From ee7a8c8b4adf6a8fc2d4284af792a89436ea6660 Mon Sep 17 00:00:00 2001
From: Matthieu Schaller <schaller@strw.leidenuniv.nl>
Date: Tue, 26 Jul 2022 10:53:09 +0200
Subject: [PATCH] Add the M_200=10^15 idealised cluster of Husko+2022 to the
examples
---
.../IdealisedCluster_M15/getIC.sh | 13 +
.../idealised_cluster_M15.yml | 231 ++++++++++++++++++
.../IdealisedCluster_M15/run.sh | 27 ++
examples/IdealisedCluster/README | 5 +-
4 files changed, 275 insertions(+), 1 deletion(-)
create mode 100755 examples/IdealisedCluster/IdealisedCluster_M15/getIC.sh
create mode 100644 examples/IdealisedCluster/IdealisedCluster_M15/idealised_cluster_M15.yml
create mode 100755 examples/IdealisedCluster/IdealisedCluster_M15/run.sh
diff --git a/examples/IdealisedCluster/IdealisedCluster_M15/getIC.sh b/examples/IdealisedCluster/IdealisedCluster_M15/getIC.sh
new file mode 100755
index 0000000000..ec17bb5aa7
--- /dev/null
+++ b/examples/IdealisedCluster/IdealisedCluster_M15/getIC.sh
@@ -0,0 +1,13 @@
+#!/bin/bash
+
+# fiducial IC (T_0 = 10^7 K)
+wget http://virgodb.cosma.dur.ac.uk/swift-webstorage/ICs/IdealisedCluster/M5_H15_fid.hdf5
+
+# Different central temperatures (T_0)
+#wget http://virgodb.cosma.dur.ac.uk/swift-webstorage/ICs/IdealisedCluster/M5_H15_Tmin725.hdf5
+#wget http://virgodb.cosma.dur.ac.uk/swift-webstorage/ICs/IdealisedCluster/M5_H15_Tmin75.hdf5
+#wget http://virgodb.cosma.dur.ac.uk/swift-webstorage/ICs/IdealisedCluster/M5_H15_Tmin80.hdf5
+
+# Fiducial IC at different resolutions
+#wget http://virgodb.cosma.dur.ac.uk/swift-webstorage/ICs/IdealisedCluster/M5_H15_lowres8.hdf5
+#wget http://virgodb.cosma.dur.ac.uk/swift-webstorage/ICs/IdealisedCluster/M5_H15_lowres512.hdf5
diff --git a/examples/IdealisedCluster/IdealisedCluster_M15/idealised_cluster_M15.yml b/examples/IdealisedCluster/IdealisedCluster_M15/idealised_cluster_M15.yml
new file mode 100644
index 0000000000..cb36183ef4
--- /dev/null
+++ b/examples/IdealisedCluster/IdealisedCluster_M15/idealised_cluster_M15.yml
@@ -0,0 +1,231 @@
+# Define some meta-data about the simulation
+MetaData:
+ run_name: Idealised-Cluster-M15-fid
+
+# Define the system of units to use internally.
+InternalUnitSystem:
+ UnitMass_in_cgs: 1.98841e43 # 10^10 M_sun in grams
+ UnitLength_in_cgs: 3.08567758e21 # kpc in centimeters
+ UnitVelocity_in_cgs: 1e5 # km/s in centimeters per second
+ UnitCurrent_in_cgs: 1 # Amperes
+ UnitTemp_in_cgs: 1 # Kelvin
+
+# 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: 8.184 # The end time of the simulation 8 Gyr (in internal units).
+ dt_min: 1e-16 # 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: cluster # 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
+
+# Parameters governing the conserved quantities statistics
+Statistics:
+ delta_time: 1.01
+ scale_factor_first: 0.01
+
+# 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: 1.2 # Maximal Plummer-equivalent softening length in physical coordinates for baryon particles (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: 0.01 # Minimal smoothing length in units of softening.
+ h_max: 800. # 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)
+ particle_splitting: 1 # Particle splitting is ON
+ particle_splitting_mass_threshold: 3e-3 # (internal units, i.e. 7e6 Msun ~ 4x initial gas particle mass)
+ H_mass_fraction: 0.756
+
+# 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
+ luminosity_filename: ./photometry
+ birth_time: -9.207 # (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).
+
+Scheduler:
+ max_top_level_cells: 16
+ 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: M15_fiducial.hdf5 # The file to read
+ periodic: 0 # Are we running with periodic ICs?
+ stars_smoothing_length: 0.5
+
+# NFW potential parameters
+NFWPotential:
+ useabspos: 0 # 0 -> positions based on centre, 1 -> absolute positions
+ position: [0.0,0.0,0.0] # Location of centre of the NFW potential with respect to centre of the box (internal units) if useabspos=0 otherwise with respect to the 0,0,0, coordinates.
+ concentration: 5.6 # Concentration of the halo
+ M_200: 10000.0 # Mass of the halo (M_200 in internal units)
+ h: 0.704 # Critical density (internal units).
