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# Configurations for "fg21sim"
# -*- mode: conf -*-
#
# Syntax: `ConfigObj`, https://github.com/DiffSK/configobj
#
# This file contains the options corresponding the extragalactic emission
# components, which currently includes the following components:
# - clusters: halos
# - pointsources
[extragalactic]
# Press-Schechter formalism to determine the dark matter halos
# distribution with respect to masses and redshifts, from which
# to further determine the total number of halos within a sky
# patch and to sample the masses and redshifts for each halo.
# NOTE: only consider the *dark matter* mass within the halo!
[[psformalism]]
# The model of the fitting function for halo mass distribution
# For all models and more details:
# https://hmf.readthedocs.io/en/latest/_autosummary/hmf.fitting_functions.html
model = option("jenkins", "ps", "smt", default="smt")
# The minimum (inclusive) and maximum (exclusive) halo mass (dark
# matter only) within which to calculate the halo mass distribution.
# Unit: [Msun]
M_min = float(default=1e13, min=1e10, max=1e14)
M_max = float(default=1e16, min=1e14, max=1e18)
# The logarithmic (base 10) step size for the halo masses; therefore
# the number of intervals is: (log10(M_max) - log10(M_min)) / M_step
M_step = float(default=0.01, min=0.001, max=0.1)
# The minimum and maximum redshift within which to calculate the
# halo mass distribution; as well as the step size.
z_min = float(default=0.01, min=0.001, max=1.0)
z_max = float(default=4.0, min=1.0, max=100)
z_step = float(default=0.01, min=0.001, max=1.0)
# Output file (NumPy ".npz" format) to save the calculated halo mass
# distributions at every redshift.
#
# This file packs the following 3 NumPy arrays:
# * ``dndlnm``:
# Shape: (len(z), len(mass))
# Differential mass function in terms of natural log of M.
# Unit: [Mpc^-3] (the little "h" is folded into the values)
# * ``z``:
# Redshifts where the halo mass distribution is calculated.
# * ``mass``:
# (Logarithmic-distributed) masses points.
# Unit: [Msun] (the little "h" is folded into the values)
dndlnm_outfile = string(default=None)
# Extended emissions from the clusters of galaxies
# The configurations in this ``[[clusters]]`` section may also be
# used by the following ``[[halos]]`` section.
[[clusters]]
# Output CSV file of the clusters catalog containing the simulated
# mass, redshift, position, shape, and the recent major merger info.
catalog_outfile = string(default=None)
# Directly use the (previously simulated) catalog file specified
# as the above "catalog_outfile" option.
# NOTE:
# By using an existing catalog, the steps to derive these data are
# simply skipped.
# Due to the small number density of the galaxy clusters, the simulated
# results within a small patch of sky (e.g., 100 [deg^2]) show
# significant fluctuations (several or even several tens of times
# of differences between simulations). Therefore, one may run many
# tests and only create images at some frequencies necessary for
# testing, then select the satisfying one to continue the simulation
# to generate images at all frequencies.
use_output_catalog = boolean(default=False)
# Output CSV file of the halos catalog containing the calculated
# properties of the simulated halos.
halos_catalog_outfile = string(default=None)
# Whether to dump the whole data of the simulated halos in Python
# native pickle format (i.e., ".pkl") to a file with the same basename
# as the above ``halos_catalog_outfile``?
# The dumped data also includes the derived electron spectrum for
# each halo, therefore this file can be reloaded back in order to
# calculate the emissions at other frequencies.
dump_halos_data = boolean(default=True)
# Whether to directly use the (previously dumped) halos data (".pkl")
# as specified by the above ``halos_catalog_outfile`` and
# ``dump_halos_data`` options?
# In this way, the radio emissions at additional frequencies can be
# easily (and consistently) calculated.
use_dump_halos_data = boolean(default=False)
# The minimum mass for clusters when to determine the galaxy clusters
# total counts and their distributions.
# Unit: [Msun]
mass_min = float(default=2e14, min=1e12)
# Boost the number of expected cluster number within the sky coverage
# by the specified times.
# (NOTE: mainly for testing purpose.)
boost = float(default=1.0, min=0.1, max=1e4)
# Minimum mass change of the main cluster to be regarded as a merger
# event instead of an accretion event.
# Unit: [Msun]
merger_mass_min = float(default=1e12, min=1e10, max=1e14)
# Mass ratio of the main and sub clusters, below which is regarded as
# a major merger event.
ratio_major = float(default=3.0, min=1.0, max=10.0)
# The merger timescale, which roughly describes the duration of the
# merger-induced disturbance (~2-3 Gyr). This timescale is much longer
# the merger crossing time (~1 Gyr), and is also longer than the lifetime
# of radio halos.
# Unit: [Gyr]
tau_merger = float(default=2.0, min=1.0, max=5.0)
# Magnetic field scaling relation for clusters
# Reference: Cassano et al. 2012, A&A, 548, A100, Eq.(1)
#
# The mean magnetic field assumed
# Unit: [uG]
b_mean = float(default=1.9, min=0.1, max=10)
# The index of the scaling relation
b_index = float(default=1.5, min=0.0, max=3.0)
# Filename prefix for this component
prefix = string(default="cluster")
# Output directory to save the simulated results
output_dir = string(default=None)
# Giant radio halos for clusters with recent major mergers
[[halos]]
# Roughly the fraction of turbulence energy transformed to accelerate
# the electrons, describing the efficiency of turbulence acceleration.
eta_turb = float(default=0.2, min=0.1, max=1.0)
# Ratio of the total energy injected into cosmic-ray electrons during
# the cluster life to its total thermal energy.
eta_e = float(default=0.003, min=0.001, max=0.1)
# Minimum and maximum Lorentz factor (i.e., energy) of the relativistic
# electron spectrum.
gamma_min = float(default=1e1)
gamma_max = float(default=1e5)
# Number of momentum points/cells for solving the Fokker-Planck
# equation.
gamma_np = integer(default=200, min=50)
# Number of grid points used as the buffer region near the lower
# boundary, and the value within this buffer region will be fixed to
# avoid unphysical pile-up of low-energy electrons.
# Reference: Donnert & Brunetti 2014, MNRAS, 443, 3564, Sec.(3.3)
buffer_np = integer(default=5, min=0)
# Time step for solving the Fokker-Planck equation
# Unit: [Gyr]
time_step = float(default=0.02, min=1e-4, max=0.1)
# Electron injection, which is assumed to have a constant injection
# rate and a power-law spectrum.
injection_index = float(default=2.4, min=2.1, max=3.5)
# Extragalactic point sources
[[pointsources]]
# Output directory to save the simulated catalog
output_dir = string(default="PS_tables")
# PS components to be simulated
pscomponents = string_list(default=list())
# Resolution [arcmin]
resolution = float(default=0.6, min=0.0)
[[[starforming]]]
# Number of samples
numps = integer(default=1000)
# Prefix
prefix = string(default="SF")
[[[starbursting]]]
# Number of samples
numps = integer(default=1000)
# Prefix
prefix = string(default="SB")
[[[radioquiet]]]
# Number of samples
numps = integer(default=1000)
# Prefix
prefix = string(default="RQ")
[[[FRI]]]
# Number of samples
numps = integer(default=1000)
# Prefix
prefix = string(default="FRI")
[[[FRII]]]
# Number of samples
numps = integer(default=1000)
# Prefix
prefix = string(default="FRII")
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