Commit 92ee32bf authored by Matthieu Schaller's avatar Matthieu Schaller

Added the EAGLE 6Mpc box Initial conditions example

parent e303f7a1
Initial conditions corresponding to the 6.25 Mpc volume
of the EAGLE suite. The ICs only contain DM particles. The
gas particles will be generated in SWIFT.
Note that this is a very very small volume. It will not result
in a galaxy population matching the data averaged on large scale.
# Define some meta-data about the simulation
MetaData:
run_name: EAGLE-L0006N0094-Ref
# Define the system of units to use internally.
InternalUnitSystem:
UnitMass_in_cgs: 1.98841e43 # 10^10 M_sun in grams
UnitLength_in_cgs: 3.08567758e24 # Mpc in centimeters
UnitVelocity_in_cgs: 1e5 # km/s in centimeters per second
UnitCurrent_in_cgs: 1 # Amperes
UnitTemp_in_cgs: 1 # Kelvin
# Cosmological parameters
Cosmology:
h: 0.6777 # Reduced Hubble constant
a_begin: 0.0078125 # Initial scale-factor of the simulation
a_end: 1.0 # Final scale factor of the simulation
Omega_m: 0.307 # Matter density parameter
Omega_lambda: 0.693 # Dark-energy density parameter
Omega_b: 0.0482519 # Baryon density parameter
# Parameters governing the time integration
TimeIntegration:
dt_min: 1e-10 # The minimal time-step size of the simulation (in internal units).
dt_max: 1e-2 # The maximal time-step size of the simulation (in internal units).
# Parameters governing the snapshots
Snapshots:
basename: eagle # Common part of the name of output files
output_list_on: 1
output_list: ./output_list.txt
# Parameters governing the conserved quantities statistics
Statistics:
delta_time: 1.02
scale_factor_first: 0.05
# Parameters for the self-gravity scheme
Gravity:
eta: 0.025 # Constant dimensionless multiplier for time integration.
MAC: geometric # Use the geometric opening angle condition
theta_cr: 0.7 # Opening angle (Multipole acceptance criterion)
use_tree_below_softening: 0
mesh_side_length: 32
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.
#!/bin/bash
wget http://virgodb.cosma.dur.ac.uk/swift-webstorage/ICs/EAGLE_ICs/EAGLE_L0006N0094_ICs.hdf5
# Redshift
18.08
15.28
13.06
11.26
9.79
8.57
7.54
6.67
5.92
5.28
4.72
4.24
3.81
3.43
3.09
2.79
2.52
2.28
2.06
1.86
1.68
1.51
1.36
1.21
1.08
0.96
0.85
0.74
0.64
0.55
0.46
0.37
0.29
0.21
0.14
0.07
0.00
#!/bin/bash
# Generate the initial conditions if they are not present.
if [ ! -e EAGLE_L0006N0094_ICs.hdf5 ]
then
echo "Fetching initial conditions for the EAGLE 6Mpc example..."
./getIC.sh
fi
# Grab the cooling and yield tables if they are not present.
if [ ! -e yieldtables ]
then
echo "Fetching EAGLE yield tables..."
../getEagleYieldTable.sh
fi
if [ ! -e coolingtables ]
then
echo "Fetching EAGLE cooling tables..."
../getEagleCoolingTable.sh
fi
# The following run-time options are broken down by line as:
# Basic run-time options
# Create and run with stars
# Radiative options - run with cooling and stellar feedback
# Run with the time-step limiter required to capture feedback
# Run with black holes - fof is needed for the seeding
# Threading options - run with threads and pinning (latter not required but improves performance)
# The corresponding parameter file for this run
../../swift \
--cosmology --eagle \
--threads=16 --pin \
eagle_6.yml
#Configuration file for analysing Hydro
#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
#converting hydro quantities
Stellar_age_input_is_cosmological_scalefactor=1
Metallicity_input_unit_conversion_to_output_unit=1.0
Stellar_age_input_unit_conversion_to_output_unit=1.0
Star_formation_rate_input_unit_conversion_to_output_unit=1.0
#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
Kinetic_reference_frame_type=0
Unbinding_max_unbound_removal_fraction_per_iteration=0.5
Unbinding_max_unbound_fraction=0.95
Unbinding_max_unbound_fraction_allowed=0.005
################################
#Calculation of properties related options
################################
Virial_density=500 #user defined virial overdensity. Note that 200 rho_c, 200 rho_m and BN98 are already calculated.
