# Define some meta-data about the simulation MetaData: run_name: COLIBRE-GCs-L006N0094 # 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 # 1 km/s UnitCurrent_in_cgs: 1 # Amperes UnitTemp_in_cgs: 1 # Kelvin # 3x2pt + all external constraints cosmology Cosmology: Omega_cdm: 0.256011 Omega_b: 0.048600 Omega_lambda: 0.693922 h: 0.681 a_begin: 0.0078125 # z = 127.0 a_end: 1.0000000000 N_ur: 2.0308 N_nu: 1 T_nu_0: 1.9517578050 M_nu_eV: 0.06 deg_nu: 1.0 # Parameters governing the time integration TimeIntegration: dt_min: 1e-10 dt_max: 1e-2 # Parameters for the self-gravity scheme Gravity: eta: 0.025 # Constant dimensionless multiplier for time integration. MAC: adaptive # Use the adaptive opening angle condition theta_cr: 0.7 # Opening angle (Multipole acceptance criterion) epsilon_fmm: 0.001 # Adaptive opening angle precision mesh_side_length: 64 # use 128 for 188^3 particles and 256 for 376^3 particles comoving_DM_softening: 0.003320 # New EAGLE-Ref values: 0.003320 # Comoving softening for DM (3.32 ckpc); scale with resolution max_physical_DM_softening: 0.001300 # New EAGLE-Ref values: 0.001300 # Physical softening for DM (1.30 pkpc); scale with resolution comoving_baryon_softening: 0.001790 # New EAGLE-Ref values: 0.001790 # Comoving softening for baryons (1.79 ckpc); scale with resolution max_physical_baryon_softening: 0.000700 # New EAGLE-Ref values: 0.000700 # Physical softening for baryons (0.70 pkpc); scale with resolution # Parameters governing the snapshots Snapshots: basename: colibre output_list_on: 1 output_list: ./output_list.txt compression: 4 invoke_fof: 1 # Run FOF before saving particle outputs. use_delta_from_edge: 1 # Lossy compression demands we shift things a tiny bit to avoid out-of-box rounding. delta_from_edge: 1e-6 # (Internal units) We shift by 1pc. recording_triggers_part: [1.0227e-4, 1.0227e-5] # Recording starts 100M and 10M years before a snapshot recording_triggers_bpart: [1.0227e-4, 1.0227e-5] # Recording starts 100M and 10M years before a snapshot # Line-of-sight parameters LineOfSight: basename: los scale_factor_first: 0.1 delta_time: 1.01 time_first: 0. output_list_on: 0 num_along_x: 35 num_along_y: 35 num_along_z: 35 # Parameters governing the conserved quantities statistics Statistics: delta_time: 1.01 scale_factor_first: 0.01 Scheduler: max_top_level_cells: 8 # use 8 for 188^3, 16 for 376^3, 32 for 752^3 particles cell_split_size: 200 # should be fine for most systems, could use 50 for older system such as cosma5 and cosma6 engine_max_parts_per_cooling: 200 # Better value for CHIMES: split the tasks as finely as possible # Parameters related to the initial conditions InitialConditions: file_name: Eagle_06Mpc_094.hdf5 periodic: 1 cleanup_h_factors: 1 cleanup_velocity_factors: 1 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 # Remap the IDs to the range [1, N] # Parameters of the hydro scheme SPH: H_mass_fraction: 0.756 # overwrites the default H mass fraction (updated since EAGLE) resolution_eta: 1.2348 # "48 Ngb" with the cubic spline kernel h_min_ratio: 1e-8 CFL_condition: 0.2 initial_temperature: 268.7 minimal_temperature: 10. h_max: 0.5 # Maximal smoothing length in co-moving internal units. particle_splitting: 1 # Particle splitting is ON particle_splitting_mass_threshold: 7.2e-4 # (internal units, i.e. 7.2e6 Msun ~ 4x initial gas particle mass) # Standard COLIBRE cooling options COLIBRECooling: dir_name: ./cooling_files # Location of the cooling tables filebase_cool: UVB_dust1_CR1_G1_shield1_v1 H_reion_z: 7.5 # Redshift of Hydrogen re-ionization 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. # CHIMES cooling parameters CHIMESCooling: data_path: ./chimes-data # Path to chimes-data repository EqmAbundanceTable: colibre_HHe # Path to equilibrium abundance tables PhotoIonTable_UVB: SP20_cross_sections # Path to cross-sections tables; UVB PhotoIonTable_ISRF: cross_sections_B87.hdf5 # Path to cross-sections tables; ISRF UV_field: COLIBRE # Flag specifying radiation field model Shielding_model: COLIBRE # Flag specifying local shielding model UVB_z_dependence: COLIBRE # Flag to switch on redshift-dependent UVB shielding_length_factor: 0.5 # Multiplicative factor to scale shielding length max_shielding_length_kpc: 100.0 # Max shielding length in kpc rad_field_norm_factor: 1.0 # Multiplicative factor to scale ISRF init_abundance_mode: read # Flag to specify how to set initial CHIMES abundances colibre_metal_depletion: 1 # Flag to specify metal depletion model turbulent_velocity_dispersion_km_p_s: 6.0 # 1D velocity dispersion, in km/s. colibre_use_turbulent_jeans_length: 1 # Integer flag, 0 - use only thermal Jeans length, 1 - use maximum of thermal or turbulent Jeans length. colibre_saturate_radiation_field: 0 # Integer flag, 0 - no max rad field, 1 - impose max rad field. colibre_col_dens_saturate_rad: 1.3e22 # Column density at which the Colibre rad field saturates, in cm^-2. colibre_saturate_cr_rate: 0 # Integer flag, 0 - no max CR rate, 1 - impose max CR rate. colibre_col_dens_saturate_cr: 3.63e20 # Column density at which the CR rate saturates, in cm^-2. colibre_cr_plaw_index: 1.0 # Power law index of the scaling between CR rate and column density. relativeTolerance: 1e-3 # Relative tolerance for CHIMES intergration absoluteTolerance: 1e-10 # Absolute tolerance for CHIMES chemistry integration explicitTolerance: 0.1 # Tolerance below which we use the explicit solution in CHIMES scale_metal_tolerances: 1 # Flag to scale absolute tolerances by element abundance Tmol_K: 1.0e5 # Maximum temperature for the molecular network ChemistryEqmMode: 0 # Flag to use pre-computed equilibrium abundances throughout ThermEvolOn: 1 # Flag to switch on thermal evolution in CHIMES chimes_debug: 0 # Flag to include extra debug outputs in CHIMES cosmic_ray_rate_cgs: 1.8e-16 # HI ionisation rate from cosmic rays in units of HI per second. delta_logTEOS_subgrid_properties: 0.3 # delta logT above the EOS below which set CHIMES to eqm and use subgrid properties use_colibre_subgrid_EOS: 1 # Flag to set subgrid rho and T to thermal and pressure eqm on the EOS set_FB_particles_to_eqm: 1 # Flag to set particles to eqm if they have been heated by feedback destroy_FB_heated_dust: 1 # Destroy dust in the cooling step if particle directly heated, representing supernova destruction use_hybrid_cooling: 1 # Use hybrid cooling, to read in eqm cooling rates from metals not included in CHIMES rapid_cooling_threshold: 0.333333 # Threshold in dt / t_cool to switch between rapid- and slow-cooling modes colibre_table_path: ./cooling_rates # Path to COLIBRE cooling tables (Ploeckinger & Schaye 2020) colibre_table_filebase: cooling_rates # Filebase of COLIBRE cooling tables split in redshift (Ploeckinger & Schaye 2020) UVB_cutoff_z: 127.0 # Redshift above which the UVB is switched off ISRF_low_dens_cutoff_z: 7.5 # Redshift above which the ISRF is cut off at low densities (UV_field_flag == 2 only) ISRF_low_dens_cutoff_cJprime: -8. # Parameter that controls the position of the low density cutoff (Ploeckinger & Schaye 2020, eq.15) ISRF_low_dens_cutoff_kJprime: -3. # Parameter that controls the steepness of the low density cutoff (Ploeckinger & Schaye 2020, eq.15) ISRF_low_dens_cutoff_logJmin: -20. # Parameter that sets the minimum radiation field for the cutoff (Ploeckinger & Schaye 2020, eq.15) S_over_Si_in_solar: 1.0 # S / Si relative to Solar Ca_over_Si_in_solar: 1.0 # Ca / Si relative to Solar IncludeCarbon: 0 # Include Carbon in the CHIMES network IncludeNitrogen: 0 # Include Nitrogen in the CHIMES network IncludeOxygen: 0 # Include Oxygen in the CHIMES network IncludeNeon: 0 # Include Neon