# 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) # 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")