diff --git a/examples/EAGLE_ICs/EAGLE_100/eagle_100.yml b/examples/EAGLE_ICs/EAGLE_100/eagle_100.yml
index d81764896aaed82d8562fc759658a10359af5945..44b7fe446d8d818fd8c67a70c5444e2b3ccb37a7 100644
--- a/examples/EAGLE_ICs/EAGLE_100/eagle_100.yml
+++ b/examples/EAGLE_ICs/EAGLE_100/eagle_100.yml
@@ -143,7 +143,7 @@ EAGLEStarFormation:
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_threshold_H_p_cm3: 1e8 # 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 # When using Z-based SF threshold, logarithm base 10 of the maximal entropy above the EOS at which stars can form.
threshold_norm_H_p_cm3: 0.1 # When using Z-based SF threshold, normalisation of the metal-dependant density threshold for star formation in Hydrogen atoms per cm^3.
@@ -249,3 +249,4 @@ EAGLEAGN:
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.
+ minimum_timestep_Myr: 0.1 # Minimum of the accretion-limited time-step length.
diff --git a/examples/EAGLE_ICs/EAGLE_12/eagle_12.yml b/examples/EAGLE_ICs/EAGLE_12/eagle_12.yml
index 4029cd32263e1000c2ad02a0d67432f31f9cbba6..b5bb8bdbfa17ad396362b53c790100b013ee830c 100644
--- a/examples/EAGLE_ICs/EAGLE_12/eagle_12.yml
+++ b/examples/EAGLE_ICs/EAGLE_12/eagle_12.yml
@@ -142,7 +142,7 @@ EAGLEStarFormation:
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_threshold_H_p_cm3: 1e8 # 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 # When using Z-based SF threshold, logarithm base 10 of the maximal entropy above the EOS at which stars can form.
threshold_norm_H_p_cm3: 0.1 # When using Z-based SF threshold, normalisation of the metal-dependant density threshold for star formation in Hydrogen atoms per cm^3.
@@ -248,3 +248,4 @@ EAGLEAGN:
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.
+ minimum_timestep_Myr: 0.1 # Minimum of the accretion-limited time-step length.
diff --git a/examples/EAGLE_ICs/EAGLE_25/eagle_25.yml b/examples/EAGLE_ICs/EAGLE_25/eagle_25.yml
index a52590c9d761da9d8a167e73cbc6f0a8e8a5979f..1f56b79cf8ca09e9d27fb0fd64a2ee896da306b6 100644
--- a/examples/EAGLE_ICs/EAGLE_25/eagle_25.yml
+++ b/examples/EAGLE_ICs/EAGLE_25/eagle_25.yml
@@ -142,7 +142,7 @@ EAGLEStarFormation:
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_threshold_H_p_cm3: 1e8 # 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 # When using Z-based SF threshold, logarithm base 10 of the maximal entropy above the EOS at which stars can form.
threshold_norm_H_p_cm3: 0.1 # When using Z-based SF threshold, normalisation of the metal-dependant density threshold for star formation in Hydrogen atoms per cm^3.
@@ -248,3 +248,4 @@ EAGLEAGN:
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.
+ minimum_timestep_Myr: 0.1 # Minimum of the accretion-limited time-step length.
diff --git a/examples/EAGLE_ICs/EAGLE_25_low_res/eagle_25.yml b/examples/EAGLE_ICs/EAGLE_25_low_res/eagle_25.yml
index e37450795a9847fbb1a89d0ae92220372873094a..46d02012f5d4223e41127d3741a13bd0187dc59c 100644
--- a/examples/EAGLE_ICs/EAGLE_25_low_res/eagle_25.yml
+++ b/examples/EAGLE_ICs/EAGLE_25_low_res/eagle_25.yml
@@ -139,7 +139,7 @@ EAGLEStarFormation:
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_threshold_H_p_cm3: 1e8 # 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 # When using Z-based SF threshold, logarithm base 10 of the maximal entropy above the EOS at which stars can form.
threshold_norm_H_p_cm3: 0.1 # When using Z-based SF threshold, normalisation of the metal-dependant density threshold for star formation in Hydrogen atoms per cm^3.