in the CHIMES network IncludeMagnesium: 0 # Include Magnesium in the CHIMES network IncludeSilicon: 0 # Include Silicon in the CHIMES network IncludeSulphur: 0 # Include Sulphur in the CHIMES network IncludeCalcium: 0 # Include Calcium in the CHIMES network IncludeIron: 0 # Include Iron in the CHIMES network # Solar abundances COLIBREChemistry: init_abundance_metal: 0.0 # Inital fraction of particle mass in *all* metals init_abundance_Hydrogen: 0.756 # Inital fraction of particle mass in Hydrogen init_abundance_Helium: 0.244 # Inital fraction of particle mass in Helium init_abundance_Carbon: 0.0 # Inital fraction of particle mass in Carbon init_abundance_Nitrogen: 0.0 # Inital fraction of particle mass in Nitrogen init_abundance_Oxygen: 0.0 # Inital fraction of particle mass in Oxygen init_abundance_Neon: 0.0 # Inital fraction of particle mass in Neon init_abundance_Magnesium: 0.0 # Inital fraction of particle mass in Magnesium init_abundance_Silicon: 0.0 # Inital fraction of particle mass in Silicon init_abundance_Iron: 0.0 # Inital fraction of particle mass in Iron init_abundance_Europium: 0.0 # Inital fraction of particle mass in Europium init_abundance_Strontium: 0.0 # Inital fraction of particle mass in Strontium init_abundance_Barium: 0.0 # Inital fraction of particle mass in Barium metal_diffusion_constant: 0.01 # Metal diffusion constant (Smagorinsky constant) metal_diffusion_timestep_mult: 0.2 # Run-time parameter to control the time-step condition based on the diffusion rate. # Parameters of the dust model DustEvolution: pair_to_cooling: 1 # Whether to override implicit dust depletion in cooling with the modelled dust depletion (default 0) clumping_factor_mode chimes_synced # clumping factor mode: 'constant' (single clumping factor), 'variable' (density dependent clumping) or 'chimes_synced (follow CHIMES dust boost)' use_subgrid_props: 1 # Whether to use subgrid density/temperature or hydro (default 1) use_sputtering: 1 # Include destructive effects of sputtering on dust grains (default 1) use_SNII_destruction: 0 # Include destructive effects of SNII on dust grains (default 0) use_accretion: 1 # Include grain growth by accretion of metals (default 1) clumping_factor: 30. # Boost factor applied to accretion rate (default 1.) diffusion_boost_factor: 1. # Boost factor applied to diffusion rate for dust (default 1.) dust_yields_path: ./dust_yields # T20 dust only: Path to where AGB dust yield tables are locatedv (default ./dust_yields) silicate_fe_grain_fraction: 0.5 # T20 dust only: value X controls forsterite/fayalite grain mix (giving effective grain of Fe_2XMg_(2X-2)MgSiO_4) initial_abundance_graphite: 0.0 # T20 dust only: Initial abundance of graphite dust initial_abundance_silicate: 0.0 # T20 dust only: Initial abundance of silicate dust initial_abundance_depletedC: 0.0 # M16 dust only: Initial abundance of dust-phase carbon initial_abundance_depletedO: 0.0 # M16 dust only: Initial abundance of dust-phase oxygen initial_abundance_depletedMg: 0.0 # M16 dust only: Initial abundance of dust-phase magnesiun initial_abundance_depletedSi: 0.0 # M16 dust only: Initial abundance of dust-phase silicon initial_abundance_depletedFe: 0.0 # M16 dust only: Initial abundance of dust-phase iron # COLIBRE star formation model (Following a density Schmidt law) COLIBREStarFormation: min_over_density: 100.0 # Minimum over density above which star formation is allowed alpha_virial: 1. # set the alpha virial for star forming gas. SF_model: SchmidtLaw # star formation model to use (SchmidtLaw or PressureLaw) star_formation_efficiency: 0.01 # Star formation efficiency (SFE) of the Schmidt law, \rho_\star = SFE * \rho / t_ff KS_exponent: 1.4 # Kennicutt-Schmidt slope for the pressure law. KS_normalisation_Msun_p_yr_p_kpc2: 1.515e-4 # Normalization of the