comoving_DM_softening:0.003320# Comoving softening for DM (3.32 ckpc)
max_physical_DM_softening:0.001300# Physical softening for DM (1.30 pkpc)
comoving_baryon_softening:0.001790# Comoving softening for baryons (1.79 ckpc)
max_physical_baryon_softening:0.000700# Physical softening for baryons (0.70 pkpc)
# Parameters for the hydrodynamics scheme
SPH:
resolution_eta:1.2348# Target smoothing length in units of the mean inter-particle separation (1.2348 == 48Ngbs with the cubic spline kernel).
h_min_ratio:0.1# Minimal smoothing length in units of softening.
h_max:0.5# Maximal smoothing length in co-moving internal units.
CFL_condition:0.2# Courant-Friedrich-Levy condition for time integration.
minimal_temperature:100.0# (internal units)
initial_temperature:268.7# (internal units)
particle_splitting:1# Particle splitting is ON
particle_splitting_mass_threshold:7e-4# (internal units, i.e. 7e6 Msun ~ 4x initial gas particle mass)
# Parameters of the stars neighbour search
Stars:
resolution_eta:1.1642# Target smoothing length in units of the mean inter-particle separation
h_tolerance:7e-3
# Parameters for the Friends-Of-Friends algorithm
FOF:
basename:fof_output# Filename for the FOF outputs.
min_group_size:256# The minimum no. of particles required for a group.
linking_length_ratio:0.2# Linking length in units of the main inter-particle separation.
black_hole_seed_halo_mass_Msun:1.5e10# Minimal halo mass in which to seed a black hole (in solar masses).
scale_factor_first:0.05# Scale-factor of first FoF black hole seeding calls.
delta_time:1.00751# Scale-factor ratio between consecutive FoF black hole seeding calls.
Scheduler:
max_top_level_cells:8
cell_split_size:200
Restarts:
onexit:1
delta_hours:6.0
max_run_time:71.5# Three days minus fergie time
resubmit_on_exit:1
resubmit_command:./resub.sh
# Parameters related to the initial conditions
InitialConditions:
file_name:EAGLE_L0012N0188_ICs.hdf5
periodic:1
cleanup_h_factors:1# Remove the h-factors inherited from Gadget
cleanup_velocity_factors:1# Remove the sqrt(a) factor in the velocities inherited from Gadget
generate_gas_in_ics:1# Generate gas particles from the DM-only ICs
cleanup_smoothing_lengths:1# Since we generate gas, make use of the (expensive) cleaning-up procedure.
remap_ids:1# Re-map the IDs to [1, N] to avoid collision problems when splitting
# Parameters of the line-of-sight outputs
LineOfSight:
basename:eagle_los
num_along_x:0
num_along_y:0
num_along_z:100
scale_factor_first:0.1
delta_time:1.1
# Impose primoridal metallicity
EAGLEChemistry:
init_abundance_metal:0.
init_abundance_Hydrogen:0.752
init_abundance_Helium:0.248
init_abundance_Carbon:0.0
init_abundance_Nitrogen:0.0
init_abundance_Oxygen:0.0
init_abundance_Neon:0.0
init_abundance_Magnesium:0.0
init_abundance_Silicon:0.0
init_abundance_Iron:0.0
# EAGLE cooling parameters
EAGLECooling:
dir_name:./coolingtables/
H_reion_z:7.5# Planck 2018
H_reion_eV_p_H:2.0
He_reion_z_centre:3.5
He_reion_z_sigma:0.5
He_reion_eV_p_H:2.0
# COLIBRE cooling parameters
COLIBRECooling:
dir_name:./UV_dust1_CR1_G1_shield1.hdf5# Location of the cooling tables
H_reion_z:7.5# Redshift of Hydrogen re-ionization (Planck 2018)
H_reion_eV_p_H:2.0
He_reion_z_centre:3.5# Redshift of the centre of the Helium re-ionization Gaussian
He_reion_z_sigma:0.5# Spread in redshift of the Helium re-ionization Gaussian
He_reion_eV_p_H:2.0# Energy inject by Helium re-ionization in electron-volt per Hydrogen atom
delta_logTEOS_subgrid_properties:0.3# delta log T above the EOS below which the subgrid properties use Teq assumption
rapid_cooling_threshold:0.333333# Switch to rapid cooling regime for dt / t_cool above this threshold.
