Cosmological radiative transfer codes comparison project – I. The static density field tests

  title={Cosmological radiative transfer codes comparison project – I. The static density field tests},
  author={Ilian T. Iliev and Benedetta Ciardi and Marcelo A. Alvarez and Antonella Maselli and Andrea Ferrara and Nickolay Y. Gnedin and Garrelt Mellema and Taishi Nakamoto and Michael L. Norman and Alexei O. Razoumov and Erik-Jan Rijkhorst and Jelle Ritzerveld and Paul R. Shapiro and Hajime Susa and Masayuki Umemura and Daniel J. Whalen Cita and M.Pi and UTexas and Sissa and Fermilab and UChicago and Astron. and Leiden Obs. and UTsukuba and U. C. San Diego and Oak Ridge Natl. Lab. and Rikkyo U. Lanl},
  journal={Monthly Notices of the Royal Astronomical Society},
Radiative transfer (RT) simulations are now at the forefront of numerical astrophysics. They are becoming crucial for an increasing number of astrophysical and cosmological problems; at the same time their computational cost has come within reach of currently available computational power. Further progress is retarded by the considerable number of different algorithms (including various flavours of ray tracing and moment schemes) developed, which makes the selection of the most suitable… 

Cosmological radiative transfer comparison project – II. The radiation-hydrodynamic tests

The development of radiation hydrodynamical methods that are able to follow gas dynamics and radiative transfer (RT) self-consistently is key to the solution of many problems in numerical


The recent implementation of radiative transfer algorithms in numerous hydrodynamics codes has led to a dramatic improvement in studies of feedback in various astrophysical environments. However,

A new moment method for continuum radiative transfer in cosmological re‐ionization

We introduce a new code for computing time-dependent continuum radiative transfer and non-equilibrium ionization states in static density fields with periodic boundaries. Our code solves the moments

Cosmological RHD simulations of early galaxy formation

With the increasing sophistication and efficiency of cosmological hydrodynamics codes, ithas become viable to include ionizing radiative transfer (RT) in cosmological simulations,either in

Multifrequency, thermally coupled radiative transfer with TRAPHIC: method and tests

We present an extension of traphic, the method for radiative transfer of ionizing radiation in smoothed particle hydrodynamics simulations that we introduced in Pawlik & Schaye. The new version keeps


We describe an extension of the Enzo code to enable fully coupled radiation hydrodynamical simulation of inhomogeneous reionization in large ∼(100 Mpc)3 cosmological volumes with thousands to

crash3: cosmological radiative transfer through metals

Here we introduce CRASH3, the latest release of the 3D radiative transfer code CRASH. In its current implementation CRASH3 integrates into the reference algorithm the code Cloudy to evaluate the

Efficient Simulations of Early Structure Formation and Reionization

Detailed theoretical studies of the high-redshift universe, and especially reionization, are generally forced to rely on time-consuming N-body codes and/or radiative transfer algorithms. We present a

EMMA: an adaptive mesh refinement cosmological simulation code with radiative transfer

EMMA is a cosmological simulation code aimed at investigating the reionization epoch. It handles simultaneously collisionless and gas dynamics, as well as radiative transfer physics using a

ramses-rt: radiation hydrodynamics in the cosmological context

We present a new implementation of radiation hydrodynamics (RHD) in the adaptive mesh refinement (AMR) code RAMSES. The multi-group radiative transfer (RT) is performed on the AMR grid with a



CRASH: A radiative transfer scheme

We present a largely improved version of crash, a 3D radiative transfer code that treats the effects of ionizing radiation propagating through a given inhomogeneous H/He cosmological density field on

Cosmological reionization around the first stars: Monte Carlo radiative transfer

We study the evolution of ionization fronts around the first protogalaxies by using high-resolution numerical cosmological (Λ+ cold dark matter, CDM, model) simulations and Monte Carlo radiative

Simulating Cosmic Reionization at Large Scales I: the Geometry of Reionization

We present the first large-scale radiative transfer simulat ions of cosmic reionization, in a simulation volume of (100 h 1 Mpc) 3 . This is more than a 2 orders of magnitude improvement over

Cosmological Hydrogen Reionization with Three-dimensional Radiative Transfer

We present new calculations of the inhomogeneous process of cosmological reionization by carefully following the radiative transfer in precomputed hydrodynamic simulations of galaxy formation. These

The Cosmological simulation code GADGET-2

We discuss the cosmological simulation code GADGET-2, a new massively parallel TreeSPH code, capable of following a collisionless fluid with the N-body method, and an ideal gas by means of smoothed

Smoothed Particle Hydrodynamics Coupled with Radiation Transfer

  • H. Susa
  • Physics, Computer Science
  • 2006
A brand-new radiation hydrodynamics solver based upon Smoothed Particle Hydrodynamicics (SPH), which works on parallel computer system, is constructed, designed to investigate the formation and evolution of the first generation objects at z, where the radiative feedback from various sources play important roles.

The H II Region of the First Star

Simulations predict that the first stars in a ΛCDM universe formed at redshifts z > 20 in minihalos with masses of about 106 M☉. We have studied their radiative feedback by simulating the propagation

A Multistep Algorithm for the Radiation Hydrodynamical Transport of Cosmological Ionization Fronts and Ionized Flows

Radiation hydrodynamical transport of ionization fronts (I-fronts) in the next generation of cosmological reionization simulations holds the promise of predicting UV escape fractions from first