diff --git a/examples/EAGLE_ICs/EAGLE_100/README b/examples/EAGLE_ICs/EAGLE_100/README
new file mode 100644
index 0000000000000000000000000000000000000000..580ca383b36be99a704f627a3da5dacc151152fb
--- /dev/null
+++ b/examples/EAGLE_ICs/EAGLE_100/README
@@ -0,0 +1,3 @@
+Initial conditions corresponding to the 100 Mpc volume
+of the EAGLE suite. The ICs only contain DM particles. The
+gas particles will be generated in SWIFT.
diff --git a/examples/EAGLE_ICs/EAGLE_100/eagle_100.yml b/examples/EAGLE_ICs/EAGLE_100/eagle_100.yml
new file mode 100644
index 0000000000000000000000000000000000000000..8210ff68199d4d67b1985add14f266cc602fe319
--- /dev/null
+++ b/examples/EAGLE_ICs/EAGLE_100/eagle_100.yml
@@ -0,0 +1,192 @@
+# Define some meta-data about the simulation
+MetaData:
+  run_name:   EAGLE-L0100N1504-Ref
+
+# Define the system of units to use internally. 
+InternalUnitSystem:
+  UnitMass_in_cgs:     1.98848e43    # 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.
+  theta:                  0.7       # Opening angle (Multipole acceptance criterion)
+  mesh_side_length:       512
+  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)
+  dithering:             0
+
+# 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 in units of softening.
+  h_max:                             0.5      # Maximal softening in co-moving internal units.
+  CFL_condition:                     0.1      # 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:  1.5e10      # Minimal halo mass in which to seed a black hole (in solar masses).
+  scale_factor_first:              0.01        # Scale-factor of first FoF black hole seeding calls.
+  delta_time:                      1.005       # Scale-factor ratio between consecutive FoF black hole seeding calls.
+
+Scheduler:
+  max_top_level_cells:   64
+  tasks_per_cell:        5
+  cell_split_size:       200
+  
+Restarts:
+  onexit:       1
+  delta_hours:  1.0
+
+# Parameters related to the initial conditions
+InitialConditions:
+  file_name:  EAGLE_L0100N1504_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.
+
+# 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
+
+# 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:            0.5       # 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:               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_wind_delay_Gyr:              dummy           # 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:      4.0             # (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.
+  max_eddington_fraction:           1.0        # 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.
+  viscous_alpha:                    1e6        # Normalisation constant of the Bondi viscuous time-scale accretion reduction term
+  radiative_efficiency:             0.1        # Fraction of the accreted mass that gets radiated.
+  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.
+  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'
diff --git a/examples/EAGLE_ICs/EAGLE_100/getIC.sh b/examples/EAGLE_ICs/EAGLE_100/getIC.sh
new file mode 100755
index 0000000000000000000000000000000000000000..8b60aea542befc829f4b7b6825402adf1eaa7205
--- /dev/null
+++ b/examples/EAGLE_ICs/EAGLE_100/getIC.sh
@@ -0,0 +1,2 @@
+#!/bin/bash
+wget http://virgodb.cosma.dur.ac.uk/swift-webstorage/ICs/EAGLE_ICs/EAGLE_L0100N1504_ICs.hdf5
diff --git a/examples/EAGLE_ICs/EAGLE_100/output_list.txt b/examples/EAGLE_ICs/EAGLE_100/output_list.txt
new file mode 100644
index 0000000000000000000000000000000000000000..592ab8483d015fe1bfafe5cc603fabc230b25589
--- /dev/null
+++ b/examples/EAGLE_ICs/EAGLE_100/output_list.txt
@@ -0,0 +1,38 @@
+# Redshift
+18.08
+15.28
+13.06
+11.26
+9.79
+8.57
+7.54
+6.67
+5.92
+5.28
+4.72
+4.24
+3.81
+3.43
+3.09
+2.79
+2.52
+2.28
+2.06
+1.86
+1.68
+1.51
+1.36
+1.21
+1.08
+0.96
+0.85
+0.74
+0.64
+0.55
+0.46
+0.37
+0.29
+0.21
+0.14
+0.07
+0.00
diff --git a/examples/EAGLE_ICs/EAGLE_100/run.sh b/examples/EAGLE_ICs/EAGLE_100/run.sh
new file mode 100755
index 0000000000000000000000000000000000000000..6a2f423cd91fef9fa215d261839758443a2e0756
--- /dev/null
+++ b/examples/EAGLE_ICs/EAGLE_100/run.sh
@@ -0,0 +1,35 @@
+#!/bin/bash
+
+ # Generate the initial conditions if they are not present.