# EAGLE star formation parameters
EAGLEStarFormation:
EOS_density_norm_H_p_cm3:0.1# Physical density used for the normalisation of the EOS assumed for the star-forming gas in Hydrogen atoms per cm^3.
EOS_temperature_norm_K:8000# Temperature om the polytropic EOS assumed for star-forming gas at the density normalisation in Kelvin.
EOS_gamma_effective:1.3333333# Slope the of the polytropic EOS assumed for the star-forming gas.
KS_normalisation:1.515e-4# The normalization of the Kennicutt-Schmidt law in Msun / kpc^2 / yr.
KS_exponent:1.4# The exponent of the Kennicutt-Schmidt law.
min_over_density:57.7# The over-density above which star-formation is allowed.
KS_high_density_threshold_H_p_cm3:1e3# Hydrogen number density above which the Kennicut-Schmidt law changes slope in Hydrogen atoms per cm^3.
KS_high_density_exponent:2.0# Slope of the Kennicut-Schmidt law above the high-density threshold.
EOS_entropy_margin_dex:0.3# Logarithm base 10 of the maximal entropy above the EOS at which stars can form.
threshold_norm_H_p_cm3:0.1# Normalisation of the metal-dependant density threshold for star formation in Hydrogen atoms per cm^3.
threshold_Z0:0.002# Reference metallicity (metal mass fraction) for the metal-dependant threshold for star formation.
threshold_slope:-0.64# Slope of the metal-dependant star formation threshold
threshold_max_density_H_p_cm3:10.0# Maximal density of the metal-dependant density threshold for star formation in Hydrogen atoms per cm^3.
# Parameters for the EAGLE "equation of state"
EAGLEEntropyFloor:
Jeans_density_threshold_H_p_cm3:1e-4# Physical density above which the EAGLE Jeans limiter entropy floor kicks in expressed in Hydrogen atoms per cm^3.
Jeans_over_density_threshold:10.# Overdensity above which the EAGLE Jeans limiter entropy floor can kick in.
Jeans_temperature_norm_K:800# Temperature of the EAGLE Jeans limiter entropy floor at the density threshold expressed in Kelvin.
Jeans_gamma_effective:1.3333333# Slope the of the EAGLE Jeans limiter entropy floor
Cool_density_threshold_H_p_cm3:1e-5# Physical density above which the EAGLE Cool limiter entropy floor kicks in expressed in Hydrogen atoms per cm^3.
Cool_over_density_threshold:10.# Overdensity above which the EAGLE Cool limiter entropy floor can kick in.
Cool_temperature_norm_K:10.# Temperature of the EAGLE Cool limiter entropy floor at the density threshold expressed in Kelvin. (NOTE: This is below the min T and hence this floor does nothing)
Cool_gamma_effective:1.# Slope the of the EAGLE Cool limiter entropy floor
# EAGLE feedback model
EAGLEFeedback:
use_SNII_feedback:1# Global switch for SNII thermal (stochastic) feedback.
use_SNIa_feedback:1# Global switch for SNIa thermal (continuous) feedback.
use_AGB_enrichment:1# Global switch for enrichement from AGB stars.
use_SNII_enrichment:1# Global switch for enrichement from SNII stars.
use_SNIa_enrichment:1# Global switch for enrichement from SNIa stars.
filename:./yieldtables/# Path to the directory containing the EAGLE yield tables.
IMF_min_mass_Msun:0.1# Minimal stellar mass considered for the Chabrier IMF in solar masses.
IMF_max_mass_Msun:100.0# Maximal stellar mass considered for the Chabrier IMF in solar masses.
SNII_min_mass_Msun:8.0# Minimal mass considered for SNII stars in solar masses.
SNII_max_mass_Msun:100.0# Maximal mass considered for SNII stars in solar masses.
SNII_sampled_delay:1# Sample the SNII lifetimes to do feedback.
SNII_delta_T_K:3.16228e7# Change in temperature to apply to the gas particle in a SNII thermal feedback event in Kelvin.
SNII_energy_erg:1.0e51# Energy of one SNII explosion in ergs.
SNII_energy_fraction_min:0.3# Minimal fraction of energy applied in a SNII feedback event.
SNII_energy_fraction_max:3.0# Maximal fraction of energy applied in a SNII feedback event.
SNII_energy_fraction_Z_0:0.0012663729# Pivot point for the metallicity dependance of the SNII energy fraction (metal mass fraction).