Kennicutt-Schmidt slope for the pressure law. gas_fraction: 1.0 # (Optional) gas fraction for pressure law, default to 1.0 # COLIBRE feedback model COLIBREFeedback: 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 enrichment from AGB stars. use_SNII_enrichment: 1 # Global switch for enrichment from SNII stars. use_SNIa_enrichment: 1 # Global switch for enrichment from SNIa stars. with_r_process_enrichment: 1 # Global switch for r process enrichment from neutron star mergers and rare core-collapse SN (collapsars and common envelop jets SN). with_RadiationPressure: 1 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 feedback (not SNII enrichment!) in solar masses. SNII_max_mass_Msun: 100.0 # Maximal mass considered for SNII feedback (not SNII enrichment!) in solar masses. SNII_wind_delay_Gyr: -1.0 # Time in Gyr between a star's birth and the SNII thermal feedback event. (< 0. for continuous SNe) SNII_delay_thermal_feedback_Gyr: 0.02 # Time in Gyr between a star's birth and the earliest possible SNII thermal feedback event. If SNe occur at earlier times, these events are postponed. SNII_delta_T_n_0_H_p_cm3: 0.3 # Pivot (physical) density in SNII variable-dT thermal feedback in H/cm3. SNII_delta_T_K_pivot: 3.16228e6 # Pivot temperature in SNII variable-dT thermal feedback in Kelvin. SNII_delta_T_slope: 0.666666666 # Slope in SNII variable-dT thermal feedback. SNII_delta_T_K_min: 3.16228e6 # Minimal change in temperature to apply to the gas particle in an SNII thermal feedback event in Kelvin. SNII_delta_T_K_max: 1e8 # Maximal change in temperature to apply to the gas particle in na SNII thermal feedback event in Kelvin. SNII_energy_erg: 1.0e51 # Energy of one SNII explosion in ergs. SNII_delta_v_km_p_s: 50.0 # Change in the gas-particle velocity that is kicked in a SNII kinetic feedback event SNII_f_kinetic: 0.1 # Fraction of SNII energy injected into the gas in kinetic form (the remaining fraction is injected in thermal form) SNII_energy_fraction_min: 0.1 # Minimal fraction of energy applied in a SNII feedback event. SNII_energy_fraction_max: 3.5 # Maximal fraction of energy applied in a SNII feedback event. SNII_energy_fraction_Z_0: 0.012663729 # Pivot point for the metallicity dependance of the SNII energy fraction (metal mass fraction). SNII_energy_fraction_n_0_H_p_cm3: 0.67 # Pivot point for the birth density dependance of the SNII energy fraction in cm^-3. SNII_energy_fraction_P_0_K_p_cm3: 3.16228e3 # Pivot point for the birth pressure dependance of the SNII energy fraction in cm^-3. SNII_energy_fraction_n_Z: 0.0 # Power-law for the metallicity dependance of the SNII energy fraction. SNII_energy_fraction_n_n: 0.0 # Power-law for the birth density dependance of the SNII energy fraction. SNII_energy_fraction_sigma_P: 0.3 # Width of the birth pressure dependance of the SNII energy fraction (relates to the power-law as n_P = -1/(sigma_P * ln(10))). SNIa_energy_erg: 1.0e51 # Energy of one SNIa explosion in ergs. SNIa_delta_T_n_0_H_p_cm3: 0.3 # Pivot (physical) density in SNIa variable-dT thermal feedback in H/cm3. SNIa_delta_T_K_pivot: 3.16228e6 # Pivot temperature in SNIa variable-dT thermal feedback in Kelvin. SNIa_delta_T_slope: 0.666666666 # Slope in SNIa variable-dT thermal feedback. SNIa_delta_T_K_min: 3.16228e6 # Minimal change in temperature to apply to the gas particle in an SNIa thermal feedback event in Kelvin. SNIa_delta_T_K_max: 1e8 # Maximal change in temperature to apply to the gas particle in na SNIa thermal feedback event in Kelvin. SNIa_energy_fraction: 1.0 # Fraction of energy applied in a SNIa feedback event. AGB_ejecta_velocity_km_p_s: 10.0 # Velocity of the AGB ejectas in km/s. 