diff options
| -rw-r--r-- | fg21sim/configs/20-extragalactic.conf.spec | 27 | ||||
| -rw-r--r-- | fg21sim/extragalactic/clusters/halo.py | 10 |
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 ---------- |