SNII_energy_fraction_n_0_H_p_cm3:1.4588# Pivot point for the birth density dependance of the SNII energy fraction in cm^-3.
SNII_energy_fraction_n_Z:0.8686# Power-law for the metallicity dependance of the SNII energy fraction.
SNII_energy_fraction_n_n:0.8686# Power-law for the birth density dependance of the SNII energy fraction.
SNIa_DTD:Exponential# Functional form of the SNIa delay time distribution.
SNIa_DTD_delay_Gyr:0.04# Stellar age after which SNIa start in Gyr (40 Myr corresponds to stars ~ 8 Msun).
SNIa_DTD_exp_timescale_Gyr:2.0# Time-scale of the exponential decay of the SNIa rates in Gyr.
SNIa_DTD_exp_norm_p_Msun:0.002# Normalisation of the SNIa rates in inverse solar masses.
SNIa_energy_erg:1.0e51# Energy of one SNIa explosion in ergs.
AGB_ejecta_velocity_km_p_s:10.0# Velocity of the AGB ejectas in km/s.
stellar_evolution_age_cut_Gyr:0.1# Stellar age in Gyr above which the enrichment is down-sampled.
stellar_evolution_sampling_rate:10# Number of time-steps in-between two enrichment events for a star above the age threshold.
SNII_yield_factor_Hydrogen:1.0# (Optional) Correction factor to apply to the Hydrogen yield from the SNII channel.
SNII_yield_factor_Helium:1.0# (Optional) Correction factor to apply to the Helium yield from the SNII channel.
SNII_yield_factor_Carbon:0.5# (Optional) Correction factor to apply to the Carbon yield from the SNII channel.
SNII_yield_factor_Nitrogen:1.0# (Optional) Correction factor to apply to the Nitrogen yield from the SNII channel.
SNII_yield_factor_Oxygen:1.0# (Optional) Correction factor to apply to the Oxygen yield from the SNII channel.
SNII_yield_factor_Neon:1.0# (Optional) Correction factor to apply to the Neon yield from the SNII channel.
SNII_yield_factor_Magnesium:2.0# (Optional) Correction factor to apply to the Magnesium yield from the SNII channel.
SNII_yield_factor_Silicon:1.0# (Optional) Correction factor to apply to the Silicon yield from the SNII channel.
SNII_yield_factor_Iron:0.5# (Optional) Correction factor to apply to the Iron yield from the SNII channel.
# EAGLE AGN model
EAGLEAGN:
subgrid_seed_mass_Msun:1.5e5# Black hole subgrid mass at creation time in solar masses.
multi_phase_bondi:0# Compute Bondi rates per neighbour particle?
subgrid_bondi:0# Compute Bondi rates using the subgrid extrapolation of the gas properties around the BH?
with_angmom_limiter:1# Are we applying the Rosas-Guevara et al. (2015) viscous time-scale reduction term?
viscous_alpha:1e6# Normalisation constant of the viscous time-scale in the accretion reduction term
radiative_efficiency:0.1# Fraction of the accreted mass that gets radiated.
max_eddington_fraction:1.# Maximal allowed accretion rate in units of the Eddington rate.
eddington_fraction_for_recording:0.1# Record the last time BHs reached an Eddington ratio above this threshold.
coupling_efficiency:0.15# Fraction of the radiated energy that couples to the gas in feedback events.
AGN_delta_T_K:3.16228e8# Change in temperature to apply to the gas particle in an AGN feedback event in Kelvin.
AGN_num_ngb_to_heat:1.# Target number of gas neighbours to heat in an AGN feedback event.
max_reposition_mass:2e8# Maximal BH mass considered for BH repositioning in solar masses.
max_reposition_distance_ratio:3.0# Maximal distance a BH can be repositioned, in units of the softening length.
with_reposition_velocity_threshold:1# Should we only reposition to particles that move slowly w.r.t. the black hole?
max_reposition_velocity_ratio:0.5# Maximal velocity offset of a particle to reposition a BH to, in units of the ambient sound speed of the BH. Only meaningful if with_reposition_velocity_ratio is 1.
min_reposition_velocity_threshold:-1.0# Minimal value of the velocity threshold for repositioning [km/s], set to < 0 for no effect. Only meaningful if with_reposition_velocity_ratio is 1.
set_reposition_speed:0# Should we reposition black holes with (at most) a prescribed speed towards the potential minimum?
threshold_major_merger:0.333# Mass ratio threshold to consider a BH merger as 'major'
threshold_minor_merger:0.1# Mass ratio threshold to consider a BH merger as 'minor'
merger_threshold_type:2# Type of velocity threshold for BH mergers (0: v_circ at kernel edge, 1: v_esc at actual distance, with softening, 2: v_esc at actual distance, no softening).
merger_max_distance_ratio:3.0# Maximal distance over which two BHs can merge, in units of the softening length.