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: 1.5 # (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: 1.5 # (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: 1.0 # (Optional) Correction factor to apply to the Iron yield from the SNII channel. with_HIIRegions: 1 # Switch for early feedback (HII regions). with_StellarWinds: 1 # Switch for early feedback (Stellar winds). Momentum_desired_delta_v: 50.0 # Desired kick in km/s (Done stochastically given the amount of momentum available - v<0 for the code to decide the kick - ) HIIregion_ionization_fraction: 1.0 # Ionization fraction for gas particles tagged as HII regions (between 0.5 and 1.) HIIregion_temperature_K: 1.e4 # Temperature of gas particles tagged as HII regions HIIregion_rebuild_dt_Myr: 2.0 # Time between rebuilding the HII region in Myr earlyfb_filename: ./Early_stellar_feedback.hdf5 # Location of file for early feedback, no needed if stellarwind_maxage_Myr = HIIregion_maxage_Myr = 0. stellar_evolution_age_cut_Gyr: 0.1 # Stellar age in Gyr above which the enrichment is down-sampled. stellar_evolution_sampling_age_fraction: 0.05 # Time-step of the stars in units of the star's current age when the star is older than the age cut. num_of_NSM_per_Msun: 1.3e-5 # Number of neutron star mergers per Msolar. yield_Eu_from_NSM_event_Msun: 1e-5 # Amount of europium (in units of Msolar) released by NSM. num_of_CEJSN_per_Msun: 1.22e-5 # Number of rare core-collapse SN (CEJSN) per Msolar. yield_Eu_from_CEJSN_event_Msun: 2e-5 # Amount of europium (in units of Msolar) released by CEJSN(=Common envelop jet SN). num_of_collapsar_per_Msun: 2.6e-5 # Number of rare core-collapse SN (collapsars) per Msolar. yield_Eu_from_collapsar_event_Msun: 1e-6 # Amount of europium (in units of Msolar) released by collapsars. collapsar_min_mass_Msun: 10.0 # Minimal mass considered for r-process enrichment from collapsars in solar masses. collapsar_max_mass_Msun: 100.0 # Maximal mass considered for r-process enrichment from collapsars in solar masses. # Parameters for the COLIBRE "equation of state" COLIBREEntropyFloor: Jeans_density_norm_H_p_cm3: 0.1 # Physical density above which the COLIBRE Jeans limiter entropy floor kicks in expressed in Hydrogen atoms per cm^3. Jeans_temperature_norm_K: 10. # Temperature of the COLIBRE Jeans limiter entropy floor at the density normalisation expressed in Kelvin. Jeans_gamma_effective: 1.0 # Slope the of the COLIBRE Jeans limiter entropy floor Cool_density_norm_H_p_cm3: 1e-5 # Physical density above which the COLIBRE Cool limiter entropy floor kicks in expressed in Hydrogen atoms per cm^3. Cool_temperature_norm_K: -1. # Temperature of the COLIBRE Cool limiter entropy floor at the density normalisation expressed in Kelvin. Cool_gamma_effective: 1. # Slope the of the COLIBRE Cool limiter entropy floor # The SNIa DTD properties in the COLIBRE feedback SNIaDTD: SNIa_efficiency_p_Msun: 0.0016 # Normalisation of the SNIa rates in inverse solar masses, used when there is only one functional form in the DTD. SNIa_timescale_Gyr: 2. # Time-scale of the SNIa delay time distribution SNIa_delay_time_Gyr: 0.04 # Delay time before the DTD kicks in. Event_logger: delta_time_SNIa_Myr: 100 delta_time_SNII_Myr: 10 delta_time_r_processes_Myr: 100 # COLIBRE AGN model COLIBREAGN: subgrid_seed_mass_Msun: 1e3 # Black hole subgrid mass at creation time in solar masses. use_multi_phase_bondi: 0 # Compute Bondi rates per neighbour particle [1] or for the smoothed ambient gas around the black hole [0]? use_subgrid_gas_properties: 1 # Use subgrid density [1] or dynamical density [0] to calculate BH accretion rates? use_krumholz: 1 # Use Krumholz et al. (2006) [1] or standard Bondi-Hoyle-Lyttleton formula [0] for black hole accretion rates? Only used if multi_phase_bondi is 0. with_krumholz_vorticity: 1 # Include the vorticity term in Krumholz et al. formula? Only used if use_multi_phase_bondi is 0. with_angmom_limiter: 0 # Are we applying the Rosas-Guevara (2015) viscous time-scale reduction term? radiative_efficiency: 0.1 # Fraction of the accreted mass that gets radiated. max_eddington_fraction: 100.0 # 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. 