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The Renaissance Simulations Vault

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The Renaissance Simulations Vault

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Published Works
Scaling Relations for Galaxies Prior to Reionization
Spatially Extended 21 cm Signal from Strongly Clustered Uv and X-Ray Sources in the Early Universe
Probing the Ultraviolet Luminosity Function of the Earliest Galaxies with the Renaissance Simulations
Late Pop III Star Formation During the Epoch of Reionization: Results from the Renaissance Simulations
X-Ray Background at High Redshifts from Pop III Remnants: Results from Pop III Star Formation Rates in the Renaissance Simulations
Population III Stars and Remnants in High Redshift Galaxies
Galaxy Properties and UV Escape Fractions during the Epoch of Reionization: Results from the Renaissance Simulations
Heating the Intergalactic Medium by X-Rays from Population III Binaries in High-redhsift Galaxies
First light: exploring the spectra of high-redshift galaxies in the Renaissance Simulations
First light – II. Emission line extinction, population III stars, and X-ray binaries
Fully Coupled Simulation of Cosmic Reionization. III. Stochastic Early Reionization by the Smallest Galaxies
The growth of black holes from Population III remnants in the Renaissance simulations
Simulating the Cosmic Dawn With Enzo
Formation of massive black holes in rapidly growing pre-galactic gas clouds
The emergence of the first star-free atomic cooling haloes in the Universe
Massive Star Formation in Metal-Enriched Haloes at High Redshift
Some First Stars Were Red: Detecting Signatures of Massive Population III Formation through Long-term Stochastic Color Variations
How long do high-redshift massive black hole seeds remain outliers in black hole vs. host galaxy relations?
No Tension: JWST Galaxies at z > 10 Consistent with Cosmological Simulations
Beyond the Goldilocks Zone: Identifying Critical Features in Massive Black Hole Formation
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Beyond No Tension: JWST z > 10 Galaxies Push Simulations to the Limit

Beyond the Goldilocks Zone: Identifying Critical Features in Massive Black Hole Formation

Mone, E., Pries, B., Wise, J.H., & Ferrans, S., 2025, ApJ, 982, 39.

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