EDGE Physics


Since the publication of the original EDGE suite in 2020, computational advancements have made it possible to improve the fidelity of the EDGE simulations. Consequently, the physics prescription of the second generation of EDGE simulations has undergone incremental improvements in various areas.

Changes between suites are shown below; however, for a comprehensive overview, we encourage the reader to read the relevant introductory paper.

EDGE-1 EDGE-2
Introduction Paper Agertz et al 2020 Rey et al 2025

Code Base		 Teyssier 2002

RAMSES		 Rosdahl et al 2013

RAMSES-RT

Cosmology		 Planck Collaboration et al 2014

LCDM		 Planck Collaboration et al 2020

LCDM
Resolution
(DM/Gas/Stellar)		 118M⊙/3pc/300M⊙ 944M⊙/3pc/300M⊙
Box Size 50 Mpc 100 Mpc
Halo Mass Range (M⊙) 1.2×109 - 7.5×109 1.2×109 - 1.1×1010
Stellar Mass Range (M⊙) 4.5×104 - 1.1×107 1.5×104 - 4.2×107
UVB Background A Modified version of
Haardt & Madau 1996
Faucher-Giguère 2020

Stellar Feedback		 CCSNe, SNe-Ia, fast winds from massive stars, and slow winds from AGB stars CCSNe, SNe-Ia, fast winds from massive stars, slow winds from AGB stars, and radiative feedback

Type-Ia Supernova Model		 Raiteri et al 1996
Yields from:
Thielemann et al 1986		 Maoz et al 2012
Yields from:
Seitenzahl et al 2013

Yields
Woosley & Heger 2007		 NUGrid Yields:
Pignatari et al 2016
Ritter et al 2018
Tracked Elements Fe, O C, N, O, Mg, Al, Si, Fe, Eu
Initial Mass Function Chabrier 2003 Kroupa 2001

Initial Conditions		 GenetIC

Stopyra et al 2021a		 GenetIC

Stopyra et al 2021a

Cooling		 Equilibrium cooling

Courty & Alimi 2004		 Non-equilibrium primordial and molecular chemistry
Rosdahl et al 2013
Nickerson et al 2018
GenetICally Modified
Initial Conditions		 Early/Late
Higher Final Mass
 Early/Late
Higher Final Mass
Fully Cosmological
Radiative Transfer As implemented in
Agertz et al 2020
High Cadence Tracer Particles Cadiou et al 2019
Population III Stars
The Science

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EDGE: A New Model for Nuclear Star Cluster Formation in Dwarf Galaxies

In this paper, we investigate the formation of simulated dwarf galaxies that play host Nulear Star Clsters, additionally we study their observational properties, and compare them to observed Globular Clusters such as Omega-Centuri.

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