+ timestep_mult: 0.01 # Dimensionless pre-factor for the time-step condition, basically determines fraction of orbital time we need to do an integration step
+ bulgefraction: 0.0025 # Bulge mass fraction
+ epsilon: 1.2 # Softening of the NFW potential
+
+
+# Impose primoridal metallicity
+EAGLEChemistry:
+ init_abundance_metal: 0.004457 # Inital fraction of particle mass in *all* metals
+ init_abundance_Hydrogen: 0.749796 # Inital fraction of particle mass in Hydrogen
+ init_abundance_Helium: 0.245747 # Inital fraction of particle mass in Helium
+ init_abundance_Carbon: 0.000788 # Inital fraction of particle mass in Carbon
+ init_abundance_Nitrogen: 0.000231 # Inital fraction of particle mass in Nitrogen
+ init_abundance_Oxygen: 0.001911 # Inital fraction of particle mass in Oxygen
+ init_abundance_Neon: 0.000419 # Inital fraction of particle mass in Neon
+ init_abundance_Magnesium: 0.000236 # Inital fraction of particle mass in Magnesium
+ init_abundance_Silicon: 0.000222 # Inital fraction of particle mass in Silicon
+ init_abundance_Iron: 0.000431 # Inital fraction of particle mass in Iron
+
+# 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:
+ SF_threshold: Subgrid # Zdep (Schaye 2004) or Subgrid
+ SF_model: PressureLaw # PressureLaw (Schaye et al. 2008) or SchmidtLaw
+ 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: 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.
+ threshold_Z0: 0.002 # When using Z-based SF threshold, reference metallicity (metal mass fraction) for the metal-dependant threshold for star formation.
+ threshold_slope: -0.64 # When using Z-based SF threshold, slope of the metal-dependant star formation threshold
+ threshold_max_density_H_p_cm3: 10.0 # When using Z-based SF threshold, maximal density of the metal-dependant density threshold for star formation in Hydrogen atoms per cm^3.
+ threshold_temperature1_K: 1000 # When using subgrid-based SF threshold, subgrid temperature below which gas is star-forming.
+ threshold_temperature2_K: 31622 # When using subgrid-based SF threshold, subgrid temperature below which gas is star-forming if also above the density limit.
+ threshold_number_density_H_p_cm3: 10 # When using subgrid-based SF threshold, subgrid number density above which gas is star-forming if also below the second temperature limit.
+
+# 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_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.
+ SNII_energy_fraction_function: Independent # Type of functional form to use for scaling the energy fraction with density and metallicity ('EAGLE', 'Separable', or 'Independent').
+ SNII_energy_fraction_min: 0.5 # 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_delta_E_n: 6.0 # Maximal energy increase due to high density (only used if SNII_energy_fraction_function is 'Independent').
+ 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.
+ SNII_energy_fraction_use_birth_density: 0 # Are we using the density at birth to compute f_E or at feedback time?
+ SNII_energy_fraction_use_birth_metallicity: 0 # Are we using the metallicity at birth to compuote f_E or at feedback time?
+ 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.
+ 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_only: 0 # If using the boost factor, are we using a constant boost only?
+ 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).
+ with_fixed_T_near_EoS: 0 # Are we using a fixed temperature to compute the sound-speed of gas on the entropy floor in the Bondy-Hoyle accretion term?
+ fixed_T_above_EoS_dex: 0.3 # Distance above the entropy floor for which we use a fixed sound-speed
+ fixed_T_near_EoS_K: 8000 # Fixed temperature assumed to compute the sound-speed of gas on the entropy floor in the Bondy-Hoyle accretion term
+ 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_Msun: 4e6 # 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?
+ with_potential_correction: 1 # Should the BH's own contribution to the potential be removed from the neighbour's potentials when looking for repositioning targets.
+ 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: DynamicalEscapeVelocity # Type of velocity threshold for BH mergers ('CircularVelocity', 'EscapeVelocity', 'DynamicalEscapeVelocity').
+ 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/IdealisedCluster/IdealisedCluster_M15/run.sh b/examples/IdealisedCluster/IdealisedCluster_M15/run.sh
new file mode 100755
index 0000000000..c791af80b0
--- /dev/null
+++ b/examples/IdealisedCluster/IdealisedCluster_M15/run.sh
@@ -0,0 +1,27 @@
+#!/bin/bash
+
+if [ ! -e M15_fiducial.hdf5 ]
+then
+ echo "Fetching initial conditions for the idealised cluster example..."
+ ./getIC.sh
+fi
+
+if [ ! -e UV_dust1_CR1_G1_shield1.hdf5 ]
+then
+ echo "Fetching PS20 cooling tables for the isolated galaxy example..."
+ ../getPS20CoolingTables.sh
+fi
+
+if [ ! -e yieldtables ]
+then
+ echo "Fetching EAGLE stellar yield tables for the isolated galaxy example..."
+ ../getYieldTable.sh
+fi
+
+if [ ! -e photometry ]
+then
+ echo "Fetching EAGLE photometry tables..."
+ ../getEaglePhotometryTable.sh
+fi
+
+../../../swift --threads=16 --feedback --external-gravity --self-gravity --stars --star-formation --cooling --temperature --hydro --limiter --sync --black-holes idealised_cluster_M15.yml 2>&1 | tee output.log
diff --git a/examples/IdealisedCluster/README b/examples/IdealisedCluster/README
index aba53aaec4..18689194da 100644
--- a/examples/IdealisedCluster/README
+++ b/examples/IdealisedCluster/README
@@ -8,7 +8,10 @@ for the three different halo masse used in Nobels et al. (2022).
The fiducial ICs for the 10^13 Msun and 10^14 Msun idealised cluster
contain resolution variations for 5 different resolutions. For each
halo mass the central temperature variations discussed in the paper
-are provided.
+are provided.
+The 10^15 Msun halo of the same series introduced by Husko et
+al. (2022) https://arxiv.org/abs/2206.06402 is also available at
+different resolution and different central temperatures.
The code should be configured using a NFW profile and the desired subgrid
models:
--
GitLab