Commit 2fbb4023 authored by Matthieu Schaller's avatar Matthieu Schaller
Browse files

Merge branch 'master' into line_of_sight

parents 117c61e5 b9af415a
Various hints on settings needed to get various MPIs running with SWIFT.
Last update 5th May 2020.
## Intel MPI
_Intel MPI 2018_ usually runs without any needs for special settings.
_Intel MPI 2019 and 2020_ can run for small tests, but without flags will
generally deadlock in the MPI exchanges of the engine, or worse. In that case
try the following settings.
```
FI_OFI_RXM_RX_SIZE=4096
FI_OFI_RXM_TX_SIZE=4096
FI_UNIVERSE_SIZE=2048
```
If you want use the `release_mt` library, then you also need to use:
```
source $I_MPI_ROOT/intel64/bin/mpivars.sh release_mt
```
when initializing the library environment. Some success has also been seen
using the asynchronous progression settings:
```
I_MPI_ASYNC_PROGRESS=1
I_MPI_ASYNC_PROGRESS_THREADS=1
```
(note these are tested with `2019 update-4` and `2020 update-1` on Mellanox).
## OpenMPI
_Open MPI_ comes in many flavours with many combinations of underlying
transport libraries and running on many different fabrics. A complete
description of all combinations is beyond the scope of this guide.
On Mellanox hardware, we have had success running version 4.0 with the
UCX layer version 1.6 and using the following settings:
```
-mca coll_hcoll_enable 0
UCX_TLS=ud_x,shm,self
UCX_RC_MLX5_TM_ENABLE=n
UCX_DC_MLX5_TM_ENABLE=n
```
......@@ -1493,7 +1493,7 @@ case "$with_subgrid" in
with_subgrid_feedback=GEAR
with_subgrid_black_holes=none
with_subgrid_task_order=GEAR
with_subgrid_sink=none
with_subgrid_sink=none
enable_fof=no
;;
QLA)
......@@ -1506,7 +1506,7 @@ case "$with_subgrid" in
with_subgrid_feedback=none
with_subgrid_black_holes=none
with_subgrid_task_order=default
with_subgrid_sink=none
with_subgrid_sink=none
enable_fof=no
;;
EAGLE)
......@@ -1519,7 +1519,7 @@ case "$with_subgrid" in
with_subgrid_feedback=EAGLE
with_subgrid_black_holes=EAGLE
with_subgrid_task_order=EAGLE
with_subgrid_sink=none
with_subgrid_sink=none
enable_fof=yes
;;
*)
......@@ -2025,62 +2025,62 @@ case "$with_black_holes" in
;;
esac
# sink model.
# Sink model.
AC_ARG_WITH([sink],
[AS_HELP_STRING([--with-sink=<model>],
[Sink particle model to use @<:@none, default: none@:>@]
)],
[with_sink="$withval"],
[with_sink="none"]
[AS_HELP_STRING([--with-sink=<model>],
[Sink particle model to use @<:@none, default: none@:>@]
)],
[with_sink="$withval"],
[with_sink="none"]
)
if test "$with_subgrid" != "none"; then
if test "$with_sink" != "none"; then
AC_MSG_ERROR([Cannot provide with-subgrid and with-sink together])
else
with_sink="$with_subgrid_sink"
fi
if test "$with_sink" != "none"; then
AC_MSG_ERROR([Cannot provide with-subgrid and with-sink together])
else
with_sink="$with_subgrid_sink"
fi
fi
case "$with_sink" in
none)
AC_DEFINE([SINK_NONE], [1], [No sink particle model])
;;
*)
AC_MSG_ERROR([Unknown sink particle model model: $with_sink])
;;
none)
AC_DEFINE([SINK_NONE], [1], [No sink particle model])
;;
*)
AC_MSG_ERROR([Unknown sink particle model model: $with_sink])
;;
esac
# Task order
AC_ARG_WITH([task-order],
[AS_HELP_STRING([--with-task-order=<model>],
[Task order to use @<:@default, EAGLE, GEAR default: default@:>@]
)],
[with_task_order="$withval"],
[with_task_order="default"]
[AS_HELP_STRING([--with-task-order=<model>],
[Task order to use @<:@default, EAGLE, GEAR default: default@:>@]
)],
[with_task_order="$withval"],
[with_task_order="default"]
)
if test "$with_subgrid" != "none"; then
if test "$with_task_order" != "default"; then
AC_MSG_ERROR([Cannot provide with-subgrid and with-task-order together])
else
with_task_order="$with_subgrid_task_order"
fi
if test "$with_task_order" != "default"; then
AC_MSG_ERROR([Cannot provide with-subgrid and with-task-order together])
else
with_task_order="$with_subgrid_task_order"
fi
fi
case "$with_task_order" in
EAGLE)
AC_DEFINE([TASK_ORDER_EAGLE], [1], [EAGLE task order])
;;
default)
AC_DEFINE([TASK_ORDER_DEFAULT], [1], [Default (i.e. EAGLE/OWLS) task order])
;;
GEAR)
AC_DEFINE([TASK_ORDER_GEAR], [1], [GEAR task order])
;;
*)
AC_MSG_ERROR([Unknown task ordering: $with_task_order])
;;
EAGLE)
AC_DEFINE([TASK_ORDER_EAGLE], [1], [EAGLE task order])
;;
default)
AC_DEFINE([TASK_ORDER_DEFAULT], [1], [Default (i.e. EAGLE/OWLS) task order])
;;
GEAR)
AC_DEFINE([TASK_ORDER_GEAR], [1], [GEAR task order])
;;
*)
AC_MSG_ERROR([Unknown task ordering: $with_task_order])
;;
esac
# External potential
......
