AMBER: A Semi-numerical Abundance Matching Box for the Epoch of Reionization

Abstract

The Abundance Matching Box for the Epoch of Reionization (AMBER) is a semi-numerical code for modeling the cosmic dawn. The new algorithm is not based on the excursion set formalism for reionization, but takes the novel approach of calculating the reionization-redshift field $z_{\mathrm{re}}(\mathbf{x})$ assuming that hydrogen gas encountering higher radiation intensity are photoionized earlier. Redshift values are assigned while matching the abundance of ionized mass according to a given mass-weighted ionization fraction ${\bar{x}}_{\mathrm{i}}(z)$. The code has the unique advantage of allowing users to directly specify the reionization history through the redshift midpoint $z_{\mathrm{mid}}$, duration ${\Delta }_{\mathrm{z}}$, and asymmetry $A_{\mathrm{z}}$ input parameters. The reionization process is further controlled through the minimum halo mass $M_{\min }$ for galaxy formation and the radiation mean free path $l_{\mathrm{mfp}}$ for radiative transfer. We implement improved methods for constructing density, velocity, halo, and radiation fields, which are essential components for modeling reionization observables. We compare AMBER with two other semi-numerical methods and find that our code more accurately reproduces the results from radiation-hydrodynamic simulations. The parallelized code is over four orders of magnitude faster than radiative transfer simulations and will efficiently enable large-volume models, full-sky mock observations, and parameter-space studies. AMBER will be made publicly available to facilitate and transform studies of the EoR.

AMBER is publicly available at https://github.com/hytrac/amber

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• Retrieving cosmological information from small-scale CMB foregrounds II. The kinetic Sunyaev Zel'dovich effect
• First Constraints on the Epoch of Reionization Using the non-Gaussianity of the Kinematic Sunyaev-Zel{'}dovich Effect from the South Pole Telescope and {\it Herschel}-SPIRE Observations
• Improved treatments of the ionizing photon mean free path in semi-numerical simulations of reionization
• The Morphology of Reionization in a Dynamically Clumpy Universe
• An Effective Bias Expansion for 21 cm Cosmology in Redshift Space
• Patchy Kinetic Sunyaev-Zel'dovich Effect with Controlled Reionization History and Morphology
• Optical depth to reionization from perturbative 21cm clustering
• A multi-tracer empirically-driven approach to line-intensity mapping lightcones
• The Ultramarine Simulation: properties of dark matter haloes before redshift 5.5
• Efficient simulation of discrete galaxy populations and associated radiation fields during the first billion years
• The Atacama Cosmology Telescope: DR6 Power Spectrum Foreground Model and Validation
• A framework to mitigate patchy reionization contamination on the primordial gravitational wave signal
• Topology of Reionisation times: concepts, measurements and comparisons to gaussian random field predictions
• Reionisation time fields reconstruction from 21 cm signal maps
• Efficient Modelling of Lyman-α opacity fluctuations during late reionization epoch
• Cross-correlating the patchy screening and kinetic Sunyaev-Zel'dovich effects as a new probe of reionization
• Measuring the IGM correlation length at 5<z<6.1: a fast change at the end of Reionization
• Studying dark gaps in Ly-$\alpha$ forest transmission with large reionization simulations
• Forward-modelling the Luminosity, Distance, and Size distributions of the Milky Way Satellites
• A first look at the topology of reionization redshifts in models of the Epoch of the Reionization
• Exploring the Model Dependence of MCMC-Based 21 cm Power Spectrum Parameter Constraints