# # Configurations for "fg21sim" # Syntax: `ConfigObj`, https://github.com/DiffSK/configobj # # Foreground components to be simulated [foregrounds] # Diffuse Galactic synchrotron emission (unpolarized) galactic/synchrotron = boolean(default=False) # Diffuse Galactic free-free emission galactic/freefree = boolean(default=False) # Galactic supernova remnants emission galactic/snr = boolean(default=False) # Extragalactic clusters of galaxies emission extragalactic/clusters = boolean(default=False) # Simulation sky/region configurations [sky] # Type of the input/output simulation sky # + patch: # Input/output sky template is only a (square) patch of the sky. # The simulated output maps have the same coverage/field as the # input template, as well as the coordinate projection. # + healpix: # Input/output sky template covers (almost) all sky, and stored # in HEALPix format. The simulated output maps will also be # all-sky using the HEALPix projection. type = option("patch", "healpix", default="patch") # Configurations for input/output sky patch [[patch]] # The (R.A., Dec.) coordinate of the sky patch center # Unit: [deg] # (MWA EoR0 field center: (0, -27)) xcenter = float(default=0, min=0, max=360) ycenter = float(default=-27, min=-90, max=90) # The image dimensions (i.e., number of pixels) of the sky patch, # along the X (R.A./longitude) and Y (Dec./latitude) axes. # Default: 1800x1800 => 10x10 [deg^2] (20 arcsec/pixel) xsize = integer(default=1800, min=1) ysize = integer(default=1800, min=1) # Pixel size [arcsec] pixelsize = float(default=20, min=0) # Configurations for input/output HEALPix sky [[healpix]] # HEALPix Nside value, i.e., pixel resolution nside = integer(default=1024, min=128) # Frequencies specification of the simulation products [frequency] # How to specify the frequencies # + custom: # directly specify the frequency values using the "frequencies" config # + calc: # calculate the frequency values by "start", "stop", and "step" type = option("custom", "calc", default="custom") # The frequency values to be simulated if above "type" is "custom". # Unit: [MHz] frequencies = float_list(default=list()) # Parameters to calculate the frequencies # NOTE: "start" and "stop" frequencies are both inclusive. # Unit: [MHz] start = float(default=None) stop = float(default=None) step = float(default=None) # Configuration for output products [output] # Filename pattern for the output products, which will be finally # formatted using `str.format()`. filename_pattern = string(default="{prefix}_{frequency:06.2f}.fits") # Use single-precision float instead of double (to save spaces) float32 = boolean(default=True) # Whether to calculate the checksum for the output FITS file? # NOTE: May cost significantly more time on writing FITS file. checksum = boolean(default=False) # Whether to overwrite existing files (e.g., maps, catalogs, manifest, ...) clobber = boolean(default=False) # Filename of the simulation products manifest (JSON format), which # records all output products together with their sizes and MD5 hashes. # Do not create such a manifest if this option is not specified. manifest = string(default=None) # Cosmological parameters # References: Komatsu et al. 2011, ApJS, 192, 18; Tab.(1) [cosmology] # Hubble constant at z=0; [km/s/Mpc] H0 = float(default=71.0, min=0.0) # Density of non-relativistic matter in units of the critical density at z=0 OmegaM0 = float(default=0.27, min=0.0, max=1.0) # Density of the baryon at present day Omegab0 = float(default=0.046, min=0.0, max=1.0) # Present-day CMB temperature; [K] Tcmb0 = float(default=2.725) # Present-day rms density fluctuations on a scale of 8 h^-1 [Mpc] sigma8 = float(default=0.81, min=0.0) # Scalar spectral index ns = float(default=0.96, min=0.0) # Configurations for initialization/reconfiguration of the `logging` module [logging] # debug: Detailed information, typically of interest only when diagnosing # problems. # info: Confirmation that things are working as expected. # warning: An indication that something unexpected happended, or indicative # of some problem in the near future (e.g., "disk space low"). # The software is still working as expected. # error: Due to a more serious problem, the software has not been able to # perform some function. # critical: A serious error, indicating that the program itself may be unable # to continue running. level = option("debug", "info", "warning", "error", "critical", default="info") # Set the format of displayed messages format = string(default="%(asctime)s [%(levelname)s] <%(name)s:%(lineno)d> %(message)s") # Set the date/time format in messages datefmt = string(default="%H:%M:%S") # Set the logging filename (will create a `FileHandler`) # If set to "" (empty string), then the `FileHandler` will be disabled. filename = string(default="") # Set the stream used to initialize the `StreamHandler` # If set to "" (empty string), then the `StreamHandler` will be disabled. stream = option("stderr", "stdout", "", default="stderr") # # Galactic emission components # [galactic] # Synchrotron emission component (unpolarized) [[synchrotron]] # The template map for the simulation, e.g., Haslam 408 MHz survey. # Unit: [K] (Kelvin) template = string(default=None) # The frequency of the template map. # Unit: [MHz] template_freq = float(default=None, min=0) # Spectral index map indexmap = string(default=None) # Whether add fluctuations on the small scales according the angular # power spectrum prediction? add_smallscales = boolean(default=False) # Range of multipole moments (l) of the angular power spectrum. # The power spectrum will be cut off to a constant for multipole l < lmin. # NOTE: Update the ``lmax`` accordingly w.r.t. ``sky/healpix/nside``. # Generally, lmax = 3 * nside - 1 lmin = integer(min=0, default=10) lmax = integer(min=1, default=3071) # Filename prefix for this component prefix = string(default="gsync") # Output directory