# Define the system of units to use internally. InternalUnitSystem: UnitMass_in_cgs: 1.9891E43 # 10^10 solar masses UnitLength_in_cgs: 3.08567758E21 # 1 kpc UnitVelocity_in_cgs: 1E5 # km/s UnitCurrent_in_cgs: 1 # Amperes UnitTemp_in_cgs: 1 # Kelvin # 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 max_physical_baryon_softening: 0.2 # Maximal Plummer-equivalent softening length in physical coordinates for baryon particles (in internal units). # Parameters governing the time integration (Set dt_min and dt_max to the same value for a fixed time-step run.) TimeIntegration: time_begin: 0. # The starting time of the simulation (in internal units). time_end: 0.5115 # The end time of the simulation (in internal units). dt_min: 1e-9 # 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: output # Common part of the name of output files time_first: 0. # (Optional) Time of the first output if non-cosmological time-integration (in internal units) delta_time: 0.01023 # Time difference between consecutive outputs (in internal units) 0.01023 TU = 10 Myr compression: 4 # Compress the snapshots recording_triggers_part: [-1, -1] # Not recording as we have many snapshots recording_triggers_bpart: [-1, -1] # Not recording as we have many snapshots # Parameters governing the conserved quantities statistics Statistics: delta_time: 1e-2 # Time between statistics output time_first: 0. # (Optional) Time of the first stats output if non-cosmological time-integration (in internal units) # Parameters related to the initial conditions InitialConditions: file_name: M5_disk.hdf5 # The file to read periodic: 0 # Are we running with periodic ICs? stars_smoothing_length: 0.5 # Parameters for the hydrodynamics scheme SPH: minimal_temperature: 10. # Minimum allowed gas temperature resolution_eta: 1.2348 # Target smoothing length in units of the mean inter-particle separation (1.2348 == 48Ngbs with the cubic spline kernel). CFL_condition: 0.2 # Courant-Friedrich-Levy condition for time integration. h_min_ratio: 1e-8 # Minimal smoothing in units of softening. h_max: 10. H_mass_fraction: 0.756 # 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 rad_field_norm_factor: 0.01 # Multiplicative factor to scale ISRF init_abundance_mode: read # Flag to specify how to set initial CHIMES abundances colibre_metal_depletion: 0 # 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: 1 # 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: 1 # 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_files # Path to COLIBRE cooling tables colibre_table_filebase: cooling_rates # Filebase of COLIBRE cooling tables split in redshift 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) 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 max_dust_boost_factor: 100.0 # Max boost factor applied to all reactions on dust grains dust_boost_nH_min_cgs: 1.0 # Density below which the dust boost factor is equal to unity, in units of cm^-3 dust_boost_nH_max_cgs: 100.0 # Density below which the dust boost factor is equal to unity, in units of cm^-3 # Solar abundances COLIBREChemistry: init_abundance_metal: 0.0133714 # Initial fraction of particle mass in *all* metal init_abundance_Hydrogen: 0.73738788833 # Initial fraction of particle mass in Hydrogen init_abundance_Helium: 0.24924186942 # Initial fraction of particle mass in Helium init_abundance_Carbon: 0.0023647215 # Initial fraction of particle mass in Carbon init_abundance_Nitrogen: 0.0006928991 # Initial fraction of particle mass in Nitrogen init_abundance_Oxygen: 0.00573271036 # Initial fraction of particle mass in Oxygen init_abundance_Neon: 0.00125649278 # Initial fraction of particle mass in Neon init_abundance_Magnesium: 0.00070797838 # Initial fraction of particle mass in Magnesium init_abundance_Silicon: 0.00066495154 # Initial fraction of particle mass in Silicon init_abundance_Iron: 0.00129199252 # Initial fraction of particle mass in Iron init_abundance_Europium: 0.0 # Initial 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_molecule_subscript_oxygen: 4.0 # subscript for oxygen in the effective silicate molecule e.g. FeMgSi2O6 (default 6) silicate_molecule_subscript_magnesium: 1.3 # subscript for magnesium in the effective silicate molecule e.g. FeMgSi2O6 (default 1) silicate_molecule_subscript_silicon: 1.0 # subscript for silicon in the effective silicate molecule e.g. FeMgSi2O6 (default 2) silicate_molecule_subscript_iron: 0.7 # subscript for iron in the effective silicate molecule e.g. FeMgSi2O6 (default 1) limit_depletion: 1 # whether to limit the depleted fraction of metals into dust grains to prevent complete depletion of elements undepleted_min_reduction_factor: 0.423345 # The diffuse element limit, represented by a reduction factor to the default saturated diffuse fractions, and chosen to maintain a realistic resevoir of diffuse CO (Fuente et al 2019) initial_abundance_graphite: 0.0 # Initial