@@ -173,6 +173,7 @@ EAGLEFeedback:
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_feedback_model: MinimumDistance # Feedback modes: Random, Isotropic, MinimumDistance, MinimumDensity
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.
@@ -204,41 +205,44 @@ EAGLEFeedback:
# 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
- with_boost_factor: 0 # Are we using the model from Booth & Schaye (2009)?
- boost_alpha: 1. # Lowest value for the accretion effeciency for the Booth & Schaye 2009 accretion model.
- boost_beta: 2. # Slope of the power law for the Booth & Schaye 2009 model, set beta to zero for constant alpha models.
- boost_n_h_star_H_p_cm3: 0.1 # Normalization of the power law for the Booth & Schaye 2009 model in cgs (cm^-3).
- radiative_efficiency: 0.1 # Fraction of the accreted mass that gets radiated.
- 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: 7.2e6 # Minimum mass for a gas particle to be nibbled from [M_Sun]. Only used if use_nibbling is 1.
- 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.
- use_variable_delta_T: 1 # Switch to enable adaptive calculation of AGN dT [1], rather than using a constant value [0].
- AGN_with_locally_adaptive_delta_T: 1 # Switch to enable additional dependence of AGN dT on local gas density and temperature (only used if use_variable_delta_T is 1).
- AGN_delta_T_mass_norm: 3e8 # Normalisation temperature of AGN dT scaling with BH subgrid mass [K] (only used if use_variable_delta_T is 1).
- AGN_delta_T_mass_reference: 1e8 # BH subgrid mass at which the normalisation temperature set above applies [M_Sun] (only used if use_variable_delta_T is 1).
- AGN_delta_T_mass_exponent: 0.666667 # Power-law index of AGN dT scaling with BH subgrid mass (only used if use_variable_delta_T is 1).
- AGN_delta_T_crit_factor: 1.0 # Multiple of critical dT for numerical efficiency (Dalla Vecchia & Schaye 2012) to use as dT floor (only used if use_variable_delta_T and AGN_with_locally_adaptive_delta_T are both 1).
- AGN_delta_T_background_factor: 0.0 # Multiple of local gas temperature to use as dT floor (only used if use_variable_delta_T and AGN_with_locally_adaptive_delta_T are both 1).
- AGN_delta_T_min: 1e7 # Minimum allowed value of AGN dT [K] (only used if use_variable_delta_T is 1).
- AGN_delta_T_max: 3e9 # Maximum allowed value of AGN dT [K] (only used if use_variable_delta_T is 1).
- AGN_delta_T_K: 3.16228e8 # Change in temperature to apply to the gas particle in an AGN feedback event [K] (used if use_variable_delta_T is 0 or AGN_use_nheat_with_fixed_dT is 1 AND to initialise the BHs).
- AGN_use_nheat_with_fixed_dT: 0 # Switch to use the constant AGN dT, rather than the adaptive one, for calculating the energy reservoir threshold.
- AGN_use_adaptive_energy_reservoir_threshold: 0 # Switch to calculate an adaptive AGN energy reservoir threshold.
- AGN_num_ngb_to_heat: 1. # Target number of gas neighbours to heat in an AGN feedback event (only used if AGN_use_adaptive_energy_reservoir_threshold is 0).
- 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.
+ subgrid_seed_mass_Msun: 1.0e4 # Black hole subgrid mass at creation time in solar masses.
+ use_multi_phase_bondi: 0 # Compute Bondi rates per neighbour particle?
+ use_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
+ with_boost_factor: 0 # Are we using the model from Booth & Schaye (2009)?
+ boost_alpha: 1. # Lowest value for the accretion effeciency for the Booth & Schaye 2009 accretion model.
+ boost_beta: 2. # Slope of the power law for the Booth & Schaye 2009 model, set beta to zero for constant alpha models.
+ boost_n_h_star_H_p_cm3: 0.1 # Normalization of the power law for the Booth & Schaye 2009 model in cgs (cm^-3).
+ radiative_efficiency: 0.1 # Fraction of the accreted mass that gets radiated.
