# Define the system of units to use internally. InternalUnitSystem: UnitMass_in_cgs: 1.98848e43 # 10^10 M_sun in grams UnitLength_in_cgs: 3.08567758e21 # 1 kpc in cm UnitVelocity_in_cgs: 1e5 # 1 km/s in cm/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. theta: 0.7 # Opening angle (Multipole acceptance criterion). max_physical_baryon_softening: 0.8 # 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: 0.1 # The end time of the simulation (in internal units). dt_min: 1e-14 # 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: 0.001 # Time difference between consecutive outputs (in internal units) # 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: lowres64.hdf5 # The file to read periodic: 0 # Are we running with periodic ICs? stars_smoothing_length: 0.5 # 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). CFL_condition: 0.1 # Courant-Friedrich-Levy condition for time integration. h_min_ratio: 0.1 # Minimal smoothing in units of softening. h_max: 10. minimal_temperature: 100. # Standard EAGLE cooling options EAGLECooling: dir_name: ./coolingtables/ # Location of the Wiersma+08 cooling tables H_reion_z: 11.5 # Redshift of Hydrogen re-ionization H_reion_eV_p_H: 2.0 # Energy inject by Hydrogen re-ionization in electron-volt per Hydrogen atom 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 # Use solar abundances EAGLEChemistry: init_abundance_metal: 0.0129 init_abundance_Hydrogen: 0.7065 init_abundance_Helium: 0.2806 init_abundance_Carbon: 0.00207 init_abundance_Nitrogen: 0.000836 init_abundance_Oxygen: 0.00549 init_abundance_Neon: 0.00141 init_abundance_Magnesium: 0.000591 init_abundance_Silicon: 0.000683 init_abundance_Iron: 0.0011 # 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: 0.014 # 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: 0.1 # Softening size (internal units) # 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. gas_fraction: 0.3 # The gas fraction used internally by the model. 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_temperature_margin_dex: 0.5 # Logarithm base 10 of the maximal temperature difference above the EOS allowed to form stars. 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: 0.1 # 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: 8000 # 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: 8000 # Temperature of the EAGLE Cool limiter entropy floor at the density threshold expressed in Kelvin. Cool_gamma_effective: 1. # Slope the of the EAGLE Cool limiter entropy floor # EAGLE feedback model with constant feedback energy fraction 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: 6.0 # 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: 0.03 # Time in Gyr between a star's birth and the SNII thermal feedback event. 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: 1.0 # Minimal fraction of energy applied in a SNII feedback event. SNII_energy_fraction_max: 1.0 # 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: 0.67 # 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_max_mass_Msun: 8.0 # Maximal mass considered for SNIa feedback and enrichment in solar masses. SNIa_timescale_Gyr: 2.0 # Time-scale of the exponential decay of the SNIa rates in Gyr. SNIa_efficiency_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. 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. # 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: 0 # Global switch for enrichement from AGB stars. use_SNII_enrichment: 0 # Global switch for enrichement from SNII stars. use_SNIa_enrichment: 0 # 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: 6.0 # 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: 0.03 # Time in Gyr between a star's birth and the SNII thermal feedback event. 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 # Maximal fraction of energy applied in a SNII feedback event. SNII_energy_fraction_max: 3.0 # Minimal 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: 0.67 # 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_max_mass_Msun: 8.0 # Maximal mass considered for SNIa feedback and enrichment in solar masses. SNIa_energy_erg: 1.0e51 # Energy of one SNIa explosion in ergs. SNIa_delta_T_K: 3.16228e7 # Change in temperature to apply to the gas particle in a 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: 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. Momentum_per_StellarMass: 1.8e40 # Momentum per unit stellar mass available from Starburst 99 g cm s^-1 Msun^-1 Momentum_time_scale: 6.5 # Momentum timescale in Myr Momentum_desired_delta_v: -1.0 # Desired kick in km/s (Done stochastically given the amount of momentum available - v<0 for the code to decide the kick - ) Momentum_Metallicity_norm: 0.01 # Metallicity (mass fraction). Momentum_Metallicity_exponent: 0.38 # Exponent of the relation with metallicty delta_time_feedback_logger_Myr: 10.0 HIIregion_maxage_Myr: 30. # Maximum age in Myr of star particle to build HII region HIIregion_rebuild_dt_Myr: 2.0 # Time between rebuilding the HII region in Myr earlyfb_filename: ./Early_stellar_feedback.hdf5 with_HIIRegions: 0 # Switch for early feedback (HII regions). with_StellarWinds: 0 # Switch for early feedback (Stellar winds). with_RadiationPressure: 0 # Switch for early feedback (Radiation pressure). # 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: 2.0 # Exponential delay time for exponential DTD normalization_timescale_Gyr: 13.6 # Normalization time for DTDs that cannot be integrated to infinity #power_law_slope: 1.1 # Power law slope for the power law DTD SNIa_delay_time_Gyr: 0.04 # Delay time before the DTD kicks in. # Solar abundances COLIBREChemistry: init_abundance_metal: 0.0133714 # Inital fraction of particle mass in *all* metals init_abundance_Hydrogen: 0.73738788833 # Inital fraction of particle mass in Hydrogen init_abundance_Helium: 0.24924186942 # Inital fraction of particle mass in Helium init_abundance_Carbon: 0.0023647215 # Inital fraction of particle mass in Carbon init_abundance_Nitrogen: 0.0006928991 # Inital fraction of particle mass in Nitrogen init_abundance_Oxygen: 0.00573271036 # Inital fraction of particle mass in Oxygen init_abundance_Neon: 0.00125649278 # Inital fraction of particle mass in Neon init_abundance_Magnesium: 0.00070797838 # Inital fraction of particle mass in Magnesium init_abundance_Silicon: 0.00066495154 # Inital fraction of particle mass in Silicon init_abundance_Iron: 0.00129199252 # Inital fraction of particle mass in Iron 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. Stars: birth_time: -0.1 # (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: 1 # (Optional) Do we want to overwrite the birth time of the stars read from the ICs? (default: 0). COLIBRECooling: dir_name: UV_dust1_CR1_G1_shield1.hdf5 # Location of the cooling tables H_reion_z: 11.5 # 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 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 delta_logTEOS_subgrid_properties: 0.2 # delta log T above the EOS below which the subgrid properties use Teq assumption rapid_cooling_threshold: 1.0 # Switch to rapid cooling regime for dt / t_cool above this threshold. # COLIBRE star formation model (Following a density Schmidt law) COLIBREStarFormation: min_over_density: 57.7 # Minimum over density above which star formation is allowed star_formation_efficiency: 0.01 # Star formation efficiency (SFE) of the Schmidt law, \rho_\star = SFE * \rho / t_ff temperature_threshold_K: 1000 # (Optional) Temperature threshold below which stars are allowed to form (Default set to infinity). density_direct_H_p_cm3: 1e5 # (Optional) Density above which a gas particle gets automatically turned into a star in Hydrogen atoms per cm^3 (Default set to infinity). EOS_temperature_margin_dex: 0.2 # (Optional) Logarithm base 10 of the maximal temperature difference above the EOS allowed to form stars. Default set to 10 (almost infinity) Event_logger: delta_time_SNII_Myr: 1. delta_time_SNIa_Myr: 10. delta_time_r_processes_Myr: 20.