eagle_25.yml

MetaData:
  run_name:   EAGLE-L0025N0376-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

# Structure finding options
StructureFinding:
  config_file_name:     stf_input.cfg    # Name of the STF config file.
  basename:             ./stf         # Common part of the name of output files.
  scale_factor_first:   0.92          # Scale-factor of the first snaphot (cosmological run)
  time_first:           0.01        # Time of the first structure finding output (in internal units).
  delta_time:           1.10          # Time difference between consecutive structure finding outputs (in internal units) in simulation time intervals.

# Cosmological parameters
Cosmology:
  h:              0.6777        # Reduced Hubble constant
  a_begin:        0.9090909     # 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

Scheduler:
  links_per_tasks: 500

# Parameters governing the time integration
TimeIntegration:
  time_begin: 0.    # The starting time of the simulation (in internal units).
  time_end:   1e-2  # The end time of the simulation (in internal units).
  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
  scale_factor_first:  0.91  # Scale-factor of the first snaphot (cosmological run)
  time_first:          0.01  # Time of the first output (non-cosmological run) (in internal units)
  delta_time:          1.01  # Time difference between consecutive outputs (in internal units)

# Parameters governing the conserved quantities statistics
Statistics:
  scale_factor_first:  0.92 # Scale-factor of the first stat dump (cosmological run)
  time_first:          0.01 # Time of the first stat dump (non-cosmological run) (in internal units)
  delta_time:          1.05 # Time between statistics output

# Parameters for the self-gravity scheme
Gravity:
  eta:                      0.025    # Constant dimensionless multiplier for time integration.
  MAC:                      geometric
  theta_cr:                 0.7      # Opening angle (Multipole acceptance criterion)
  use_tree_below_softening: 1
  mesh_side_length:         64
  comoving_DM_softening:         0.0026994 # Comoving DM softening length (in internal units).
  max_physical_DM_softening:     0.0007    # Max physical DM softening length (in internal units).
  comoving_baryon_softening:     0.0026994 # Comoving DM softening length (in internal units).
  max_physical_baryon_softening: 0.0007    # Max physical DM softening length (in internal units).


# 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              # (internal units)
  particle_splitting:    1
  particle_splitting_mass_threshold: 7e-4 # Internal units (i.e. 7e6 Msun ~ 4 times the initial gas 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
  overwrite_birth_time:  1
  birth_time:            0.33333  # Pretend all the stars were born at z = 2

# 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:  1.5e10      # Minimal halo mass in which to seed a black hole (in solar masses).
  scale_factor_first:              0.91        # Scale-factor of first FoF black hole seeding calls.
  delta_time:                      1.005       # Scale-factor ratio between consecutive FoF black hole seeding calls.

# Parameters related to the initial conditions
InitialConditions:
  file_name:  ./EAGLE_ICs_25.hdf5    # The file to read
  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

EAGLEChemistry: 	     # Solar abundances
  init_abundance_metal:      0.014
  init_abundance_Hydrogen:   0.70649785
  init_abundance_Helium:     0.28055534
  init_abundance_Carbon:     2.0665436e-3
  init_abundance_Nitrogen:   8.3562563e-4
  init_abundance_Oxygen:     5.4926244e-3
  init_abundance_Neon:       1.4144605e-3
  init_abundance_Magnesium:  5.907064e-4
  init_abundance_Silicon:    6.825874e-4
  init_abundance_Iron:       1.1032152e-3
  
# EAGLE cooling parameters
EAGLECooling:
  dir_name:                ./coolingtables/
  H_reion_z:               11.5 
  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
  H_reion_z:               11.5
  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
  delta_logTEOS_subgrid_properties: 0.3
  rapid_cooling_threshold:          0.333333

# 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:                  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_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: 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
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 stars in solar masses.
  SNII_max_mass_Msun:             100.0             # Maximal mass considered for SNII stars in solar masses.
  SNII_sampled_delay:               0               # Sample the SNII lifetimes to do feedback.
  SNII_wind_delay_Gyr:              0.03            # Time in Gyr between a star's birth and the SNII thermal feedback event when not sampling.
  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             # Minimal fraction of energy applied in a SNII feedback event.
  SNII_energy_fraction_max:         3.0             # 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:                         PowerLaw        # 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_power_law_norm_p_Msun:   0.0012          # Normalization of the SNIa delay time distribution (in Msun^-1).
  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:             1.5e5      # Black hole subgrid mass at creation time in solar masses.
  multi_phase_bondi:                  0          # Compute Bondi rates per neighbour particle?
  with_angmom_limiter:                1          # 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:                0.15       # 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:                2e8        # 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: 1          # 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_ratio 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_ratio 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.
  use_subgrid_mass_from_ics:          0          # Use the dynamical mass as the subgrid mass since we don't have subgrid masses in the ICs.