+if [ ! -e EAGLE_L0100N1504_ICs.hdf5 ]
+then
+    echo "Fetching initial conditions for the EAGLE 100Mpc example..."
+    ./getIC.sh
+fi
+
+# Grab the cooling and yield tables if they are not present.
+if [ ! -e yieldtables ]
+then
+    echo "Fetching EAGLE yield tables..."
+    ../getEagleYieldtable.sh
+fi
+
+if [ ! -e coolingtables ]
+then
+    echo "Fetching EAGLE cooling tables..."
+    ../getEagleCoolingTable.sh
+fi
+
+# The following run-time options are broken down by line as:
+# Basic run-time options
+# Create and run with stars
+# Radiative options - run with cooling and stellar feedback
+# Run with the time-step limiter required to capture feedback
+# Run with black holes - fof is needed for the seeding
+# Threading options - run with threads and pinning (latter not required but improves performance)
+# The corresponding parameter file for this run
+
+../../swift \
+    --cosmology --eagle \
+    --threads=16 --pin \
+    eagle_100.yml
diff --git a/examples/EAGLE_ICs/EAGLE_100/vrconfig_3dfof_subhalos_SO_hydro.cfg b/examples/EAGLE_ICs/EAGLE_100/vrconfig_3dfof_subhalos_SO_hydro.cfg
new file mode 100644
index 0000000000000000000000000000000000000000..8590cbf5bc77e8d7a956d210339cced4bbdc692c
--- /dev/null
+++ b/examples/EAGLE_ICs/EAGLE_100/vrconfig_3dfof_subhalos_SO_hydro.cfg
@@ -0,0 +1,191 @@
+#Configuration file for analysing Hydro
+#runs 3DFOF + substructure algorithm, demands subhalos and FOF halos be self-bound, calculates many properties
+#Units currently set to take in as input, Mpc, 1e10 solar masses, km/s, output in same units
+#To set temporally unique halo ids, alter Snapshot_value=SNAP to appropriate value. Ie: for snapshot 12, change SNAP to 12
+
+################################
+#input options
+#set up to use SWIFT HDF input, load gas, star, bh and dark matter
+################################
+HDF_name_convention=6 #HDF SWIFT naming convention
+Input_includes_dm_particle=1 #include dark matter particles in hydro input
+Input_includes_gas_particle=1 #include gas particles in hydro input
+Input_includes_star_particle=1 #include star particles in hydro input
+Input_includes_bh_particle=1 #include bh particles in hydro input
+Input_includes_wind_particle=0 #include wind particles in hydro input (used by Illustris and moves particle type 0 to particle type 3 when decoupled from hydro forces). Here shown as example
+Input_includes_tracer_particle=0 #include tracer particles in hydro input (used by Illustris). Here shown as example
+Input_includes_extradm_particle=0 #include extra dm particles stored in particle type 2 and type 3, useful for zooms
+
+Halo_core_phase_merge_dist=0.25 #merge substructures if difference in dispersion normalised distance is < this value
+Apply_phase_merge_to_host=1 #merge substructures with background if centrally located and phase-distance is small
+
+#units conversion from input input to desired internal unit
+Length_input_unit_conversion_to_output_unit=1.0 #default code unit,
+Velocity_input_unit_conversion_to_output_unit=1.0 #default velocity unit,
+Mass_input_unit_conversion_to_output_unit=1.0 #default mass unit,
+#assumes input is in 1e10 msun, Mpc and km/s and output units are the same
+Gravity=43.0211349 #for 1e10 Msun, km/s and Mpc
+Hubble_unit=100.0 # assuming units are km/s and Mpc, then value of Hubble in km/s/Mpc
+#converting hydro quantities
+Stellar_age_input_is_cosmological_scalefactor=1
+Metallicity_input_unit_conversion_to_output_unit=1.0
+Stellar_age_input_unit_conversion_to_output_unit=1.0
+Star_formation_rate_input_unit_conversion_to_output_unit=1.0
+
+#set the units of the output by providing conversion to a defined unit
+#conversion of output length units to kpc
+Length_unit_to_kpc=1000.0
+#conversion of output velocity units to km/s
+Velocity_to_kms=1.0
+#conversion of output mass units to solar masses
+Mass_to_solarmass=1.0e10
+#1 / 0.012
+Metallicity_to_solarmetallicity=83.33
+Star_formation_rate_to_solarmassperyear=97.78
+Stellar_age_to_yr=1.0
+#ensures that output is physical and not comoving distances per little h
+Comoving_units=0
+
+#sets the total buffer size in bytes used to store temporary particle information
+#of mpi read threads before they are broadcast to the appropriate waiting non-read threads
+#if not set, default value is equivalent to 1e6 particles per mpi process, quite large
+#but significantly minimises the number of send/receives
+#in this example the buffer size is roughly that for a send/receive of 10000 particles
+#for 100 mpi processes
+MPI_particle_total_buf_size=100000000
+
+################################
+#search related options
+################################
+
+#how to search a simulation
+Particle_search_type=1 #search dark matter particles only
+#for baryon search
+Baryon_searchflag=2 #if 1 search for baryons separately using phase-space search when identifying substructures, 2 allows special treatment in field FOF linking and phase-space substructure search, 0 treat the same as dark matter particles
+#for search for substruture
+Search_for_substructure=1 #if 0, end search once field objects are found
+#also useful for zoom simulations or simulations of individual objects, setting this flag means no field structure search is run
+Singlehalo_search=0 #if file is single halo in which one wishes to search for substructure. Here disabled.