to save the simulated results output_dir = string(default=None) # Free-free bremsstrahlung emission component [[freefree]] # The Hα map from which to derive the free-free emission # Unit: [Rayleigh] halphamap = string(default=None) # The 100-μm dust map used to correct Hα dust absorption # Unit: [MJy/sr] dustmap = string(default=None) # Effective dust fraction in the LoS actually absorbing Halpha dust_fraction = float(default=0.33, min=0.1, max=1) # Halpha absorption threshold: # When the dust absorption goes rather large, the true Halpha # absorption can not well determined. This configuration sets the # threshold below which the dust absorption can be well determined, # while the sky regions with higher absorption are masked out due # to unreliable absorption correction. # Unit: [mag] halpha_abs_th = float(default=1) # The electron temperature assumed for the ionized interstellar medium # that generating Hα emission. # Unit: [K] electron_temperature = float(default=7000, min=1000) # Filename prefix for this component prefix = string(default="gfree") # Output directory to save the simulated results output_dir = string(default=None) # Supernova remnants emission [[snr]] # The Galactic SNRs catalog data (CSV file) catalog = string(default=None) # Output the effective/inuse SNRs catalog data (CSV file) catalog_outfile = string(default=None) # Resolution for simulating each SNR template, which are finally # mapped to the all-sky HEALPix map if used. # Unit: [arcsec] resolution = float(default=30, min=5) # Filename prefix for this component prefix = string(default="gsnr") # Output directory to save the simulated results output_dir = string(default=None) # # Extragalactic emission components # [extragalactic] # # Press-Schechter formalism to determine the cluster distributions # with respect to mass and redshift, from which to further determine # the total number of clusters within a sky patch and to sample the # masses and redshifts for each cluster. # [[psformalism]] # The model of the fitting function for halo/cluster 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!) cluster mass # 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) z_max = float(default=4, min=1, max=100) z_step = float(default=0.01, min=0.001, max=1) # Output file (NumPy ".npz" format) to save the calculated halo mass # distributions at every redshift. # # This file packs the following 3 NumPy arrays: # * ``z``: # Redshifts where the halo mass distribution is calculated. # * ``mass``: # (Logarithmic-distributed) mass points. # Unit: [Msun] (the little "h" is folded into the values) # * ``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) 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 cluster catalog containing the simulated # mass, redshift, position, shape, recent merger info, etc. catalog_outfile = string(default=None) # Whether to dump the raw data of the simulated cluster catalog in # Python native pickle format (i.e., ".pkl") to a file with the same # basename as the above ``catalog_outfile``? # The dumped data can be easily loaded back for reuse. dump_catalog_data = boolean(default=True) # Whether to directly use the (previously simulated) catalog data as # specified by the above "catalog_outfile" and ``dump_catalog_data`` # options? # # 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_dump_catalog_data = 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: for testing usage. boost = float(default=1) # Minimal elongated fraction for creating the images of radio halos # The ``felong`` is defined as ``felong = b/a``, similar to the Hubble # classification for the elliptical galaxies. ``felong_min = 1.0`` # means no elongation, and ``felong_min = 0.6`` is a good choice as # the observed radio halos are generally regular. felong_min = float(default=1, min=0.1, max=1) # 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=1e13, min=1e11, 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, min=1, max=5) # 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, # with: kT_out ~ 0.5 [keV] # Reference: Fujita et al. 2003, ApJ, 584, 190; Eq.(49) # Unit: [keV] kT_out = float(default=0, min=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 # [[halos]] # A custom factor to tune the turbulent acceleration efficiency. # NOTE: This parameter incorporates the efficiency factor describing # the effectiveness of the ICM plasma instabilities. f_acc = float(default=1, min=0.1, max=10) # The factor that is multiplied to the turbulence injection radius # to derive the radio halo radius. f_radius = float(default=1, min=0.1, max=10) # 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=0.003, min=0.001, max=0.1) # The energy density ratio of cosmic ray to the thermal ICM. # NOTE: Equipartition between the magnetic field and cosmic ray is # assumed, i.e., eta_b == x_cr. x_cr = float(default=0.015, min=0.001, max=0.1) # The scaling index of the diffusion coefficient (D_γγ) w.r.t. the # mass of the main cluster. mass_index = float(default=0, min=0, max=2) # The spectral index of the injected primary electrons. 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=1e6) # Number of cells on the logarithmic momentum grid used to solve the # Fokker-Planck equation. gamma_np = integer(default=256) # 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. # # NOTE: To disable the boundary fix, set this to 0, otherwise, set to # a number >= 2. It is suggested to be about 5%-10% of the # ``gamma_np``. buffer_np = integer(default=10, min=0) # Time step for solving the Fokker-Planck equation # Unit: [Gyr] time_step = float(default=0.02, 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=1, min=0) # Parameters of the beta-model that is used to describe the gas density # profile of the cluster. # The fraction of the core radius to cluster's virial radius. f_rc = float(default=0.1) # The slope parameter (i.e., beta). beta = float(default=0.8)