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Diffstat (limited to 'fg21sim/extragalactic/clusters/formation.py')
| -rw-r--r-- | fg21sim/extragalactic/clusters/formation.py | 34 |
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( |