+#additional option for field haloes
+Keep_FOF=0 #if field 6DFOF search is done, allows to keep structures found in 3DFOF (can be interpreted as the inter halo stellar mass when only stellar search is used).\n
+
+#minimum size for structures
+Minimum_size=20 #min 20 particles
+Minimum_halo_size=32 #if field halos have different minimum sizes, otherwise set to -1.
+
+#for field fof halo search
+FoF_Field_search_type=5 #5 3DFOF search for field halos, 4 for 6DFOF clean up of field halos, 3 for 6DFOF with velocity scale distinct for each initial 3D FOF candidate
+Halo_3D_linking_length=0.20
+
+#for mean field estimates and local velocity density distribution funciton estimator related quantiites, rarely need to change this
+Local_velocity_density_approximate_calculation=1 #calculates velocity density using approximative (and quicker) near neighbour search
+Cell_fraction = 0.01 #fraction of field fof halo used to determine mean velocity distribution function. Typical values are ~0.005-0.02
+Grid_type=1 #normal entropy based grid, shouldn't have to change
+Nsearch_velocity=32 #number of velocity neighbours used to calculate local velocity distribution function. Typial values are ~32
+Nsearch_physical=256 #numerof physical neighbours from which the nearest velocity neighbour set is based. Typical values are 128-512
+
+#for substructure search, rarely ever need to change this
+FoF_search_type=1 #default phase-space FOF search. Don't really need to change
+Iterative_searchflag=1 #iterative substructure search, for substructure find initial candidate substructures with smaller linking lengths then expand search region
+Outlier_threshold=2.5 #outlier threshold for a particle to be considered residing in substructure, that is how dynamically distinct a particle is. Typical values are >2
+Substructure_physical_linking_length=0.10
+Velocity_ratio=2.0 #ratio of speeds used in phase-space FOF
+Velocity_opening_angle=0.10 #angle between velocities. 18 degrees here, typical values are ~10-30
+Velocity_linking_length=0.20 #where scaled by structure dispersion
+Significance_level=1.0 #how significant a substructure is relative to Poisson noise. Values >= 1 are fine.
+
+#for iterative substructure search, rarely ever need to change this
+Iterative_threshold_factor=1.0 #change in threshold value when using iterative search. Here no increase in threshold if iterative or not
+Iterative_linking_length_factor=2.0 #increase in final linking final iterative substructure search 
+Iterative_Vratio_factor=1.0 #change in Vratio when using iterative search. no change in vratio
+Iterative_ThetaOp_factor=1.0 #change in velocity opening angle. no change in velocity opening angle
+
+#for checking for halo merger remnants, which are defined as large, well separated phase-space density maxima
+Halo_core_search=2 # searches for separate 6dfof cores in field haloes, and then more than just flags halo as merging, assigns particles to each merging "halo". 2 is full separation, 1 is flagging, 0 is off
+#if searching for cores, linking lengths. likely does not need to change much
+Use_adaptive_core_search=0 #calculate dispersions in configuration & vel space to determine linking lengths
+Use_phase_tensor_core_growth=2 #use full stepped phase-space tensor assignment
+Halo_core_ellx_fac=0.7 #how linking lengths are changed when searching for local 6DFOF cores,
+Halo_core_ellv_fac=2.0 #how velocity lengths based on dispersions are changed when searching for local 6DFOF cores
+Halo_core_ncellfac=0.005 #fraction of total halo particle number setting min size of a local 6DFOF core
+Halo_core_num_loops=8 #number of loops to iteratively search for cores
+Halo_core_loop_ellx_fac=0.75 #how much to change the configuration space linking per iteration
+Halo_core_loop_ellv_fac=1.0 #how much to change the velocity space linking per iteration
+Halo_core_loop_elln_fac=1.2 #how much to change the min number of particles per iteration
+Halo_core_phase_significance=2.0 #how significant a core must be in terms of dispersions (sigma) significance
+
+################################
+#Unbinding options (VELOCIraptor is able to accurately identify tidal debris so particles need not be bound to a structure)
+################################
+
+#unbinding related items
+Unbind_flag=1 #run unbinding
+#objects must have particles that meet the allowed kinetic to potential ratio AND also have some total fraction that are completely bound.
