# 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("smt", "jenkins", "ps", default="ps") # 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=1e12, 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) # Whether to 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=1e14, min=1e13) # 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) # Number of most powerful halos to be dropped out. halo_dropout = integer(default=0, min=0) # 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) # The trace back time when to stop tracing the merging history of # clusters. ~2-3 Gyr should be enough since the turbulence acceleration # effective time ~<1 Gyr and the halo lifetime is also short compared # to mergers. # Unit: [Gyr] time_traceback = float(default=3.0, min=1.0, max=5.0) # Mass ratio of the main and sub clusters, below which is regarded as # a major merger event. ratio_major = float(default=5.0, min=1.0, max=10.0) # Whether to use the maximum merger event (i.e., biggest mass of the # sub cluster) within the above ``tau_merger`` timescale to simulate the # subsequent radio halo simulation? Otherwise only the most recent major # merger event will be used. use_max_merger = boolean(default=False) # The fraction of the magnetic field energy density w.r.t. the ICM # thermal energy density, which is used to determine the mean magnetic # field strength within the ICM and is also assumed to be uniform. eta_b = float(default=0.001, min=1e-5, max=0.1) # The temperature of the outer gas surrounding the cluster. Accretion # shocks form near the cluster virial radius during the cluster formation, # which can heat the cluster ICM to have a higher temperature than the # virial temperature: # kT_icm ~ kT_vir + 1.5 * kT_out # Reference: Fujita et al. 2003, ApJ, 584, 190; Eq.(49) # Unit: [keV] kT_out = float(default=0.5, min=0, max=1) # Filename prefix for this component prefix = string(default="cluster") # Output directory to save the simulated results output_dir = string(default=None) # # Giant radio halos # [[halos]] # A custom parameter to tune the turbulent acceleration timescale. # NOTE: The smaller this parameter, the shorter the acceleration # timescale, therefore more efficient acceleration. f_acc = float(default=1.0, min=0.1, max=10) # The turbulence is generally injected at the cluster center during # a merger. This option parameterize the turbulence injection scale # to be a fraction of the virial radius of the cluster, which is also # used to determine the radio halo size. f_lturb = float(default=0.33, min=0.1, max=1.0) # An efficiency factor describing the effectiveness of plasma # instabilities (e.g., due to spatial or temporal intermittency). zeta_ins = float(default=0.1, min=0.1, max=1.0) # The fraction of merger energy transferred into the turbulence. eta_turb = float(default=0.1, min=0.1, max=0.5) # The fraction of the thermal energy injected into the cosmic-ray # electrons during the cluster life time. eta_e = float(default=0.001, min=0.001, max=0.1) # The ratio of cosmic ray (including protons and electrons) energy # density (i.e., pressure) to the thermal energy density. # NOTE: Fermi-LAT has placed an upper limit of ~1.25%-1.4% # (Ackermann et al. 2014, ApJ, 787, 18) # NOTE: The energy ratio of cosmic-ray electrons to protons K_ep ~0.01 # for our Galaxy (Pinzke et al. 2017, MNRAS, 465, 4800) x_cr = float(default=0.01, min=0.001, max=0.1) # Electron injection, which is assumed to have a constant injection # rate and a power-law spectrum. injection_index = float(default=2.3, min=2.1, max=3.0) # Minimum and maximum Lorentz factor (i.e., energy) of the relativistic # electron spectrum. gamma_min = float(default=1) gamma_max = float(default=1e5) # Number of cells on the logarithmic momentum grid used to solve the # Fokker-Planck equation. gamma_np = integer(default=200) # Number of cells used as the buffer regions near both the lower # and upper boundaries, within which the values will be replaced by # extrapolating from the inner-region data, in order to avoid the # unphysical particle pile-ups. # It is suggested to be about 5%-10% of the above ``gamma_np``. # NOTE: * set to 0 to disable boundary fixes; # * otherwise, set to a number >= 2. buffer_np = integer(default=10, min=0) # Time step for solving the Fokker-Planck equation # Unit: [Gyr] time_step = float(default=0.01, min=1e-4, max=0.1) # How long the period before the merger begins, which is used to derive # an approximately steady initial electron spectrum. During this period, # the acceleration is turned off and only leaves energy loss mechanisms. # Unit: [Gyr] time_init = float(default=0.6, min=0) # # 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")