# coding=utf-8 #=============================================== #HOME INFORMATION #=============================================== pd_source_dir = '/home/desika.narayanan/pd_git/' #=============================================== #RESOLUTION KEYWORDS #=============================================== oref = 0 # over refine factor - should typically be set to 0 n_ref = 128 # when n_particles > n_ref, octree refines further zoom_box_len = 100 # kpc; so the box will be +/- zoom_box_len from the center bbox_lim = 1.e5 # kpc - this is the initial bounding box of the grid (+/- bbox_lim) # This *must* encompass all of the particles in the # simulation. #=============================================== #PARALLELIZATION #=============================================== n_processes = 16 # number of pool processes to run for stellar SED generation n_MPI_processes = 1 # number of MPI tasks to run. for TORQUE this is # best set as the same as n_processes, while for SLURM this may not be the case. #=============================================== #RT INFORMATION #=============================================== n_photons_initial = 1.e6 n_photons_imaging = 1.e6 n_photons_raytracing_sources = 1.e6 n_photons_raytracing_dust = 1.e6 FORCE_RANDOM_SEED = False seed = -12345 # has to be an int, and negative. #=============================================== #DUST INFORMATION #=============================================== dustdir = '/home/desika.narayanan/hyperion-dust-0.1.0/dust_files/' #location of your dust files dustfile = 'd03_3.1_6.0_A.hdf5' PAH = False dust_grid_type = 'dtm' # needs to be in ['dtm','rr','manual','li_bestfit','li_ml'] dusttometals_ratio = 0.25 # skirt assumes 0.25: see http://www.skirt.ugent.be/tutorials/_tutorial_hydro_s_p_h.html ("dust system"subheading) enforce_energy_range = False # False is the default; ensures energy conservation SUBLIMATION = True # do we automatically kill dust grains above the # sublimation temperature; right now is set to fast # mode SUBLIMATION_TEMPERATURE = 1600. #K -- meaningliess if SUBLIMATION == False #=============================================== #STELLAR SEDS INFO #=============================================== FORCE_BINNED = True # If True, force all star particles to be binned for calculating SED. # If False, all star particles below max_age_direct (next parameter) are added # directly without binning for calculating SED max_age_direct = 1.e-2 # Age (in Gyr) below which stars will be directly added without binning (works only if FORCE_BINNED is False) imf_type = 2 # FSPS imf types; 0 = salpeter, 1 = chabrier; 2 = kroupa; 3 and 4 (vandokkum/dave) not currently supported imf1 = 1.3 # Logarithmic slope of the IMF over the range 0.08 < M < 0.5. Only used if imf_type=2. (Default: 1.3) imf2 = 2.3 # Logarithmic slope of the IMF over the range 0.5 < M < 1.0. Only used if imf_type=2. (Default: 2.3) imf3 = 2.3 # Logarithmic slope of the IMF over the range 1.0 < M < 120. Only used if imf_type=2. (Default: 2.3) pagb = 1 # weight given to post agb stars# 1 is the default add_agb_dust_model = False # add circumstellar AGB dust model (100%); Villaume, Conroy & Jonson 2015 use_cmdf = False # If True, star particles that fit the criteria for nebular emission (see next section) are broken down # using a cluster mass distribution function (cmdf) even if nebular emission is turned off (add_nebular_emission = False). # This allows for one to one comparison of models with and without nebular emission. The cmdf is set by the following # parameters defined under nebular emission info (next section): cmdf_min_mass, cmdf_max_mass, cmdf_bins and cmdf_beta. #=============================================== #NEBULAR EMISSION INFO #=============================================== add_neb_emission = False # add nebular line emission (under active development) use_cloudy_tables = True # If True, CLOUDY look up tables (dev. by Nell Byler) will be used to calculate # nebular