def plot_halo_mass_func(self):
"""Plots the halo mass function from simulation as well as Sheth-Torman"""
self.load_sigDLA()
mass = np.logspace(8, 13, 51)
halo_mass = halo_mass_function.HaloMassFunction(self.redshift,
omega_m=self.omegam,
omega_l=self.omegal,
hubble=self.hubble,
log_mass_lim=(7, 15))
shdndm = [halo_mass.dndm(mm) for mm in mass]
adndm = np.array(
[self.get_dndm(mass[ii], mass[ii + 1]) for ii in range(0, 50)])
plt.loglog(mass, shdndm, color="black", ls='--', label="Sheth-Tormen")
plt.loglog(mass[0:-1], adndm, color=acol, ls=astyle, label="Arepo")
#Make the ticks be less-dense
ax = plt.gca()
ax.yaxis.set_ticks(
np.power(
10.,
np.arange(int(np.log10(shdndm[-1])), int(np.log10(shdndm[0])),
2)))
plt.ylabel(r"dn/dM (h$^4$ $M^{-1}_\odot$ Mpc$^{-3}$)")
plt.xlabel(r"Mass ($M_\odot$ h$^{-1}$)")
plt.legend(loc=0)
# plt.xlim(self.minplot,self.maxplot)
tight_layout_wrapper()
plt.show()
def halonumber(n):
halo = hmf.HaloMassFunction(redshift=0) #set redshift = 0
h = 0.67 #hubble constant
mass = np.array([12 + i * 8 / n for i in range(0, n + 1)
]) / h #upper limit of halo mass is 20 Msolar/h
dn = halo.dndm(mass)
number = (sum(2 * dn) - dn[0] - dn[-1]) * 8 / (
2 * n * h) #use sum to calculate integral.
print(
"Hubble constant is %.2f.\nThe number of halos per (Mpc/h)^3 are %.0f"
% (h, number))
def plot_rel_halo_mass_func(self):
"""Plots the halo mass function from simulation divided by fitting formula"""
self.load_sigDLA()
massedge=np.logspace(8,13,51)
halo_mass=halo_mass_function.HaloMassFunction(self.redshift,omega_m=self.omegam, omega_l=self.omegal, hubble=self.hubble,log_mass_lim=(7,15))
adndm=np.array([self.get_dndm(massedge[ii],massedge[ii+1]) for ii in range(np.size(massedge)-1)])
mass=np.array([(massedge[ii]+massedge[ii+1])/2. for ii in range(np.size(massedge)-1)])
shdndm=[halo_mass.dndm(mm) for mm in mass]
plt.semilogx(mass,adndm/shdndm,color="black",ls='-')
#Make the ticks be less-dense
plt.xlabel(r"Mass ($M_\odot$ h$^{-1}$)")
# plt.xlim(self.minplot,self.maxplot)
tight_layout_wrapper()
plt.show()
def get_N_DLA_dz(self,params, mass=1e9,maxmass=12.5):
"""Get the DLA number density as a function of redshift, defined as:
d N_DLA / dz ( > M, z) = dr/dz int^infinity_M n_h(M', z) sigma_DLA(M',z) dM'
where n_h is the Sheth-Torman mass function, and
sigma_DLA is a power-law fit to self.sigma_DLA.
Parameters:
lower_mass in M_sun/h.
"""
try:
self.halo_mass.dndm(mass)
except AttributeError:
#Halo mass function object
self.halo_mass=halo_mass_function.HaloMassFunction(self.redshift,omega_m=self.omegam, omega_l=self.omegal, hubble=self.hubble,log_mass_lim=(7,15))
result = integ.quad(self.NDLA_integrand,np.log10(mass),maxmass, epsrel=1e-2,args=(params,))
#drdz is in cm/h, while the rest is in kpc/h, so convert.
return self.drdz(self.redshift)*result[0]/self.UnitLength_in_cm
import numpy as np
import halo_mass_function as HMF
import scipy as sp
#M_sun = 2 * pow(10, 30)
m = np.logspace(12, 20)
halo = HMF.HaloMassFunction(redshift=0)
h = halo.overden.hubble0
M = m / h
dndm_0 = halo.dndm_z(M, zz=0)
N = sp.integrate.trapz(dndm_0, M)
print("N = ", N)