+ 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: 7.2e6 # Minimum mass for a gas particle to be nibbled from [M_Sun]. Only used if use_nibbling is 1.
+ 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_feedback_model: MinimumDistance # Feedback modes: Random, Isotropic, MinimumDistance, MinimumDensity
+ AGN_use_deterministic_feedback: 1 # Deterministic (reservoir) [1] or stochastic [0] AGN feedback?
+ use_variable_delta_T: 1 # Switch to enable adaptive calculation of AGN dT [1], rather than using a constant value [0].
+ AGN_with_locally_adaptive_delta_T: 1 # Switch to enable additional dependence of AGN dT on local gas density and temperature (only used if use_variable_delta_T is 1).
+ AGN_delta_T_mass_norm: 3e8 # Normalisation temperature of AGN dT scaling with BH subgrid mass [K] (only used if use_variable_delta_T is 1).
+ AGN_delta_T_mass_reference: 1e8 # BH subgrid mass at which the normalisation temperature set above applies [M_Sun] (only used if use_variable_delta_T is 1).
+ AGN_delta_T_mass_exponent: 0.666667 # Power-law index of AGN dT scaling with BH subgrid mass (only used if use_variable_delta_T is 1).
+ AGN_delta_T_crit_factor: 1.0 # Multiple of critical dT for numerical efficiency (Dalla Vecchia & Schaye 2012) to use as dT floor (only used if use_variable_delta_T and AGN_with_locally_adaptive_delta_T are both 1).
+ AGN_delta_T_background_factor: 0.0 # Multiple of local gas temperature to use as dT floor (only used if use_variable_delta_T and AGN_with_locally_adaptive_delta_T are both 1).
+ AGN_delta_T_min: 1e7 # Minimum allowed value of AGN dT [K] (only used if use_variable_delta_T is 1).
+ AGN_delta_T_max: 3e9 # Maximum allowed value of AGN dT [K] (only used if use_variable_delta_T is 1).
+ AGN_delta_T_K: 3.16228e8 # Change in temperature to apply to the gas particle in an AGN feedback event [K] (used if use_variable_delta_T is 0 or AGN_use_nheat_with_fixed_dT is 1 AND to initialise the BHs).
+ AGN_use_nheat_with_fixed_dT: 0 # Switch to use the constant AGN dT, rather than the adaptive one, for calculating the energy reservoir threshold.
+ AGN_use_adaptive_energy_reservoir_threshold: 0 # Switch to calculate an adaptive AGN energy reservoir threshold.
+ AGN_num_ngb_to_heat: 1. # Target number of gas neighbours to heat in an AGN feedback event (only used if AGN_use_adaptive_energy_reservoir_threshold is 0).
+ 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.
+ minimum_timestep_Myr: 0.1 # Minimum of the accretion-limited time-step length.
diff --git a/examples/EAGLE_ICs/EAGLE_50/eagle_50.yml b/examples/EAGLE_ICs/EAGLE_50/eagle_50.yml
index b7ec98015f93782e315c8ba3d0d7c53f721ccf75..78d7d341e49e4bcce0666c93568cc2329039de1f 100644
--- a/examples/EAGLE_ICs/EAGLE_50/eagle_50.yml
+++ b/examples/EAGLE_ICs/EAGLE_50/eagle_50.yml
@@ -140,7 +140,7 @@ EAGLEStarFormation:
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_threshold_H_p_cm3: 1e8 # 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 # When using Z-based SF threshold, logarithm base 10 of the maximal entropy above the EOS at which stars can form.
threshold_norm_H_p_cm3: 0.1 # When using Z-based SF threshold, normalisation of the metal-dependant density threshold for star formation in Hydrogen atoms per cm^3.
@@ -246,3 +246,4 @@ EAGLEAGN:
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.