#runs 3DFOF + substructure algorithm, demands subhalos and FOF halos be self-bound, calculates many properties
#Units currently set to take in as input, Mpc, 1e10 solar masses, km/s, output in same units
#To set temporally unique halo ids, alter Snapshot_value=SNAP to appropriate value. Ie: for snapshot 12, change SNAP to 12
################################
#input options
#set up to use SWIFT HDF input, load gas, star, bh and dark matter
################################
HDF_name_convention=6 #HDF SWIFT naming convention
Input_includes_dm_particle=1 #include dark matter particles in hydro input
Input_includes_gas_particle=1 #include gas particles in hydro input
Input_includes_star_particle=1 #include star particles in hydro input
Input_includes_bh_particle=1 #include bh particles in hydro input
Input_includes_wind_particle=0 #include wind particles in hydro input (used by Illustris and moves particle type 0 to particle type 3 when decoupled from hydro forces). Here shown as example
Input_includes_tracer_particle=0 #include tracer particles in hydro input (used by Illustris). Here shown as example
Input_includes_extradm_particle=0 #include extra dm particles stored in particle type 2 and type 3, useful for zooms
Halo_core_phase_merge_dist=0.25 #merge substructures if difference in dispersion normalised distance is < this value
Apply_phase_merge_to_host=1 #merge substructures with background if centrally located and phase-distance is small
#units conversion from input input to desired internal unit
Length_input_unit_conversion_to_output_unit=1.0 #default code unit,
Velocity_input_unit_conversion_to_output_unit=1.0 #default velocity unit,
Mass_input_unit_conversion_to_output_unit=1.0 #default mass unit,
#assumes input is in 1e10 msun, Mpc and km/s and output units are the same
Gravity=43.0211349 #for 1e10 Msun, km/s and Mpc
Hubble_unit=100.0 # assuming units are km/s and Mpc, then value of Hubble in km/s/Mpc
#set the units of the output by providing conversion to a defined unit
#conversion of output length units to kpc
Length_unit_to_kpc=1000.0
#conversion of output velocity units to km/s
Velocity_to_kms=1.0
#conversion of output mass units to solar masses
Mass_to_solarmass=1.0e10
#1 / 0.012
Metallicity_to_solarmetallicity=83.33
Star_formation_rate_to_solarmassperyear=97.78
Stellar_age_to_yr=1.0
#ensures that output is physical and not comoving distances per little h
Comoving_units=0
#sets the total buffer size in bytes used to store temporary particle information
#of mpi read threads before they are broadcast to the appropriate waiting non-read threads
#if not set, default value is equivalent to 1e6 particles per mpi process, quite large
#but significantly minimises the number of send/receives
#in this example the buffer size is roughly that for a send/receive of 10000 particles
#for 100 mpi processes
MPI_particle_total_buf_size=100000000
################################
#search related options
################################
#how to search a simulation
Particle_search_type=1 #search dark matter particles only
#for baryon search
Baryon_searchflag=2 #if 1 search for baryons separately using phase-space search when identifying substructures, 2 allows special treatment in field FOF linking and phase-space substructure search, 0 treat the same as dark matter particles
#for search for substruture
Search_for_substructure=1 #if 0, end search once field objects are found
#also useful for zoom simulations or simulations of individual objects, setting this flag means no field structure search is run
Singlehalo_search=0 #if file is single halo in which one wishes to search for substructure. Here disabled.
#additional option for field haloes
Keep_FOF=0 #if field 6DFOF search is done, allows to keep structures found in 3DFOF (can be interpreted as the inter halo stellar mass when only stellar search is used).\n
#minimum size for structures
Minimum_size=20 #min 20 particles
Minimum_halo_size=32 #if field halos have different minimum sizes, otherwise set to -1.