digraph feedback {
subgraph cluster_data {
Data[shape="none", label=<
<table BORDER="0">
<tr>
<td><u>Data</u></td>
</tr>
<tr>
<td>elts</td>
</tr>
<tr>
<td>MeanWDMass</td>
</tr>
<tr>
<td>SolarMassAbundances</td>
</tr>
</table>>];
}
subgraph cluster_imf {
IMF[shape="none", label=<
<table BORDER="0">
<tr>
<td><u>IMF</u></td>
</tr>
<tr>
<td>n</td>
</tr>
<tr>
<td>as</td>
</tr>
<tr>
<td>ms</td>
</tr>
<tr>
<td>Mmin</td>
</tr>
<tr>
<td>Mmax</td>
</tr></table>>];
}
subgraph cluster_lifetimes {
LifeTimes[label=<<u>LifeTimes</u>>,shape="none"];
}
subgraph cluster_snii {
SNII[shape="none", label=<
<table BORDER="0">
<tr>
<td><u>SNII</u></td>
</tr>
<tr>
<td>Mmin</td>
</tr>
<tr>
<td>Mmax</td>
</tr>
</table>>];
}
subgraph cluster_snia {
SNIa[shape="none", label=<
<table BORDER="0">
<tr>
<td><u>SNIa</u></td>
</tr>
<tr>
<td>a</td>
</tr>
<tr>
<td>Mpl</td>
</tr>
<tr>
<td>Mpu</td>
</tr>
<tr>
<td>Mdu1</td>
</tr>
<tr>
<td>Mdl1</td>
</tr>
<tr>
<td>bb1</td>
</tr>
<tr>
<td>Mdu2</td>
</tr>
<tr>
<td>Mdl2</td>
</tr>
<tr>
<td>bb2</td>
</tr>
</table>>];
}
subgraph cluster_snii_all {
graph[style="dotted"];
snii_all[shape="none", label=<
<table BORDER="0">
<tr>
<td><u>An array per element</u></td>
</tr>
<tr>
<td>min</td>
</tr>
<tr>
<td>step</td>
</tr>
</table>>];
}
subgraph cluster_snii_ej {
graph[style="dotted"];
snii_ej[shape="none", label=<
<table BORDER="0">
<tr>
<td><u>Ej</u></td>
</tr>
<tr>
<td>min</td>
</tr>
<tr>
<td>step</td>
</tr>
</table>>];
}
subgraph cluster_snii_ejnp {
graph[style="dotted"];
snii_ejnp[shape="none", label=<
<table BORDER="0">
<tr>
<td><u>Ejnp</u></td>
</tr>
<tr>
<td>min</td>
</tr>
<tr>
<td>step</td>
</tr>
</table>>];
}
subgraph cluster_coeff_z {
graph[style="dotted"];
coeff_z[label=<<u>coeff_z</u>>, shape="none"];
}
subgraph cluster_snia_metals {
snia_metals[shape="none", label=<
<table BORDER="0">
<tr>
<td><u>Metals</u></td>
</tr>
<tr>
<td>elts</td>
</tr>
<tr>
<td>data</td>
</tr>
</table>>];
}
Data->LifeTimes;
Data->IMF;
Data->SNII;
Data->SNIa;
LifeTimes->coeff_z;
SNII->snii_all;
SNII->snii_ej;
SNII->snii_ejnp;
SNIa->snia_metals;
}
\ No newline at end of file
......@@ -115,7 +115,7 @@ A star will be able to form if a randomly drawn number is below :math:`\frac{m_g
Chemistry
~~~~~~~~~
In the chemistry, we are using the smoothed metallicity scheme that consists in using the SPH to smooth the metallicity of each particle over the neighbors. It is worth to point the fact that we are not exchanging any metals but only smoothing it. The parameter ``GEARChemistry:initial_metallicity`` set the initial mass fraction of each element for all the particles and ``GEARChemistry:scale_initial_metallicity`` use the feedback table to scale the initial metallicity of each element according the Sun's composition.
