diff --git a/examples/EAGLE_ICs/EAGLE_25_low_res/README b/examples/EAGLE_ICs/EAGLE_25_low_res/README new file mode 100644 index 0000000000000000000000000000000000000000..38e99d1fe74f30912633c7f609f20cbadcf8bee6 --- /dev/null +++ b/examples/EAGLE_ICs/EAGLE_25_low_res/README @@ -0,0 +1,8 @@ +Initial conditions corresponding to the 25 Mpc volume +of the EAGLE suite at 8x lower resolution. +The ICs only contain DM particles. The gas particles will be generated in SWIFT. + +This resolution corresponds to: EAGLE low res. (m_B = 1.45e7 Msol) + +MD5 hash: +62e7ec93a1b0b4c57ff0c63ad0da2028 EAGLE_L0025N0188_ICs.hdf5 diff --git a/examples/EAGLE_ICs/EAGLE_25_low_res/eagle_25.yml b/examples/EAGLE_ICs/EAGLE_25_low_res/eagle_25.yml new file mode 100644 index 0000000000000000000000000000000000000000..06b80444506ff17c4c645a9b59de041c723427a0 --- /dev/null +++ b/examples/EAGLE_ICs/EAGLE_25_low_res/eagle_25.yml @@ -0,0 +1,243 @@ +# Define some meta-data about the simulation +MetaData: + run_name: EAGLE-L0025N0188-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: 1.01 + scale_factor_first: 0.01 + +# 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: 128 + comoving_DM_softening: 0.006640 # Comoving softening for DM (6.67 ckpc) + max_physical_DM_softening: 0.002600 # Physical softening for DM (2.60 pkpc) + comoving_baryon_softening: 0.003580 # Comoving softening for baryons (3.58 ckpc) + max_physical_baryon_softening: 0.001400 # Physical softening for baryons (1.40 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: 5.6e-3 # (internal units, i.e. 5.6e7 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: 32 # 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: 1.0e10 # 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: 16 + cell_split_size: 200 + +Restarts: + onexit: 1 + delta_hours: 6.0 + +# Parameters related to the initial conditions +InitialConditions: + file_name: EAGLE_L0025N0188_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: + SF_model: PressureLaw + 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: 100.0 # 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: 0.5 # Minimal fraction of energy applied in a SNII feedback event. + SNII_energy_fraction_max: 5.0 # 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. + SNII_energy_fraction_use_birth_density: 0 # Are we using the density at birth to compute f_E or at feedback time? + SNII_energy_fraction_use_birth_metallicity: 0 # Are we using the metallicity at birth to compuote f_E or at feedback time? + 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: 1.0e4 # 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: 0 # 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 + with_boost_factor: 0 # Are we using the model from Booth & Schaye (2009)? + boost_alpha: 1. # Lowest value for the accretion effeciency for the Booth & Schaye 2009 accretion model. + boost_beta: 2. # Slope of the power law for the Booth & Schaye 2009 model, set beta to zero for constant alpha models. + boost_n_h_star_H_p_cm3: 0.1 # Normalization of the power law for the Booth & Schaye 2009 model in cgs (cm^-3). + radiative_efficiency: 0.1 # Fraction of the accreted mass that gets radiated. + use_nibbling: 1 # Continuously transfer small amounts of mass from all gas neighbours to a black hole [1] or stochastically swallow whole gas particles [0]? + min_gas_mass_for_nibbling: 7.2e6 # Minimum mass for a gas particle to be nibbled from [M_Sun]. Only used if use_nibbling is 1. + 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: 0.1 # Fraction of the radiated energy that couples to the gas in feedback events. + use_variable_delta_T: 1 # Switch to enable adaptive calculation of AGN dT [1], rather than using a constant value [0]. + AGN_with_locally_adaptive_delta_T: 1 # Switch to enable additional dependence of AGN dT on local gas density and temperature (only used if use_variable_delta_T is 1). + AGN_delta_T_mass_norm: 3e8 # Normalisation temperature of AGN dT scaling with BH subgrid mass [K] (only used if use_variable_delta_T is 1). + AGN_delta_T_mass_reference: 1e8 # BH subgrid mass at which the normalisation temperature set above applies [M_Sun] (only used if use_variable_delta_T is 