emission. If False, CLOUDY models are generated individually # for each young star particle (under active development). # Note: The lookup tables work only for stars particles below 10 Myr. (Default: True) cmdf_min_mass = 3.5 # While calulating nebular emission from young stars and PAGB stars one star particle is broken down # into smaller star cluster by assuming a cluster mass distribution function of the form dN/dM goes as M^(beta). # This parameter sets the minimum mass of the star clusters in units of log(Msun). Note this value # should not be set lower than 3.5. (Default = 3.5) cmdf_max_mass = 5.0 # Minimum mass of the star clusters in units of log(Msun). (Default = 5.0) cmdf_bins = 6 # The number of bins used for calulating the cluster mass distribution function (Default = 6.0) cmdf_beta = -2.0 # Beta (power law exponent) for calculating CMDF (dN/dM goes as M^(beta)) #********************** # COMMON PARAMETERS #*********************** # NOTE: These parmeters take either three or four values as an input. # They correspond to the value of the pararmeter for young_stars, PAGB stars, AGN and DIG respectively. FORCE_gas_logu = [False, False, False] # If set, then we force the ionization parameter (gas_logu) to be # gas_logu (next parameter) else, it is taken to be variable and dependent on ionizing # radiation from star particles. (Default: [False, False, False]) gas_logu = [-2.0, -2.0, -2.0] # Gas ionization parameter. This is only relevant # if add_neb_emission is set to True and FORCE_gas_logu is set to True (Default: [-2.0, -2.0, -2.0]) gas_logu_init = [0.0, 0.0, 0.0] # Force the ionization parameter to increase/decrease by this value (Scale: log). # Useful if you want to run tests (Default: [0.0, 0.0, 0.0]) FORCE_gas_logz = [False, False, False] # If set, then we force the metallicity (gas_logz) to be gas_logz (next parameter) # else, it is taken to be the star particles metallicity. (Default: [False, False, False]) gas_logz = [0.0, 0.0, 0.0] # Metallicity of the HII region in units of log(Z/Z_sun) # only relevant if add_neb_emission = True and FORCE_gas_logz = True (Default: [0.0, 0.0, 0.0]) FORCE_logq = [False, False, False] # If set, then we force the number of ionizing photons to be source_logq (next parameter) # else, it is taken to be variable and dependent on ionizing radiation of the source. (Default: [False, False, False]) source_logq = [1.e47, 1.e47,1.e47] # The number of ionizing photons emitted by the source in units of s^-1. Only relevant if add_neb_emission = True, # use_cloudy_tables = True and FORCE_gas_logq = True (Default: [1.e47,1.e47,1.e47]) FORCE_inner_radius = [False, False, True] # If set, then we force the inner radius of the cloud to be inner_radius (next parameter). # IMP Note: This works only for young stars and Post-AGB stars. # For AGN we keep the inner radius fixed at whatever is set by inner_radius (next parameter) # irrespective of what this parameter is set to. (Default: [False,False,True]) inner_radius = [1.e19, 1.e19, 2.777e+20] # This sets the inner radius of the cloud in cm. This is used only when add_neb_emission = True, # use_cloudy_tables = False and FORCE_inner_radius = True (Default: [1.e19, 1.e19, 2.777e+20], Units = cm) FORCE_N_O_Pilyugin = [False, False, False, False] # If set to True, Nitrogen abundances are set according to the N/O vs O/H relation from Pilyugin et al. 2012 # If FORCE_N_O ratio (next parameter) is set to True then this parameter is ignored.