astronomical Society},
	author = {Barrow, Kirk S. S. and Wise, John H. and Norman, Michael L. and O'Shea, Brian W. and Xu, Hao},
	month = aug,
	year = {2017},
	keywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Instrumentation and Methods for Astrophysics, dark ages, first stars, methods: numerical, methods: observational, radiative transfer, reionization, techniques: photometric, techniques: spectroscopic},
	pages = {4863--4878},
}

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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, 2D 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 haloes with a strong dependence on stellar mass, metallicity, gas mass fraction, and formation history. Haloes with the lowest stellar mass have the greatest variability in [O III]/Hβ, [O III], and C III], while haloes with higher masses are seen to show consistency in their spectra and [O III] equivalent widths between 1 and 10 Å. Viewing angle accounted for threefold difference in flux due to the presence of ionized gas channels in a halo. Furthermore, JWST colour plots show a discernible relationship between redshift, colour, and mean stellar age.","urldate":"2020-03-26","journal":"Monthly Notices of the Royal Astronomical Society","author":[{"propositions":[],"lastnames":["Barrow"],"firstnames":["Kirk","S.","S."],"suffixes":[]},{"propositions":[],"lastnames":["Wise"],"firstnames":["John","H."],"suffixes":[]},{"propositions":[],"lastnames":["Norman"],"firstnames":["Michael","L."],"suffixes":[]},{"propositions":[],"lastnames":["O'Shea"],"firstnames":["Brian","W."],"suffixes":[]},{"propositions":[],"lastnames":["Xu"],"firstnames":["Hao"],"suffixes":[]}],"month":"August","year":"2017","keywords":"Astrophysics - Astrophysics of Galaxies, Astrophysics - Instrumentation and Methods for Astrophysics, dark ages, first stars, methods: numerical, methods: observational, radiative transfer, reionization, techniques: photometric, techniques: spectroscopic","pages":"4863–4878","bibtex":"@article{barrow_first_2017,\n\ttitle = {First light: exploring the spectra of high-redshift galaxies in the {Renaissance} {Simulations}},\n\tvolume = {469},\n\tissn = {0035-8711},\n\tshorttitle = {First light},\n\turl = {http://adsabs.harvard.edu/abs/2017MNRAS.469.4863B},\n\tdoi = {10.1093/mnras/stx1181},\n\tabstract = {We present synthetic observations for the first generations of galaxies \nin the Universe and make predictions for future deep field observations\nfor redshifts greater than 6. Due to the strong impact of nebular\nemission lines and the relatively compact scale of H II regions,\nhigh-resolution cosmological simulations and a robust suite of analysis\ntools are required to properly simulate spectra. We created a software\npipeline consisting of fsps, hyperion, cloudy and our own tools to\ngenerate synthetic IR observations from a fully three-dimensional\narrangement of gas, dust, and stars. Our prescription allows us to\ninclude emission lines for a complete chemical network and tackle the\neffect of dust extinction and scattering in the various lines of sight.\nWe provide spectra, 2D binned photon imagery for both HST and JWST IR\nfilters, luminosity relationships, and emission-line strengths for a\nlarge sample of high-redshift galaxies in the Renaissance Simulations.\nOur resulting synthetic spectra show high variability between galactic\nhaloes with a strong dependence on stellar mass, metallicity, gas mass\nfraction, and formation history. Haloes with the lowest stellar mass\nhave the greatest variability in [O III]/Hβ, [O III], and C III],\nwhile haloes with higher masses are seen to show consistency in their\nspectra and [O III] equivalent widths between 1 and 10 Å. Viewing\nangle accounted for threefold difference in flux due to the presence of\nionized gas channels in a halo. Furthermore, JWST colour plots show a\ndiscernible relationship between redshift, colour, and mean stellar age.},\n\turldate = {2020-03-26},\n\tjournal = {Monthly Notices of the Royal Astronomical Society},\n\tauthor = {Barrow, Kirk S. S. and Wise, John H. and Norman, Michael L. and O'Shea, Brian W. and Xu, Hao},\n\tmonth = aug,\n\tyear = {2017},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Instrumentation and Methods for Astrophysics, dark ages, first stars, methods: numerical, methods: observational, radiative transfer, reionization, techniques: photometric, techniques: spectroscopic},\n\tpages = {4863--4878},\n}\n\n","author_short":["Barrow, K. S. S.","Wise, J. H.","Norman, M. L.","O'Shea, B. 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