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-rw-r--r--fg21sim/configs/20-extragalactic.conf.spec27
-rw-r--r--fg21sim/extragalactic/clusters/halo.py10
2 files changed, 24 insertions, 13 deletions
diff --git a/fg21sim/configs/20-extragalactic.conf.spec b/fg21sim/configs/20-extragalactic.conf.spec
index 8749c67..44fb1ca 100644
--- a/fg21sim/configs/20-extragalactic.conf.spec
+++ b/fg21sim/configs/20-extragalactic.conf.spec
@@ -10,12 +10,13 @@
[extragalactic]
-
+ #
# Press-Schechter formalism to determine the dark matter halos
# distribution with respect to masses and redshifts, from which
# to further determine the total number of halos within a sky
# patch and to sample the masses and redshifts for each halo.
# NOTE: only consider the *dark matter* mass within the halo!
+ #
[[psformalism]]
# The model of the fitting function for halo mass distribution
# For all models and more details:
@@ -52,9 +53,12 @@
# Unit: [Msun] (the little "h" is folded into the values)
dndlnm_outfile = string(default=None)
+
+ #
# Extended emissions from the clusters of galaxies
# The configurations in this ``[[clusters]]`` section may also be
# used by the following ``[[halos]]`` section.
+ #
[[clusters]]
# Output CSV file of the clusters catalog containing the simulated
# mass, redshift, position, shape, and the recent major merger info.
@@ -148,20 +152,21 @@
output_dir = string(default=None)
- # Giant radio halos for clusters with recent major mergers
+ #
+ # Giant radio halos
+ #
[[halos]]
+ # A custom parameter to tune the turbulent acceleration timescale.
+ # NOTE: The smaller this parameter, the shorter the acceleration
+ # timescale, therefore more efficient acceleration.
+ f_acc = float(default=1.0, min=0.1, max=10)
+
# The turbulence is generally injected at the cluster center during
# a merger. This option parameterize the turbulence injection scale
- # to be a fraction of the virial radius of the (main) cluster, which
- # is also used to determine the radio halo radius.
+ # to be a fraction of the virial radius of the cluster, which is also
+ # used to determine the radio halo size.
f_lturb = float(default=0.33, min=0.1, max=1.0)
- # The custom option to tune the turbulent acceleration timescale, which
- # controls the relativistic particle acceleration efficiencies.
- # NOTE: The smaller this parameter, the shorter the acceleration
- # timescale, therefore the more efficient the turbulent acceleration.
- f_acc = float(default=1.5, min=0.1, max=10)
-
# The fraction of cluster thermal energy originating from turbulent
# dissipation, which describes the turbulence intensity in the ICM,
# and determines its Mach number.
@@ -207,7 +212,9 @@
time_init = float(default=0.6, min=0)
+ #
# Extragalactic point sources
+ #
[[pointsources]]
# Output directory to save the simulated catalog
output_dir = string(default="PS_tables")
diff --git a/fg21sim/extragalactic/clusters/halo.py b/fg21sim/extragalactic/clusters/halo.py
index 5df47cd..03e891c 100644
--- a/fg21sim/extragalactic/clusters/halo.py
+++ b/fg21sim/extragalactic/clusters/halo.py
@@ -90,7 +90,7 @@ class RadioHalo:
considering only losses and constant injection, in order to derive
an approximately steady electron spectrum for following use;
5. Calculate the magnetic field from the cluster total mass (which
- is assumed to be growth linearly from M_main+M_sub to M_obs);
+ is assumed to be growth linearly from M_main to M_obs);
6. Calculate the energy losses for the coefficients of Fokker-Planck
equation;
7. Solve the Fokker-Planck equation to derive the relativistic
@@ -789,8 +789,12 @@ class RadioHalo:
NOTE
----
- We assume that the main cluster grows (i.e., gains mass) linearly
- in time from (M_main, z_merge) to (M_obs, z_obs).
+ Since we currently only consider the last major merger event,
+ there may be a long time between ``z_merger`` and ``z_obs``.
+ So we assume that the main cluster grows linearly in time from
+ (M_main, z_merger) to (M_obs, z_obs).
+
+ TODO: consider the full merging history.
Parameters
----------