(Default: [False,False,False]) FORCE_N_O_ratio = [False, False, False, False] # If set, then we force the log of N/O ratio to be N_O_ratio (next parameter). # This can be used as a template fix adundance ratio of other elements (Default: [False, False, False]) N_O_ratio = [-0.85, -0.85, -0.85, -0.85] # This sets the log of N/O ratio. This is used only when add_neb_emission = True, # use_cloudy_tables = False, FORCE_N/O ratio = True and neb_abund = "direct" (Default: = [-0.85, -0.85, -0.85]) neb_abund = ["dopita", "dopita", "dopita", "dopita"] # This sets the HII region elemental abundances for generating CLOUDY models. # Available abundaces are. # dopita: Abundabces from Dopita (2001) with old solar abundances = 0.019 and ISM grains. # newdopita: Abundances from Dopita (2013). Solar Abundances from Grevasse 2010 - z= 0.013 # includes smooth polynomial for N/O, C/O relationship functional form for He(z), # new depletion and factors in ISM grains. # gutkin: Abundabces from Gutkin (2016) and PARSEC metallicity (Bressan+2012) based on Grevesse+Sauvel (1998) # and Caffau+2011 # direct: Abundances are taken directly from the simulation if possible. Defaults to using "dopita" if there is # an error. (Note: Works only for AGNs and star particles that are added directly without binning. # Make sure to set FORCE_BINNED to False) # This is used only when add_neb_emission = True and use_cloudy_tables = False. (Default: ["dopita", "dopita", "dopita"]) #*************************** # YOUNG STARS (HII regions) #*************************** add_young_stars = True # If set, the young stars are included when calculating nebular emission (Default: False) HII_Rinner_per_Rs = 0.01 # Rinner for cloudy calculations is set to this value times the Stromgen Radius. # For example, if set to 0.01 Rinner is taken to be 1 % of Stromgren Radius. # If FORCE_inner_radius (next parameter) is set to True then this is overridden # and the value set by the inner_radius is used. This parameter is used # only when add_neb_emission = True and use_cloudy_tables = False (Default: 0.01) HII_nh = 1.e2 # Gas hydrogen density for calcualting nebular emission in units if cm^-3. # This is used only when add_neb_emission = True and use_cloudy_tables = False (Default = 1.e2) HII_min_age = 1.e-3 # Sets the minimum age limit for calculating nebular emission in units of Gyr. # This is used only when add_neb_emission = True and use_cloudy_tables = False (Default = 1.e-3) HII_max_age = 1.e-2 # Sets the maximum age limit for calculating nebular emission in units of Gyr. # This is used only when add_neb_emission = True and use_cloudy_tables = False (Default = 1.e-2) HII_escape_fraction = 0.0 # Fraction of H-ionizaing photons that escape the HII region. # This is used only when add_neb_emission = True and use_cloudy_tables = False (Default = 0.0) HII_alpha_enhacement = False # If set to True then the metallicity of star particles to Fe/H rather than the total metals. # Since FSPS does not support non solar abundance ratios, this parameter can be used to mimic the # hardening of the radiaiton field due to alpha-enhancement. (Default: False) #**************** # Post-AGB STARS #**************** add_pagb_stars = False # If set, the Post-AGB stars are included when calculating nebular emission (Default: False) PAGB_N_enhancement = 0.4 # Enhances the Nitrogen abundance Post-AGB stars by increasing the log(N/O) by this value. # This used only when add_neb_emission = True, use_cloudy_tables = False and add_pagb_stars = True (Default = 0.4) PAGB_C_enhancement = 0.4 # Enhances the Carbon abundance Post-AGB stars by increasing the log(C/O) by this value. # This used only when add_neb_emission = True, use_cloudy_tables = False and add_pagb_stars = True (Default = 0.4) PAGB_Rinner_per_Rs = 0.01 # Rinner for cloudy calculations is set to this value times the Stromgen Radius. # For example, if set to 0.01 Rinner is taken to be 1 % of Stromgren Radius. # If FORCE_inner_radius (next parameter) is set to True then this is overridden # and the value set by the inner_radius is used. This parameter is used # only when add_neb_emission = True and use_cloudy_tables = False (Default: 0.01) PAGB_nh = 1.e2 # Gas hydrogen density for calcualting nebular emission in units if cm^-3. # This is used only when add_neb_emission = True and use_cloudy_tables = False (Default = 1.e2) PAGB_min_age = 0.1 # Sets the minimum age