In the chemistry, we are using the smoothed metallicity scheme that consists in using the SPH to smooth the metallicity of each particle over the neighbors. It is worth to point the fact that we are not exchanging any metals but only smoothing it. The parameter ``GEARChemistry:initial_metallicity`` set the (non smoothed) initial mass fraction of each element for all the particles and ``GEARChemistry:scale_initial_metallicity`` use the feedback table to scale the initial metallicity of each element according the Sun's composition.
.. code:: YAML
......@@ -145,6 +145,7 @@ Initial mass function
GEAR is using the IMF model from `Kroupa (2001) <https://ui.adsabs.harvard.edu/abs/2001MNRAS.322..231K/abstract>`_.
We have a difference of 1 in the exponent due to the usage of IMF in mass and not in number.
We also restrict the mass of the stars to be inside :math:`[0.05, 50] M_\odot`.
Here is the default model used, but it can be easily adapted through the initial mass function parameters:
.. math::
\xi(m) \propto m^{-\alpha_i}\, \textrm{where}\,
......@@ -156,8 +157,6 @@ We also restrict the mass of the stars to be inside :math:`[0.05, 50] M_\odot`.
\end{cases}
Lifetime
^^^^^^^^
......@@ -170,6 +169,7 @@ The lifetime of a star in GEAR depends only on two parameters: first its mass an
c(Z) = -261.365 Z^2 + 17.073 Z + 9.8661
where :math:`\tau` is the lifetime in years, :math:`m` is the mass of the star (in solar mass) and Z the metallicity of the star.
The parameters previously given are the default ones, they can be modified in the parameters file.
Supernovae II
^^^^^^^^^^^^^
......@@ -215,6 +215,24 @@ Energy injection
All the supernovae (type II and Ia) inject the same amount of energy into the surrounding gas (``GEARFeedback:supernovae_energy_erg``) and distribute it according to the hydro kernel.
The same is done with the metals and the mass.
Generating a new table
^^^^^^^^^^^^^^^^^^^^^^
The feedback table is an HDF5 file with the following structure:
.. graphviz:: feedback_table.dot
where the solid (dashed) squares represent a group (a dataset) with the name of the object underlined and the attributes written below. Everything is in solar mass or without units (e.g. mass fraction or unitless constant).
In ``Data``, the attribute ``elts`` is an array of string with the element names (the last should be ``Metals``, it corresponds to the sum of all the elements), ``MeanWDMass`` is the mass of the white dwarfs
and ``SolarMassAbundances`` is an array of float containing the mass fraction of the different element in the sun.
In ``IMF``, ``n + 1`` is the number of part in the IMF, ``as`` are the exponent (``n+1`` elements), ``ms`` are the mass limits between each part (``n`` elements) and
``Mmin`` (``Mmax``) is the minimal (maximal) mass of a star.
In ``LifeTimes``, the coefficient are given in the form of a single table (``coeff_z`` with a 3x3 shape).
In ``SNIa``, ``a`` is the exponent of the distribution of binaries, ``bb1`` and ``bb2`` are the coefficient :math:`b_i` and the other attributes follow the same names than in the SNIa formulas.
The ``Metals`` group from the ``SNIa`` contains the name of each elements (``elts``) and the metal mass fraction ejected by each supernovae (``data``) in the same order. They must contain the same elements than in ``Data``.