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_Msun: 8e5 # Minimum mass for a gas particle to be nibbled from [M_Sun]. Only used if use_nibbling is 1. coupling_efficiency: 0.05 # Fraction of the radiated energy that couples to the gas in feedback events. AGN_delta_T_K: 1e9 # 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. with_potential_correction: 1 # Subtract BH's own contribution to the potential of neighbours when determining repositioning targets. max_reposition_mass_Msun: 2e20 # 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: 0 # Should we only reposition to particles that move slowly w.r.t. the black hole? 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: DynamicalEscapeVelocity # Type of velocity threshold for BH mergers (CircularVelocity as in EAGLE, EscapeVelocity, or DynamicalEscapeVelocity) merger_max_distance_ratio: 3.0 # Maximal distance over which two BHs can merge, in units of the softening length. AGN_use_deterministic_feedback: 1 # Deterministic (1) or stochastic (0) AGN feedback model AGN_feedback_model: MinimumDistance # AGN feedback model (Isotropic or MinimumDistance) minimum_timestep_yr: 1000.0 # Minimum time-step of black-hole particles with_boost_factor: 0 # Are we using the model from Booth, Schaye (2009)? boost_alpha: 0.2 # Lowest value for the accretion effeciency for the Booth, Schaye 2009 accretion model. boost_beta: 1. # Slope of the power law for the Booth, Schaye 2009 model, set beta to zero for constant alpha models. boost_n_h_star_cm3: 1e10 # Normalization of the power law for the Booth Schaye 2009 model in cgs (cm^-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. seed_black_holes_enabled: 1 # Enable seeding of black holes in FoF groups black_hole_seed_halo_mass_Msun: 1e10 # 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. linking_types: [0, 1, 0, 0, 0, 0, 0] # Use DM as the primary FOF linking type attaching_types: [1, 0, 0, 0, 1, 1, 0] # Use gas, stars and black holes as FOF attachable types # 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 timestep_age_threshold_unlimited_Myr: 40 # Stars don't employ a stellar property related time-step when they are > 40Myr old. max_timestep_young_Myr: 1. # Stars below an age of 40Myr use a time-step length of 1Myr at most. luminosity_filename: ./photometry # MOSAICS GC model parameters. Number of models set in configuration (--with-mosaics-multiphys) fixed_CFE: [-1.] # Value of fixed cluster formation efficiency, otherwise locally varying (when fixed_CFE <= 0). One value for each MOSAICS_MULTIPHYS model. power_law_clMF: [0] # Use a power-law or Schechter mass function? One value for each MOSAICS_MULTIPHYS model. fixed_Mcstar: [0.] # Value of fixed Schechter mass function truncation. One value for each MOSAICS_MULTIPHYS model. clMF_slope: [2.] # Cluster mass function power-law index M^(-alpha). One value for each MOSAICS_MULTIPHYS model. 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 XrayEmissivity: xray_table_path: ./X_Ray_tables.hdf5 # Path to the X-ray emissivity tables PowerSpectrum: grid_side_length: 256 # size of the grid used in power spectrum calculation (default: 256) num_folds: 5 # Number of foldings (1 means no foldings), determines the max k fold_factor: 4 # factor by which to reduce the box along each side each folding (default: 4) window_order: 3 # order of the mass assignment scheme (default: 3, TSC) requested_spectra: ["matter-matter","cdm-cdm","starBH-starBH","gas-matter","pressure-pressure","matter-pressure", "cdm-gas", "gas-gas", "cdm-starBH", "gas-starBH"] output_list_on: 1 output_list: ./output_list_ps.txt