limit for calculating nebular emission from post-AGB stars, in units of Gyr. # This is used only when add_neb_emission = True, use_cloudy_tables = False and add_pagb_stars = True (Default = 0.1) PAGB_max_age = 10 # Sets the maximum age limit for calculating nebular emission from post-AGB stars, in units of Gyr. # This is used only when add_neb_emission = True, use_cloudy_tables = False and add_pagb_stars = True (Default = 10) PAGB_escape_fraction = 0.0 # Fraction of H-ionizaing photons that escape the HII region. # This is used only when add_neb_emission = True and use_cloudy_tables = False (Default = 0.0) #************** # AGN #************** add_AGN_neb = False # If set, AGNs are included when calculating nebular emission (Default: False) AGN_nh = 1.e3 # Gas hydrogen density for calcualting nebular emission in units if cm^-3. # This is used only when add_neb_emission = True and use_cloudy_tables = False (Default = 1.e2) AGN_num_gas = 32 # For CLOUDY calculations we use the distance weighted average metallicity of gas particles around the AGN. # The number of gas particles used for doing so is set by this parameter. (Default: 32) #********************** # DIffused Ionized Gas (DIG) #********************** add_DIG_neb = False # If set, Contribution from DIG is included when calculating nebular emission (Default: False) DIG_nh = 1.e1 # Gas hydrogen density for calcualting nebular emission in units of cm^-3. (Default: 10) DIG_min_factor = 1 # For DIG CLOUDY calculations we use Black (1987) SED as a template. The normalization of the SED is # set by a parameter called "Factor". It is the ratio of total energy dumped in a cell to the total # energy of the Black (1987) SED, which we use as the template for setting the SED shape for calculating # DIG emission. This parameter sets the minimum factor that the code uses for calculation. For example, # setting this parameter to 1 causes the code to ignore all the cells that have a factor < 1 or in other # words ignore all the cells where the total energy dumped is less than the integrated energy of the # Black (1987) SED (Default: 1). #************************* # DEBUGGING AND CLEAN UP #************************* dump_emlines = False # If True, The emission lines are saved in a file before going through the dust radiative transfer. # This can be used as a fast way getting emission lines for the purpose of debugging the code. # Naming convention: emlines.galaxy*.txt where * is the galaxy number # This works only when add_neb_emission = True (Default: False) cloudy_cleanup = True # If set to True, all the CLOUDY files will be deleted after the source addition is complete. # Only relevant if add_neb_emission = True and use_cloudy_tables = False (Default: True) #=============================================== #BIRTH CLOUD INFORMATION #=============================================== CF_on = False # if set to true, then we enable the Charlot & Fall birthcloud models birth_cloud_clearing_age = 0.01 # Gyr - stars with age < # birth_cloud_clearing_age have # charlot&fall birthclouds meaningless # of CF_on == False #=============================================== # Idealized Galaxy SED Parameters #=============================================== Z_init = 0 # force a metallicity increase in the newstar particles. # This is useful for idealized galaxies. The units for this # are absolute (so enter 0.02 for solar). Setting to 0 # means you use the stellar metallicities as they come in # the simulation (more likely appropriate for cosmological # runs) #NOTE - this is not exclusively used for idealized #simulations (i.e. one could use this for a cosmological #simulation), but the typical use case is for idealized simulations. disk_stars_age = 8 # Gyr ;meaningless if this is a cosmological simulation bulge_stars_age = 8 # Gyr ; meaningless if this is a cosmological simulation disk_stars_metals = 19 # in fsps metallicity units bulge_stars_metals = 