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authorAaron LI <aly@aaronly.me>2017-07-31 19:45:40 +0800
committerAaron LI <aly@aaronly.me>2017-07-31 19:45:40 +0800
commitcdfae1365414e1e816de62b5b0e441df456f385b (patch)
tree98ebdd3061697439da612ae7cb377f46c54c611f /fg21sim/extragalactic/clusters/formation.py
parent915bb22299a9927fcd3bce8456e4ae0dc99dac90 (diff)
downloadfg21sim-cdfae1365414e1e816de62b5b0e441df456f385b.tar.bz2
Update references a bit
Signed-off-by: Aaron LI <aly@aaronly.me>
Diffstat (limited to 'fg21sim/extragalactic/clusters/formation.py')
-rw-r--r--fg21sim/extragalactic/clusters/formation.py34
1 files changed, 15 insertions, 19 deletions
diff --git a/fg21sim/extragalactic/clusters/formation.py b/fg21sim/extragalactic/clusters/formation.py
index 02b26f4..a9c9acc 100644
--- a/fg21sim/extragalactic/clusters/formation.py
+++ b/fg21sim/extragalactic/clusters/formation.py
@@ -1,4 +1,4 @@
-# Copyright (c) 2017 Weitian LI <liweitianux@live.com>
+# Copyright (c) 2017 Weitian LI <weitian@aaronly.me>
# MIT license
"""
@@ -7,10 +7,13 @@ Press-Schechter formalism.
References
----------
-[1] Randall, Sarazin & Ricker 2002, ApJ, 577, 579
- http://adsabs.harvard.edu/abs/2002ApJ...577..579R
-[2] Cassano & Brunetti 2005, MNRAS, 357, 1313
- http://adsabs.harvard.edu/abs/2005MNRAS.357.1313C
+.. [randall2002]
+ Randall, Sarazin & Ricker 2002, ApJ, 577, 579
+ http://adsabs.harvard.edu/abs/2002ApJ...577..579R
+
+.. [cassano2005]
+ Cassano & Brunetti 2005, MNRAS, 357, 1313
+ http://adsabs.harvard.edu/abs/2005MNRAS.357.1313C
"""
import logging
@@ -32,13 +35,6 @@ class ClusterFormation:
Simulate the cluster formation (i.e., merging history) using the extended
Press-Schechter formalism by Monte Carlo methods.
- References
- ----------
- [1] Randall, Sarazin & Ricker 2002, ApJ, 577, 579
- http://adsabs.harvard.edu/abs/2002ApJ...577..579R
- [2] Cassano & Brunetti 2005, MNRAS, 357, 1313
- http://adsabs.harvard.edu/abs/2005MNRAS.357.1313C
-
Parameters
----------
M0 : float
@@ -81,7 +77,7 @@ class ClusterFormation:
The power-law spectral index assumed for the following density
perturbations sigma(M).
- References: Ref.[1],Eq.(2)
+ References: Ref.[randall2002],Eq.(2)
"""
n = -7/5
alpha = (n+3) / 6
@@ -95,7 +91,7 @@ class ClusterFormation:
It is generally sufficient to consider a power-law spectrum of
density perturbations, which is consistent with the CDM models.
- References: Ref.[1],Eq.(2)
+ References: Ref.[randall2002],Eq.(2)
"""
alpha = self.sigma_index
sigma = COSMO.sigma8 * (mass / COSMO.M8) ** (-alpha)
@@ -108,7 +104,7 @@ class ClusterFormation:
This is a monotone decreasing function.
- References: Ref.[1],App.A,Eq.(A1)
+ References: Ref.[randall2002],App.A,Eq.(A1)
"""
return COSMO.overdensity_crit(z)
@@ -121,7 +117,7 @@ class ClusterFormation:
dw^2 ~< abs(d(ln(sigma(M)^2)) / d(ln(M))) * (dMc / M) * sigma(M)^2
= 2 * alpha * sigma(M)^2 * dMc / M
- References: Ref.[1],Sec.(3.1),Para.(1)
+ References: Ref.[randall2002],Sec.(3.1),Para.(1)
"""
alpha = self.sigma_index
dMc = self.merger_mass_min
@@ -142,7 +138,7 @@ class ClusterFormation:
S = sigma(M)^2
- References: Ref.[1],Sec.(3)
+ References: Ref.[randall2002],Sec.(3)
"""
alpha = self.sigma_index
mass = COSMO.M8 * (S / COSMO.sigma8**2)**(-1/(2*alpha))
@@ -154,7 +150,7 @@ class ClusterFormation:
The cumulative probability distribution function of sub-cluster
masses.
- References: Ref.[1],Eq.(5)
+ References: Ref.[randall2002],Eq.(5)
"""
p = scipy.special.erfc(dw / np.sqrt(2*dS))
return p
@@ -187,7 +183,7 @@ class ClusterFormation:
halo/cluster.
(default: True)
- References: Ref.[1],Sec.(3.1)
+ References: Ref.[randall2002],Sec.(3.1)
"""
logger.debug("Simulating cluster formation: " +
"M0={:.3g}[Msun] from z={:.3f} to z={zmax} ...".format(