#when calculating properties, for field objects calculate inclusive masses
Inclusive_halo_masses=3 #calculate inclusive masses for halos using full Spherical overdensity apertures
#ensures that output is physical and not comoving distances per little h
Comoving_units=0
#calculate more (sub)halo properties (like angular momentum in spherical overdensity apertures, both inclusive and exclusive)
Extensive_halo_properties_output=1
Extensive_gas_properties_output=1
Extensive_star_properties_output=1
#calculate aperture masses
Calculate_aperture_quantities=1
Number_of_apertures=5
Aperture_values_in_kpc=5,10,30,50,100,
Number_of_projected_apertures=5
Projected_aperture_values_in_kpc=5,10,30,50,100,
#calculate radial profiles
Calculate_radial_profiles=1
Number_of_radial_profile_bin_edges=20
#default radial normalisation log rad bins, normed by R200crit, Integer flag of 0 is log bins and R200crit norm.
Radial_profile_norm=0
Radial_profile_bin_edges=-2.,-1.87379263,-1.74758526,-1.62137789,-1.49517052,-1.36896316,-1.24275579,-1.11654842,-0.99034105,-0.86413368,-0.73792631,-0.61171894,-0.48551157,-0.3593042,-0.23309684,-0.10688947,0.0193179,0.14552527,0.27173264,0.39794001,
Iterate_cm_flag=0 #do not interate to determine centre-of-mass
Sort_by_binding_energy=1 #sort particles by binding energy
Reference_frame_for_properties=2 #use the minimum potential as reference frame about which to calculate properties
################################
#Extra fields
################################
# Also compute the H abundance as well as the HI, HII and H_2 fractions
Gas_internal_property_names=ElementMassFractions,SpeciesFractions,SpeciesFractions,SpeciesFractions,
Gas_internal_property_index_in_file=0,0,1,2,
Gas_internal_property_input_output_unit_conversion_factors=1.0,1.0,1.0,1.0
Gas_internal_property_calculation_type =averagemassweighted,averagemassweighted,averagemassweighted,averagemassweighted,
Gas_internal_property_output_units=unitless,unitless,unitless,unitless,
# Collect the BH subgrid masses and compute the max, min, average and total mass in apertures
BH_internal_property_names=SubgridMasses,SubgridMasses,SubgridMasses,SubgridMasses,
BH_internal_property_input_output_unit_conversion_factors=1.0e10,1.0e10,1.0e10,1.0e10,
BH_internal_property_calculation_type=max,min,average,aperture_total,
BH_internal_property_output_units=solar_mass,solar_mass,solar_mass,solar_mass,
################################
#output related
################################
Write_group_array_file=0 #do not write a group array file
Separate_output_files=0 #do not separate output into field and substructure files similar to subfind
Binary_output=2 #Use HDF5 output (binary output 1, ascii 0, and HDF 2)
#output particles residing in the spherical overdensity apertures of halos, only the particles exclusively belonging to halos
Spherical_overdensity_halo_particle_list_output=1
#halo ids are adjusted by this value * 1000000000000 (or 1000000 if code compiled with the LONGINTS option turned off)
#to ensure that halo ids are temporally unique. So if you had 100 snapshots, for snap 100 set this to 100 and 100*1000000000000 will
#be added to the halo id as set for this snapshot, so halo 1 becomes halo 100*1000000000000+1 and halo 1 of snap 0 would just have ID=1
#ALTER THIS as part of a script to get temporally unique ids
Snapshot_value=SNAP
################################
#other options
################################
Verbose=0 #how talkative do you want the code to be, 0 not much, 1 a lot, 2 chatterbox
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