+Unbinding_type=0
+#alpha factor used to determine whether particle is "bound" alaph*T+W<0. For standard subhalo catalogues use >0.9 but if interested in tidal debris 0.2-0.5
+Allowed_kinetic_potential_ratio=0.95
+Min_bound_mass_frac=0.65 #minimum bound mass fraction
+#run unbinding of field structures, aka halos. This is useful for sams and 6DFOF halos but may not be useful if interested in 3DFOF mass functions.
+Bound_halos=0
+#don't keep background potential when unbinding
+Keep_background_potential=1
+#use all particles to determine velocity frame for unbinding
+Frac_pot_ref=1.0
+Min_npot_ref=20
+#reference frame only meaningful if calculating velocity frame using subset of particles in object. Can use radially sorted fraction of particles about minimum potential or centre of mass
+Kinetic_reference_frame_type=0
+Unbinding_max_unbound_removal_fraction_per_iteration=0.5
+Unbinding_max_unbound_fraction=0.95
+Unbinding_max_unbound_fraction_allowed=0.005
+
+################################
+#Calculation of properties related options
+################################
+Virial_density=500 #user defined virial overdensity. Note that 200 rho_c, 200 rho_m and BN98 are already calculated.
+#when calculating properties, for field objects calculate inclusive masses
+Inclusive_halo_masses=3 #calculate inclusive masses for halos using full Spherical overdensity apertures
+#ensures that output is physical and not comoving distances per little h
+Comoving_units=0
+#calculate more (sub)halo properties (like angular momentum in spherical overdensity apertures, both inclusive and exclusive)
+Extensive_halo_properties_output=1
+Extensive_gas_properties_output=1
+Extensive_star_properties_output=1
+#calculate aperture masses
+Calculate_aperture_quantities=1 
+Number_of_apertures=5
+Aperture_values_in_kpc=5,10,30,50,100,
+Number_of_projected_apertures=5
+Projected_aperture_values_in_kpc=5,10,30,50,100,
+#calculate radial profiles
+Calculate_radial_profiles=1
+Number_of_radial_profile_bin_edges=20
+#default radial normalisation log rad bins, normed by R200crit, Integer flag of 0 is log bins and R200crit norm. 
+Radial_profile_norm=0
+Radial_profile_bin_edges=-2.,-1.87379263,-1.74758526,-1.62137789,-1.49517052,-1.36896316,-1.24275579,-1.11654842,-0.99034105,-0.86413368,-0.73792631,-0.61171894,-0.48551157,-0.3593042,-0.23309684,-0.10688947,0.0193179,0.14552527,0.27173264,0.39794001,
+Iterate_cm_flag=0 #do not interate to determine centre-of-mass
+Sort_by_binding_energy=1 #sort particles by binding energy
+Reference_frame_for_properties=2 #use the minimum potential as reference frame about which to calculate properties 
+
+################################
+#output related
+################################
+
+Write_group_array_file=0 #do not write a group array file
+Separate_output_files=0 #do not separate output into field and substructure files similar to subfind
+Binary_output=2 #Use HDF5 output (binary output 1, ascii 0, and HDF 2)
+#output particles residing in the spherical overdensity apertures of halos, only the particles exclusively belonging to halos
+Spherical_overdensity_halo_particle_list_output=1
+
+#halo ids are adjusted by this value * 1000000000000 (or 1000000 if code compiled with the LONGINTS option turned off)
+#to ensure that halo ids are temporally unique. So if you had 100 snapshots, for snap 100 set this to 100 and 100*1000000000000 will
+#be added to the halo id as set for this snapshot, so halo 1 becomes halo 100*1000000000000+1 and halo 1 of snap 0 would just have ID=1
+
+#ALTER THIS as part of a script to get temporally unique ids
+Snapshot_value=SNAP
+
+################################
+#other options
+################################
+Verbose=0 #how talkative do you want the code to be, 0 not much, 1 a lot, 2 chatterbox
+
+