1). + AGN_delta_T_mass_exponent: 0.666667 # Power-law index of AGN dT scaling with BH subgrid mass (only used if use_variable_delta_T is 1). + AGN_delta_T_crit_factor: 1.0 # Multiple of critical dT for numerical efficiency (Dalla Vecchia & Schaye 2012) to use as dT floor (only used if use_variable_delta_T and AGN_with_locally_adaptive_delta_T are both 1). + AGN_delta_T_background_factor: 0.0 # Multiple of local gas temperature to use as dT floor (only used if use_variable_delta_T and AGN_with_locally_adaptive_delta_T are both 1). + AGN_delta_T_min: 1e7 # Minimum allowed value of AGN dT [K] (only used if use_variable_delta_T is 1). + AGN_delta_T_max: 3e9 # Maximum allowed value of AGN dT [K] (only used if use_variable_delta_T is 1). + AGN_delta_T_K: 3.16228e8 # Change in temperature to apply to the gas particle in an AGN feedback event [K] (used if use_variable_delta_T is 0 or AGN_use_nheat_with_fixed_dT is 1 AND to initialise the BHs). + AGN_use_nheat_with_fixed_dT: 0 # Switch to use the constant AGN dT, rather than the adaptive one, for calculating the energy reservoir threshold. + AGN_use_adaptive_energy_reservoir_threshold: 0 # Switch to calculate an adaptive AGN energy reservoir threshold. + AGN_num_ngb_to_heat: 1. # Target number of gas neighbours to heat in an AGN feedback event (only used if AGN_use_adaptive_energy_reservoir_threshold is 0). + max_reposition_mass: 1e20 # Maximal BH mass considered for BH repositioning in solar masses (large number implies we always reposition). + max_reposition_distance_ratio: 3.0 # Maximal distance a BH can be repositioned, in units of the softening length. + with_reposition_velocity_threshold: 0 # 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_threshold 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_threshold 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. diff --git a/examples/EAGLE_ICs/EAGLE_25_low_res/getIC.sh b/examples/EAGLE_ICs/EAGLE_25_low_res/getIC.sh new file mode 100755 index 0000000000000000000000000000000000000000..fe3ae0d395d008b5811465da14ce38a367b19fb5 --- /dev/null +++ b/examples/EAGLE_ICs/EAGLE_25_low_res/getIC.sh @@ -0,0 +1,2 @@ +#!/bin/bash +wget http://virgodb.cosma.dur.ac.uk/swift-webstorage/ICs/EAGLE_ICs/EAGLE_L0025N0188_ICs.hdf5 diff --git a/examples/EAGLE_ICs/EAGLE_25_low_res/run.sh b/examples/EAGLE_ICs/EAGLE_25_low_res/run.sh new file mode 100755 index 0000000000000000000000000000000000000000..fa2655fe295b76960311b78cbfe0fb47bb372f41 --- /dev/null +++ b/examples/EAGLE_ICs/EAGLE_25_low_res/run.sh @@ -0,0 +1,35 @@ +#!/bin/bash + + # Generate the initial conditions if they are not present. +if [ ! -e EAGLE_L0025N0188_ICs.hdf5 ] +then + echo "Fetching initial conditions for the EAGLE 25Mpc low-res. 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_25.yml diff --git a/examples/EAGLE_ICs/EAGLE_25_low_res/vrconfig_3dfof_subhalos_SO_hydro.cfg b/examples/EAGLE_ICs/EAGLE_25_low_res/vrconfig_3dfof_subhalos_SO_hydro.cfg new file mode 100644 index 0000000000000000000000000000000000000000..2c190e870ab5e2c1af92efe7c13ec2df891aa65b --- /dev/null +++ b/examples/EAGLE_ICs/EAGLE_25_low_res/vrconfig_3dfof_subhalos_SO_hydro.cfg @@ -0,0 +1,213 @@ +#Configuration file for analysing Hydro +#runs 6DFOF + 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 + +Particle_type_for_reference_frames=1 #use DM particles to define reference frame +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=43.00918 #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 +Stellar_age_to_yr=9.778134136e11 +Stellar_age_input_unit_conversion_to_output_unit=1.022690e-12 # year in units of Mpc / (km / s) + +#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 + +Metallicity_to_solarmetallicity=83.33 #1 / 0.012 +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=5.0 #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 +#extra options in new unbinding optimisation +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 +################################ + +Number_of_overdensities=5 +Overdensity_values_in_critical_density=100,200,500,1000,2500, +#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=1 #how talkative do you want the code to be, 0 not much, 1 a lot, 2 chatterbox