+ minimum_timestep_Myr: 0.1 # Minimum of the accretion-limited time-step length.
diff --git a/examples/EAGLE_ICs/EAGLE_50_low_res/eagle_50.yml b/examples/EAGLE_ICs/EAGLE_50_low_res/eagle_50.yml
index f91f7aabe9f92f0c5392897171ecd427ae41f7d4..7ce351f8ea527cd0c8692631822119ce29016e3a 100644
--- a/examples/EAGLE_ICs/EAGLE_50_low_res/eagle_50.yml
+++ b/examples/EAGLE_ICs/EAGLE_50_low_res/eagle_50.yml
@@ -139,7 +139,7 @@ EAGLEStarFormation:
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_threshold_H_p_cm3: 1e8 # 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 # When using Z-based SF threshold, logarithm base 10 of the maximal entropy above the EOS at which stars can form.
threshold_norm_H_p_cm3: 0.1 # When using Z-based SF threshold, normalisation of the metal-dependant density threshold for star formation in Hydrogen atoms per cm^3.
@@ -216,7 +216,7 @@ EAGLEAGN:
boost_n_h_star_H_p_cm3: 0.1 # Normalization of the power law for the Booth & Schaye 2009 model in cgs (cm^-3).
radiative_efficiency: 0.1 # Fraction of the accreted mass that gets radiated.
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: 9e5 # Minimum mass for a gas particle to be nibbled from [M_Sun]. Only used if use_nibbling is 1.
+ min_gas_mass_for_nibbling: 7.2e6 # Minimum mass for a gas particle to be nibbled from [M_Sun]. Only used if use_nibbling is 1.
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.
@@ -245,3 +245,4 @@ EAGLEAGN:
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.
+ minimum_timestep_Myr: 0.1 # Minimum of the accretion-limited time-step length.
diff --git a/examples/EAGLE_ICs/EAGLE_6/eagle_6.yml b/examples/EAGLE_ICs/EAGLE_6/eagle_6.yml
index 00b68c896d4cf503d2dc61b850fde06e6b87bdb7..86bdbd40d3021c469968f25fa6f7f8e8c5dbe892 100644
--- a/examples/EAGLE_ICs/EAGLE_6/eagle_6.yml
+++ b/examples/EAGLE_ICs/EAGLE_6/eagle_6.yml
@@ -142,7 +142,7 @@ EAGLEStarFormation:
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_threshold_H_p_cm3: 1e8 # 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 # When using Z-based SF threshold, logarithm base 10 of the maximal entropy above the EOS at which stars can form.
threshold_norm_H_p_cm3: 0.1 # When using Z-based SF threshold, normalisation of the metal-dependant density threshold for star formation in Hydrogen atoms per cm^3.
@@ -248,3 +248,4 @@ EAGLEAGN:
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.
+ minimum_timestep_Myr: 0.1 # Minimum of the accretion-limited time-step length.
diff --git a/examples/EAGLE_ICs/README b/examples/EAGLE_ICs/README
index 77a900d7a8c1a09e9dda4509bc77cae146dfb6ad..1d12e9422aa0c2ef1073399ea114ac84a3be0cd1 100644
--- a/examples/EAGLE_ICs/README
+++ b/examples/EAGLE_ICs/README
@@ -45,6 +45,10 @@ the following changes have been made (at standard resolution):
at least 100 (was 57.7).
- Particles with a density above 10^5 cm^-3 are not turned into
stars instantaneously any more.
+ - The normalisation of the SF law at high densities has been corrected
+ from the original code where the break in slope of the K-S law
+ also led to a jump. This change of slope is not used anymore (was
+ a K-S slope of 2 at volume particle densities > 10^3 cm^-3).
- The minimal mass of SNII stars has been raised to 8 Msun (from 6).
- The SNII feedback heats the particle closest to the star particle
(was a random set of particles in the kernel).
@@ -78,6 +82,8 @@ the following changes have been made (at standard resolution):
- The angular momentum term in the BH accretion model of
Rosas-Guevara et al. (2015) is now switched off.
- The coupling efficency of the BH feedback is now 0.1 (was 0.15).
+ - The BHs compute a time-step length based on their accretion rate
+ with a minimum time-step length of 10^5 years.
- The AGN feedback heats the particles closest to the BH particle
(was a random set of particles in the kernel).
- The AGN does not use a combination of probability and reservoir