Finally for the ``SNII``, the mass limits are given by ``Mmin`` and ``Mmax``. For the yields, the datasets required are ``Ej`` (mass fraction ejected [processed]), ``Ejnp`` (mass fraction ejected [non processed]) and one dataset for each element present in ``elts``. The datasets should all have the same size, be uniformly sampled in log and contains the attributes ``min`` (mass in log for the first element) and ``step`` (difference of mass in log between two elements).
.. code:: YAML
GEARFeedback:
......
......@@ -41,6 +41,11 @@ extensions = [
'sphinx.ext.todo',
'sphinx.ext.mathjax',
'sphinx.ext.githubpages',
'sphinx.ext.graphviz'
]
graphviz_dot_args=[
"-Grankdir=LR"
]
# Add any paths that contain templates here, relative to this directory.
......
......@@ -183,6 +183,7 @@ 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.
with_angmom_limiter: 1 # Are we applying the Rosas-Guevara (2015) viscous time-scale reduction term?
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.
......
......@@ -183,6 +183,7 @@ 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.
with_angmom_limiter: 1 # Are we applying the Rosas-Guevara (2015) viscous time-scale reduction term?
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.
......
......@@ -184,6 +184,7 @@ 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.
with_angmom_limiter: 1 # Are we applying the Rosas-Guevara (2015) viscous time-scale reduction term?
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.
......
......@@ -182,6 +182,7 @@ 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.
with_angmom_limiter: 1 # Are we applying the Rosas-Guevara (2015) viscous time-scale reduction term?
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.
......
Initial conditions corresponding to the 50 Mpc volume
of the EAGLE suite at 8x lower resolution.
The ICs only contain DM particles. The gas particles will be generated in SWIFT.
# Define some meta-data about the simulation
MetaData:
run_name: EAGLE-L0050N0376-Ref
# Define the system of units to use internally.
InternalUnitSystem:
UnitMass_in_cgs: 1.98841e43 # 10^10 M_sun in grams
UnitLength_in_cgs: 3.08567758e24 # Mpc in centimeters
UnitVelocity_in_cgs: 1e5 # km/s in centimeters per second
UnitCurrent_in_cgs: 1 # Amperes
UnitTemp_in_cgs: 1 # Kelvin
# Cosmological parameters
Cosmology:
h: 0.6777 # Reduced Hubble constant
a_begin: 0.0078125 # Initial scale-factor of the simulation
a_end: 1.0 # Final scale factor of the simulation
Omega_m: 0.307 # Matter density parameter
Omega_lambda: 0.693 # Dark-energy density parameter
Omega_b: 0.0482519 # Baryon density parameter
# Parameters governing the time integration
TimeIntegration:
dt_min: 1e-10 # The minimal time-step size of the simulation (in internal units).
dt_max: 1e-2 # The maximal time-step size of the simulation (in internal units).
# Parameters governing the snapshots
Snapshots:
basename: eagle # Common part of the name of output files
output_list_on: 1
output_list: ./output_list.txt
# Parameters governing the conserved quantities statistics
Statistics:
delta_time: 1.02
scale_factor_first: 0.05
# Parameters for the self-gravity scheme
Gravity:
eta: 0.025 # Constant dimensionless multiplier for time integration.
theta: 0.7 # Opening angle (Multipole acceptance criterion)
mesh_side_length: 128
comoving_DM_softening: 0.006640 # Comoving softening for DM (6.67 ckpc)
max_physical_DM_softening: 0.002600 # Physical softening for DM (2.60 pkpc)
comoving_baryon_softening: 0.003580 # Comoving softening for baryons (3.58 ckpc)
max_physical_baryon_softening: 0.001400 # Physical softening for baryons (1.40 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 length in units of softening.
h_max: 0.5 # Maximal smoothing length in co-moving internal units.
CFL_condition: 0.2 # Courant-Friedrich-Levy condition for time integration.
minimal_temperature: 100.0 # (internal units)
initial_temperature: 268.7 # (internal units)
particle_splitting: 1 # Particle splitting is ON
particle_splitting_mass_threshold: 5.6e-3 # (internal units, i.e. 5.6e7 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: 32 # 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: 0.05 # Scale-factor of first FoF black hole seeding calls.
delta_time: 1.00751 # Scale-factor ratio between consecutive FoF black hole seeding calls.
Scheduler:
max_top_level_cells: 16
cell_split_size: 200
Restarts:
onexit: 1
delta_hours: 6.0
# Parameters related to the initial conditions
InitialConditions:
file_name: EAGLE_L0050N0376_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.