def ionization_from_collapse(z,
coeff_ion,
temp_min,
passed_min_mass=False,
**cosmo):
"""The ionized fraction of the universe using perturbation theory.
Parameters
----------
z:
Redshift values at which to evaluate the ionized fraction.
coeff_ion:
Coefficient giving the ratio between collapse fraction and
ionized fraction (neglecting recombinations and assuming all
photons are instantly absorbed).
temp_min:
Either the minimum Virial temperature (in Kelvin) or minimum
mass of halos (in solar masses) contributing to reionization.
passed_temp_min: Boolean
Set this to True if you pass a minimum mass, False (default) if
you pass a minimum Virial temperature.
cosmo: dict
Cosmological parameters.
Notes
-----
See Furlanetto et al. (2004ApJ...613....1F).
"""
sd = cp.sig_del(temp_min, z, passed_min_mass=passed_min_mass, **cosmo)
cf = cp.collapse_fraction(*sd)
w = cf * coeff_ion
return w
def test_figure1():
"""Plot HH fig. 1: Evolution of the collapsed fraction (no quant. tests).
"Evolution of the collapsed fraction of all baryons in halos in
three different virial temperature ranges."
Haiman and Holder 2003ApJ...595....1H.
"""
dz = 1.
z = numpy.arange(45., 0.0, -1. * dz)
cosmo = hh_cosmo()
T_min = numpy.array([[1.0e2],
[1.0e4],
[2.0e5]])
linestyle = ['-', ':', '--']
# Collapse fraction with the various minimum Virial temps.
fc = cp.collapse_fraction(*cp.sig_del(T_min, z, **cosmo))
# Calculate fraction of mass in halos in the ranges of min T.
fc_diff = numpy.empty((T_min.shape[0], z.shape[0]))
fc_diff[0:-1] = fc[0:-1] - fc[1:]
fc_diff[-1] = fc[-1]
pylab.figure(figsize=(6,6))
for i in range(len(linestyle)):
pylab.plot(z, fc_diff[i], ls=linestyle[i])
pylab.xlabel(r"$\mathrm{z}$")
pylab.ylabel(r"$\mathrm{F_{coll}}$")
pylab.yscale('log')
pylab.ylim(1e-5, 1.0)
pylab.xlim(45.,0.)
pylab.title("compare to " + inspect.stack()[0][3].replace('test_', '') +
" H&H (2003ApJ...595....1H).")
def test_figure1():
"""Plot HH fig. 1: Evolution of the collapsed fraction (no quant. tests).
"Evolution of the collapsed fraction of all baryons in halos in
three different virial temperature ranges."
Haiman and Holder 2003ApJ...595....1H.
"""
dz = 1.
z = numpy.arange(45., 0.0, -1. * dz)
cosmo = hh_cosmo()
T_min = numpy.array([[1.0e2], [1.0e4], [2.0e5]])
linestyle = ['-', ':', '--']
# Collapse fraction with the various minimum Virial temps.
fc = cp.collapse_fraction(*cp.sig_del(T_min, z, **cosmo))
# Calculate fraction of mass in halos in the ranges of min T.
fc_diff = numpy.empty((T_min.shape[0], z.shape[0]))
fc_diff[0:-1] = fc[0:-1] - fc[1:]
fc_diff[-1] = fc[-1]
pylab.figure(figsize=(6, 6))
for i in range(len(linestyle)):
pylab.plot(z, fc_diff[i], ls=linestyle[i])
pylab.xlabel(r"$\mathrm{z}$")
pylab.ylabel(r"$\mathrm{F_{coll}}$")
pylab.yscale('log')
pylab.ylim(1e-5, 1.0)
pylab.xlim(45., 0.)
pylab.title("compare to " + inspect.stack()[0][3].replace('test_', '') +
" H&H (2003ApJ...595....1H).")
from __future__ import absolute_import, division, print_function
import numpy
import cosmolopy.perturbation as cp
import cosmolopy.parameters as cparam
import pylab
# Get WMAP5 cosmological parameters.
cosmo = cparam.WMAP5_BAO_SN_mean()
# Set up an array of z values.
z = numpy.arange(6.0, 20.0, 0.1)
# Calculate collapse fraction.
f_col = cp.collapse_fraction(*cp.sig_del(1e4, z, **cosmo))
pylab.figure(figsize=(8, 6))
pylab.plot(z, f_col)
pylab.xlabel('z')
pylab.ylabel(r'$f_\mathrm{col}$')
pylab.show()
import numpy
import cosmolopy.perturbation as cp
import cosmolopy.parameters as cparam
import pylab
# Get WMAP5 cosmological parameters.
cosmo = cparam.WMAP5_BAO_SN_mean()
# Set up an array of z values.
z = numpy.arange(6.0, 20.0, 0.1)
# Calculate collapse fraction.
f_col = cp.collapse_fraction(*cp.sig_del(1e4, z, **cosmo))
pylab.figure(figsize=(8,6))
pylab.plot(z, f_col)
pylab.xlabel('z')
pylab.ylabel(r'$f_\mathrm{col}$')
pylab.show()