19 # in fsps metallicity units #=============================================== # Stellar Ages and Metallicities #=============================================== # bins for binning the stellar ages and metallicities for SED # assignments in cases of many (where many == # >N_METALLICITY_BINS*N_STELLAR_AGE_BINS) stars; this is necessary for # reduction of memory load; see manual for details. N_STELLAR_AGE_BINS = 100 metallicity_legend= "/home/desika.narayanan/pd_git/fsps_files/zlegend.mist.dat" #=============================================== #BLACK HOLES #=============================================== BH_SED = False BH_eta = 0.1 #bhluminosity = BH_eta * mdot * c**2. BH_model = "Nenkova" BH_modelfile = "/home/desika.narayanan/pd_git/agn_models/clumpy_models_201410_tvavg.hdf5" # The Nenkova BH_modelfile can be downloaded here: # https://www.clumpy.org/downloads/clumpy_models_201410_tvavg.hdf5 BH_var = True # Include time variations on BH luminosity (default Hickox+ 2014) nenkova_params = [5,30,0,1.5,30,40] #Nenkova+ (2008) model parameters #=============================================== #IMAGES AND SED PARAMETERS #=============================================== NTHETA = 1 NPHI = 1 SED = True SED_MONOCHROMATIC = False FIX_SED_MONOCHROMATIC_WAVELENGTHS = False # if set, then we only use # the wavelengths in the # range between min_lam and # max_lam SED_MONOCHROMATIC_min_lam = 0.3 # micron SED_MONOCHROMATIC_max_lam = 0.4 # micron IMAGING = False filterdir = '/home/desika.narayanan/pd_git/filters/' filterfiles = [ 'arbitrary.filter', # 'ACS_F475W.filter', # 'ACS_F606W.filter', # 'ACS_F814W.filter', # 'B_subaru.filter', ] # Insert additional filter files as above. In bash, the following command # formats the filenames for easy copying/pasting. # $ shopt -s globstar; printf "# '%s'\n" *.filter npix_x = 128 npix_y = 128 #experimental and under development - not advised for use IMAGING_TRANSMISSION_FILTER = False filter_list = ['filters/irac_ch1.filter'] TRANSMISSION_FILTER_REDSHIFT = 0.001 #=============================================== #GRID INFORMATION #=============================================== MANUAL_ORIENTATION = False THETA = 0 PHI = 0 #=============================================== #OTHER INFORMATION #=============================================== solar = 0.013 PAH_frac = {'usg': 0.0586, 'vsg': 0.1351, 'big': 0.8063} # values will be normalized to 1 #=============================================== #DEBUGGING -THE PERFORMANCE OF THE CODE USING THESE PARAMETERS IS NOT GUARANTEED #=============================================== SOURCES_RANDOM_POSITIONS = False SOURCES_IN_CENTER = False STELLAR_SED_WRITE = True SKIP_RT = False # skip radiative transfer (i.e. just read in the grids and maybe write some diagnostics) SUPER_SIMPLE_SED = False # just generate 1 oct of 100 pc on a side, # centered on [0,0,0]. sources are added at # random positions. SKIP_GRID_READIN = False CONSTANT_DUST_GRID = False # if set, then we don't create a dust grid by # smoothing, but rather just make it the same # size as the octree with a constant value of # 4e-20 N_MASS_BINS = 0 # this is really just a place holder that exists in # some loops to be able to insert some code downstream # for spatially varying IMFs. right now for speed best # to set to 1 as it doesn't actually do anything. FORCE_STELLAR_AGES = False FORCE_STELLAR_AGES_VALUE = 0.05# Gyr FORCE_STELLAR_METALLICITIES = False FORCE_STELLAR_METALLICITIES_VALUE = 0.012 # absolute values (so 0.013 ~ solar) NEB_DEBUG = False # Dumps parameters related to nebular line emission in a file for debugging. # The file includes the ionization parameter, number of ionizing photons, # metallicity, inner radius, stellar mass and age for each particle. # Naming convention: nebular_properties_galaxy*.txt where * is the galaxy number DIFF_DIG_SED = False # If set, SEDs with DIG nebular emission are saved separately with "_DIG" appended to the rtout files