abundance of graphite dust initial_abundance_silicate: 0.0 # Initial abundance of silicate dust initial_abundance_depletedC: 0.00238524088 # M16 dust only: Initial abundance of dust-phase carbon (default 0.) initial_abundance_depletedO: 0.00116190453 # M16 dust only: Initial abundance of dust-phase oxygen (default 0.) initial_abundance_depletedMg: 0.00059817947 # M16 dust only: Initial abundance of dust-phase magnesiun (default 0.) initial_abundance_depletedSi: 0.00058274810 # M16 dust only: Initial abundance of dust-phase silicon (default 0.) initial_abundance_depletedFe: 0.00127192702 # M16 dust only: Initial abundance of dust-phase iron (default 0.) # COLIBRE star formation model (Following a density Schmidt law with virial criterion) 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 Stars: birth_time: -1 # (Optional) Initial birth times of *all* the stars to be used if we are overwriting them. (-1 means the stars remain inactive feedback-wise througout the run). overwrite_birth_time: 0 # (Optional) Do we want to overwrite the birth time of the stars read from the ICs? (default: 0). 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 # 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 # Switch for early feedback (Radiation pressure). with_HIIRegions: 1 # Switch for early feedback (HII regions). with_StellarWinds: 1 # Switch for early feedback (Stellar winds). 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: 0.25 # 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: 2.5e51 # 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: 0.0134 # 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: 0.25 # 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_enrichment_min_mass_Msun: 8.0 # Minimal mass considered for SNII enrichment (not SNII feedback!) in solar masses. SNII_enrichment_max_mass_Msun: 40.0 # Minimal mass considered for SNII enrichment (not SNII feedback!) in solar masses. SNII_yield_factor_Hydrogen: 1.0 # Correction factor to apply to the Hydrogen yield from the SNII channel. SNII_yield_factor_Helium: 1.0 # Correction factor to apply to the Helium yield from the SNII channel. SNII_yield_factor_Carbon: 3.0 # Correction factor to apply to the Carbon yield from the SNII channel. SNII_yield_factor_Nitrogen: 0.8 # Correction factor to apply to the Nitrogen yield from the SNII channel. SNII_yield_factor_Oxygen: 1.0 # Correction factor to apply to the Oxygen yield from the SNII channel. SNII_yield_factor_Neon: 1.0 # Correction factor to apply to the Neon yield from the SNII channel. SNII_yield_factor_Magnesium: 1.0 # Correction factor to apply to the Magnesium yield from the SNII channel. SNII_yield_factor_Silicon: 0.8 # Correction factor to apply to the Silicon yield from the SNII channel. SNII_yield_factor_Iron: 2.0 # Correction factor to apply to the Iron yield from the SNII channel. 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: 40.0 # Maximal mass considered for r-process enrichment from collapsars in solar masses. 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. # Hernquist potential parameters HernquistPotential: useabspos: 0 # 0 -> positions based on centre, 1 -> absolute positions position: [0.,0.,0.] # Location of centre of isothermal potential with respect to centre of the box (if 0) otherwise absolute (if 1) (internal units) idealizeddisk: 1 # Run with an idealized galaxy disk M200: 137.0 # M200 of the galaxy disk h: 0.704 # reduced Hubble constant (value does not specify the used units!) concentration: 9.0 # concentration of the Halo diskfraction: 0.040 # Disk mass fraction bulgefraction: 0.0 # Bulge mass fraction timestep_mult: 0.01 # Dimensionless pre-factor for the time-step condition, basically determines the fraction of the orbital time we use to do the time integration epsilon: 0.2 # Softening size (internal units) # 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: 0.002 # 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: 10 delta_time_SNII_Myr: 1 delta_time_r_processes_Myr: 10 # COLIBRE AGN model COLIBREAGN: subgrid_seed_mass_Msun: 1e4 # 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: 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. 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: 5e4 # Minimum mass for a gas particle to be nibbled from [M_Sun]. Only used if use_nibbling is 1. coupling_efficiency: 0.10 # 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. 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: 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: 1.0 # 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: Isotropic # AGN feedback model (Isotropic or MinimumDistance) minimum_timestep_yr: 10000.0 # Minimum time-step of black-hole particles with_boost_factor: 1 # 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). XrayEmissivity: xray_table_path: ./X_Ray_tables.hdf5 # Path to the X-ray emissivity tables