#for field fof halo search
FoF_Field_search_type=5 #5 3DFOF search for field halos, 4 for 6DFOF clean up of field halos, 3 for 6DFOF with velocity scale distinct for each initial 3D FOF candidate
Halo_3D_linking_length=0.20
#for mean field estimates and local velocity density distribution funciton estimator related quantiites, rarely need to change this
Local_velocity_density_approximate_calculation=1 #calculates velocity density using approximative (and quicker) near neighbour search
Cell_fraction = 0.01 #fraction of field fof halo used to determine mean velocity distribution function. Typical values are ~0.005-0.02
Grid_type=1 #normal entropy based grid, shouldn't have to change
Nsearch_velocity=32 #number of velocity neighbours used to calculate local velocity distribution function. Typial values are ~32
Nsearch_physical=256 #numerof physical neighbours from which the nearest velocity neighbour set is based. Typical values are 128-512
#for substructure search, rarely ever need to change this
FoF_search_type=1 #default phase-space FOF search. Don't really need to change
Iterative_searchflag=1 #iterative substructure search, for substructure find initial candidate substructures with smaller linking lengths then expand search region
Outlier_threshold=2.5 #outlier threshold for a particle to be considered residing in substructure, that is how dynamically distinct a particle is. Typical values are >2
Substructure_physical_linking_length=0.10
Velocity_ratio=2.0 #ratio of speeds used in phase-space FOF
Velocity_opening_angle=0.10 #angle between velocities. 18 degrees here, typical values are ~10-30
Velocity_linking_length=0.20 #where scaled by structure dispersion
Significance_level=1.0 #how significant a substructure is relative to Poisson noise. Values >= 1 are fine.
#for iterative substructure search, rarely ever need to change this
Iterative_threshold_factor=1.0 #change in threshold value when using iterative search. Here no increase in threshold if iterative or not
Iterative_linking_length_factor=2.0 #increase in final linking final iterative substructure search
Iterative_Vratio_factor=1.0 #change in Vratio when using iterative search. no change in vratio
Iterative_ThetaOp_factor=1.0 #change in velocity opening angle. no change in velocity opening angle
#for checking for halo merger remnants, which are defined as large, well separated phase-space density maxima
Halo_core_search=2 # searches for separate 6dfof cores in field haloes, and then more than just flags halo as merging, assigns particles to each merging "halo". 2 is full separation, 1 is flagging, 0 is off
#if searching for cores, linking lengths. likely does not need to change much
Use_adaptive_core_search=0 #calculate dispersions in configuration & vel space to determine linking lengths
Use_phase_tensor_core_growth=2 #use full stepped phase-space tensor assignment
Halo_core_ellx_fac=0.7 #how linking lengths are changed when searching for local 6DFOF cores,
Halo_core_ellv_fac=2.0 #how velocity lengths based on dispersions are changed when searching for local 6DFOF cores
Halo_core_ncellfac=0.005 #fraction of total halo particle number setting min size of a local 6DFOF core
Halo_core_num_loops=8 #number of loops to iteratively search for cores
Halo_core_loop_ellx_fac=0.75 #how much to change the configuration space linking per iteration
Halo_core_loop_ellv_fac=1.0 #how much to change the velocity space linking per iteration
Halo_core_loop_elln_fac=1.2 #how much to change the min number of particles per iteration
Halo_core_phase_significance=2.0 #how significant a core must be in terms of dispersions (sigma) significance
################################
#Unbinding options (VELOCIraptor is able to accurately identify tidal debris so particles need not be bound to a structure)
################################
#unbinding related items
Unbind_flag=1 #run unbinding
#objects must have particles that meet the allowed kinetic to potential ratio AND also have some total fraction that are completely bound.
Unbinding_type=0
#alpha factor used to determine whether particle is "bound" alaph*T+W<0. For standard subhalo catalogues use >0.9 but if interested in tidal debris 0.2-0.5
Allowed_kinetic_potential_ratio=0.95
Min_bound_mass_frac=0.65 #minimum bound mass fraction
#run unbinding of field structures, aka halos. This is useful for sams and 6DFOF halos but may not be useful if interested in 3DFOF mass functions.
Bound_halos=0
#don't keep background potential when unbinding
Keep_background_potential=1
#use all particles to determine velocity frame for unbinding
Frac_pot_ref=1.0
Min_npot_ref=20
#reference frame only meaningful if calculating velocity frame using subset of particles in object. Can use radially sorted fraction of particles about minimum potential or centre of mass
