# Define some meta-data about the simulation MetaData: run_name: EAGLE-L0012N0188-Ref # Define the system of units to use internally. InternalUnitSystem: UnitMass_in_cgs: 1.98841e43 # 10^10 M_sun in grams UnitLength_in_cgs: 3.08567758e24 # Mpc in centimeters UnitVelocity_in_cgs: 1e5 # km/s in centimeters per second UnitCurrent_in_cgs: 1 # Amperes UnitTemp_in_cgs: 1 # Kelvin # Cosmological parameters Cosmology: h: 0.6777 # Reduced Hubble constant a_begin: 0.0078125 # Initial scale-factor of the simulation a_end: 1.0 # Final scale factor of the simulation Omega_m: 0.307 # Matter density parameter Omega_lambda: 0.693 # Dark-energy density parameter Omega_b: 0.0482519 # Baryon density parameter # Parameters governing the time integration TimeIntegration: dt_min: 1e-10 # The minimal time-step size of the simulation (in internal units). dt_max: 1e-2 # The maximal time-step size of the simulation (in internal units). # Parameters governing the snapshots Snapshots: basename: eagle # Common part of the name of output files output_list_on: 1 output_list: ./output_list.txt # Parameters governing the conserved quantities statistics Statistics: delta_time: 1.02 scale_factor_first: 0.05 # Parameters for the self-gravity scheme Gravity: eta: 0.025 # Constant dimensionless multiplier for time integration. MAC: geometric # Use the geometric opening angle condition theta_cr: 0.7 # Opening angle (Multipole acceptance criterion) use_tree_below_softening: 0 mesh_side_length: 64 comoving_DM_softening: 0.003320 # Comoving softening for DM (3.32 ckpc) max_physical_DM_softening: 0.001300 # Physical softening for DM (1.30 pkpc) comoving_baryon_softening: 0.001790 # Comoving softening for baryons (1.79 ckpc) max_physical_baryon_softening: 0.000700 # Physical softening for baryons (0.70 pkpc) # Parameters for the hydrodynamics scheme SPH: resolution_eta: 1.2348 # Target smoothing length in units of the mean inter-particle separation (1.2348 == 48Ngbs with the cubic spline kernel). h_min_ratio: 0.1 # Minimal smoothing length in units of softening. h_max: 0.5 # Maximal smoothing length in co-moving internal units. CFL_condition: 0.2 # Courant-Friedrich-Levy condition for time integration. minimal_temperature: 100.0 # (internal units) initial_temperature: 268.7 # (internal units) particle_splitting: 1 # Particle splitting is ON particle_splitting_mass_threshold: 7e-4 # (internal units, i.e. 7e6 Msun ~ 4x initial gas particle mass) # Parameters of the stars neighbour search Stars: resolution_eta: 1.1642 # Target smoothing length in units of the mean inter-particle separation h_tolerance: 7e-3 # Parameters for the Friends-Of-Friends algorithm FOF: basename: fof_output # Filename for the FOF outputs. min_group_size: 256 # The minimum no. of particles required for a group. linking_length_ratio: 0.2 # Linking length in units of the main inter-particle separation. black_hole_seed_halo_mass_Msun: 1.0e10 # 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: 8 cell_split_size: 200 Restarts: onexit: 1 delta_hours: 6.0 max_run_time: 71.5 # Three days minus fergie time resubmit_on_exit: 1 resubmit_command: ./resub.sh # Parameters related to the initial conditions InitialConditions: file_name: EAGLE_L0012N0188_ICs.hdf5 periodic: 1 cleanup_h_factors: 1 # Remove the h-factors inherited from Gadget cleanup_velocity_factors: 1 # Remove the sqrt(a) factor in the velocities inherited from Gadget generate_gas_in_ics: 1 # Generate gas particles from the DM-only ICs cleanup_smoothing_lengths: 1 # Since we generate gas, make use of the (expensive) cleaning-up procedure. remap_ids: 1 # Re-map the IDs to [1, N] to avoid collision problems when splitting # Parameters of the line-of-sight outputs LineOfSight: basename: eagle_los num_along_x: 0 num_along_y: 0 num_along_z: 100 scale_factor_first: 0.1 delta_time: 1.1 # Impose primoridal metallicity EAGLEChemistry: init_abundance_metal: 0. init_abundance_Hydrogen: 0.752 init_abundance_Helium: 0.248 init_abundance_Carbon: 0.0 init_abundance_Nitrogen: 0.0 init_abundance_Oxygen: 0.0 init_abundance_Neon: 0.0 init_abundance_Magnesium: 0.0 init_abundance_Silicon: 0.0 init_abundance_Iron: 0.0 # EAGLE cooling parameters EAGLECooling: dir_name: ./coolingtables/ H_reion_z: 7.5 # Planck 2018 H_reion_eV_p_H: 2.0 He_reion_z_centre: 3.5 He_reion_z_sigma: 0.5 He_reion_eV_p_H: 2.0 # COLIBRE cooling parameters COLIBRECooling: dir_name: ./UV_dust1_CR1_G1_shield1.hdf5 # Location of the cooling tables H_reion_z: 7.5 # Redshift of Hydrogen re-ionization (Planck 2018) H_reion_eV_p_H: 2.0 He_reion_z_centre: 3.5 # Redshift of the centre of the Helium re-ionization Gaussian He_reion_z_sigma: 0.5 # Spread in redshift of the Helium re-ionization Gaussian He_reion_eV_p_H: 2.0 # Energy inject by Helium re-ionization in electron-volt per Hydrogen atom delta_logTEOS_subgrid_properties: 0.3 # delta log T above the EOS below which the subgrid properties use Teq assumption rapid_cooling_threshold: 0.333333 # Switch to rapid cooling regime for dt / t_cool above this threshold. # EAGLE star formation parameters EAGLEStarFormation: EOS_density_norm_H_p_cm3: 0.1 # Physical density used for the normalisation of the EOS assumed for the star-forming gas in Hydrogen atoms per cm^3. EOS_temperature_norm_K: 8000 # Temperature om the polytropic EOS assumed for star-forming gas at the density normalisation in Kelvin. EOS_gamma_effective: 1.3333333 # Slope the of the polytropic EOS assumed for the star-forming gas. KS_normalisation: 1.515e-4 # The normalization of the Kennicutt-Schmidt law in Msun / kpc^2 / yr. KS_exponent: 1.4 # The exponent of the Kennicutt-Schmidt law. min_over_density: 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. 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 radiative_efficiency: 0.1 # Fraction of the accreted mass that gets radiated. max_eddington_fraction: 1. # Maximal allowed accretion rate in units of the Eddington rate. eddington_fraction_for_recording: 0.1 # Record the last time BHs reached an Eddington ratio above this threshold. coupling_efficiency: 0.1 # Fraction of the radiated energy that couples to the gas in feedback events. AGN_delta_T_K: 3.16228e8 # Change in temperature to apply to the gas particle in an AGN feedback event in Kelvin. AGN_num_ngb_to_heat: 1. # Target number of gas neighbours to heat in an AGN feedback event. max_reposition_mass: 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.